n72-14363 (nasa-cr-11 4379) airborne auroral' data · n72-14363 (nasa-cr-11 4379) airborne...
TRANSCRIPT
N72-14363 (NASA-CR-11 4379) AIRBORNE AURORAL' DATA AND SATELLITE DATA ANALYSIS Final Report S.B. ttNende, et al (Lockheed Missiles and Space
Unclas Co.) Oct. 1971 94 p CSCL 03B1 1.3 61 . G3/13361 r1RAA LK UK IMA UK AU NUMBER) f (CATEGORY)
Reproduced by
NATIONAL TECHNICALINFORMATION SERVICE
Springfield, Va. 22151
https://ntrs.nasa.gov/search.jsp?R=19720006714 2018-07-19T13:24:27+00:00Z
NASA CR 114379
AIRBORNE AURORAL DATA
AND SATELLITE DATA ANALYSIS
FINAL REPORT
By S.B. Mende and R.H. Eather
Distribution of this report is provided
in the interest of information exchange.
Responsibility for the contents resides
in the author or organization that pre-
pared it.
October 1971
Prepared Under Contract No. NAS2-6299
By
Lockheed Palo Alto Research Laboratories
For
Ames Research Center
National Aeronautics and Space Administration
SUMMARY
The photometric data taken during the 1969 CV990 expedition
were analyzed in more detail. It was found that the so-called soft
auroral zone extends right through the night side auroral zone.
The soft precipitation is a permanent feature of the night side
auroral zone and probably signifies the position of the plasma
sheet. The harder auroras which include the conventional visible
auroras occur less frequently. The intensity and mean energy of
auroral electrons is correlated suggesting that the fluctuation in
auroral intensity comes primarily from the variability of the
acceleration mechanism rather than the variations in the particle
population densities. The results were published in a number of
oral presentations and in scientific journals. During the 1969
CV990 expedition, coordinated data was taken with the Lockheed
particle experiments on OV1-18 and ATS-5 satellites. The satellite
data was reduced to facilitate coordinated investigations with the
airborne experimenters. The airborne photometric X5200 NI data
were analyzed and the effective life time was found to be 4.5
minutes.
-1-
OBJECTIVE
To provide a final summary of the work accomplished in the
program entitled "Satellite Data Analysis" under Contract Number
NAS2-6299.
INTRODUCTION
In the framework of a previous program entitled "6 Channel
Photometric Observations from the CV990 Aircraft" (NASw 1997),
Lockheed instrumentation and scientific personnel took part in
the 1969 NASA CV990 auroral aircraft expedition.
The data taken during this expedition was combined with the
data taken during the 1968 expedition and was analyzed during the
present program.
The data obtained during the two expeditions constitutes an
extremely fine body of absolute photometric observations of the
aurora. No comparable body of data having such extensive coverage,
high sensitivity, and high resolution exists. The absolute
calibration permits the direct interpretation of the measurements.
The regularity and frequency of the observations permits the use
of statistical methods. The zenithal total column intensity
measurements can be very simply interpreted as absolute particle
intensities. The high altitude aircraft platform permitted the
spatial scanning of the aurora. The uncertainties normally intro-
duced by lower atmospheric scattering and absorption are minimized
by the high altitude aircraft platform.
The analysis of the data did produce some very significant
results in the understanding of the auroras. Further analysis
of this type of data still promises great returns and there are
a large number of questions which could be answered by the more
detailed analysis of these data.
-2-
There have been a number of observations during the 1969 air-
craft expedition which were coordinated with the Lockheed experiments
on OV1-18 and ATS-5 satellites. One of the purposes of this contract
was to reduce the satellite data into a form which is amenable for
analysis and comparison with the airborne data.
ACCOMPLISHMENTS
New Results From Photometric Data
The Lockheed airborne data was analyzed in more detail and a
number of new discoveries were made during the period of this con-
tract as regards to the properties of the aurora.
1. The dayside soft-zone is associated with the dayside cusp region
and the particles are soft being of magnetosheath energies
(Eather and Mende, 1971a).
2. In the nightside auroral zone, two types of electron auroras
occurred; namely, the hard aurora generated by electrons in the
keV range and the softer aurora, often subvisual, generated by
electrons in the 100-1000 eV range (Eather and Mende, 1971b).
3. The occurrence of soft auroras are very widespread and occur con-
tinuously within the nightside of the oval. The hard types occur
less frequently. The nightside soft zone at higher latitude is
caused by the absence of the hard components (Eather and Mende,
1971c).
4. The soft precipitation is related to the plasma sheet, both in
mean energy and flux of electrons (Eather and Mende, 1971b).
5. The intensity of auroras are correlated with mean energy. The
ratio of 6300 and 4278 intensities decreases with increasing 4278
intensity. The 5577 to 4278 intensity ratio also follows this
same tendency, but to a lesser extent (Eather and Mende, 1971c).
6. The mean electron energy at precipitation fluctuates very largely
in the aurora while the number flux is relatively constant (Eather
and Mende, 1971b,c).
7. A technique was developed in which a rough measurement of auroral
primary parameters could be obtained from ground based observa-
tions. These parameters are: proton flux, electron energy flux,
-3-
mean electron energy parameter. This provides a technique of
monitoring these quantities without the use of a spacecraft
(Eather and Mende, 1971c).
Reduction of Satellite Data
The satellite data were reduced to absolute calibrated partikcIe
fluxes for the coordination periods listed. The satellite data are
included in this report as Appendix 2.
Dissemination of the Airborne Phobometer Data
The Lockheed photometric airborne data was distributed in March
1971 in a format requested by the other experimenters. The program
was rerun and the required number of output copies were generated by
Lockheed.
X5200 NI Analysis
X5200 NI is a forbidden line from atomic nitrogen with a very
long upper-level lifetime of 26 hours. Hence, quenching is severe,
but the line still appears in auroral spectra with appreciable
intensity, implying that the excitation rate to the upper level
must be exceedingly large.
We have previously reported statistical plots of the rates of
X5200/X4278 as a function of latitude, and shown that such a plot
confirms the existence of soft-electron precipitation at high lati-
tudes (Eather and Mende, 1971).
We have also attempted to determine the effective lifetime
of the D upper level. Fig. 1 shows a plot of X5200, x6300 and
X5577 during about 1 hour of active aurora. It may be seen that
X5200 and x6300 show very similar behavior, and both are sluggish-
compared to x5577. This implies X5200 and x6300 have quite simi-
lar effective lifetimes. We filtered the X5577 signal with a
t = 100 sec filter, using digital computer techniques and got the
curve labeled "filtered 5577.' From this we see that during the
first 20 minutes of the event, 100 sec is a fair estimate of effec-
tive lifetime of both X6300 and X5200.
We used data from all flights to determine the fractional
change in X5200 intensity and x6300 intensity for a given fractional
change in the excitation rate (proportional to X4278 N2 intensity),2
and these results are shown in Figure 2. It may be seen that, on the
average, X5200 is more sluggish then x6300 and does not follow changes
in the excitation rate as quickly as does x6300. To a first approxi-
mation, the ratio of slopes on the graph gives ratios of effective upper-
level lifetimes.
i.e. NI 2D effective lifetime - 2.7 x OI 1D effective lifetime
Most x6300 emission comes from ~ 250 km with effectife lifetimes
of 100 sec, so we imply the NI 2D effective lifetime is 4-1/2 min-
utes. This agrees well with an independent determination from airglow
measurements (Weill, 1969).
Any further analysis (such as deriving excitation rates and
height of emission) involves a knowledge of excitation and quenching
processes, and we do not know enough about these to make this a pro-
fitable exercise. Dr. M.H. Rees is considering if he can use his
measurements of NI ( 2P - 4S) at X3466 to further this investigation.
-5-
PUBLICATIONS
In accordance with the contract, the results were published and
the project scientists attended meetings where they read papers.
Dr. S. B. Mende and Dr. R. H. Eather were both at the AGU meet-
ing in Washington in April 1971 and both gave related papers.
Dr. R. H. Father presented a paper at the Advanced Study Institut,
Dalseter, Norway, April 1971.
Dr. S. B. Mende attended the IUGG meeting in Moscow in August
1971 where a paper was. given. Similarly, he attended the Cortina
Advanced Study Institut in September 1971 and presented another short
paper.
Complete list of publications of this year's work arising from this
contract is in Appendix 1 of this report.
CONCLUSIONS
The satellite data have been reduced into a suitable form for
coordinated investigation. There are a number of interesting possi-
bilities in coordinating with airborne experimenters. Quantitative
comparisons can be made so that the absolute efficiencies generating
the visible and infrared emissions could be evaluated.
The Lockheed photometric data should be analyzed further and
substorm times introduced into the data. All the data analysis so
far took large averages regardless of the status of the magneto-
sphere. The substorm occurrence times should be established for all
flights from world wide magnetograms. This then has to be intro-
duced into the statistical analysis.
The conclusions of the airborne photometer experiment are sum-
marized in the review paper entitled "High Latitude Particle Pre-
cipitation and Source Regions in the Magnetosphere." A preprint
of this paper is attached to this report as Appendix 3.
-6-
REFERENCES
1. Eather,
2. Eather,
R. H., S. B. Mende, Airborne Observations of Auroral
Precipitation Patterns. J. Geophys. Res. 76, pp. 1746-
1755, 1971a.
R. H., S. B. Mende, High Latitude Precipitation and Source
Regions in the Magnetosphere. Magnetosphere Ionosphere
Interactions, Dalseter, Norway, April 1971b.
3. Eather, R. H., S. B. Mende, "Systematics in Auroral Energy Spectra."
J. Geophys. Res. Accepted for publication, 1971e.
4. Weill, G. M., NI( 4S - 2D). Radiation in the night airglow and
low latitude aurora. Atmospheric Emissions Ed.
B. M. McCormac, Van Norstad, pp. 449-470.
5. Reed, R. D., E. G. Shelley, J. C. Bakke, T. C. Sanders and
J. D. McDaniel, IEEE Trans. Nucl. Sci-NS-16, 359, 1969.
6. Sharp, R. D., E. G. Shelley, R. G. Johnson, G. Paschman,
J. Geophys. Res. 75, 6092, 1970.
7. Paschman, G., Untersuchungen des Elektroneneinfalls in die
polare atmosphare, Doctor's Thesis, Max Planck Institut
fur Physik und Astrophysik, Munich, Germany, March 1971.
8. Sharp,
9. Sharp,
R. D., R. G. Johnson, Low energy auroral particle measure-
ments from polar satellites, in "The Radiating Atmosphere"
Ed. by B. M. McCormac, Reidel Publ. Co., Dordrecht,
Holland, 1971.
R. D., D. L. Carr, R. G. Johnson, E. G. Shelley,
Coordinated Auroral Electron Observations from a
Synchronous and a Polar Satellite, J. Geophys. Res.,
Nov. 1971 (in press).
FIGURE CAPTIONS
Figure 1.
Figure 2.
Figure 3-56.
Active aurora as observed in 5200A, 6300A and 5577A.
The curve labeled filtered 5577 includes an assumed
filter with a time constant of 100 sec.
Fractional change in 5200A and 6300A as a function
of fractional change in 4278A.
Satellite data of Appendix 2.
1 hr
Figure 1.
.
I lI
-2
&.
figure 2.
I I
;;~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
'I
APPENDIX 1
LIST OF PUBLICATIONS THIS YEAR (1971)FROM CONTRACT NAS2-6299
Mende, S.B., R.H. Eather, Auroral Intensity Ratios Related to the
Energy of Precipitating Particles. Trans. A.G.U., pp. 305,
April 1971.
Eather, R.H., High Latitude Dayside Aurora. Trans. A.G.U., pp. 319,
April 1971.
Eather, R.H., S.B. Mende, High Latitude Particle Precipitation and
Source Regions in the Magnetosphere, Magnetosphere Ionosphere Inter-
action, Dalseter, Norway, April 1971. To be published in the
conference proceedings.
Mende, S.B., R.H. Eather, Auroral Intensity Ratios Related to the
Energy of Precipitating Particles. Presented at Moscow meeting
of IUGG August 1971.
Mende, S.B., R.H. Eather, "Systematics in Auroral Intensity Ratios,"
presented at Advanced Study Institut, Cortina, September 1971,
Italy. To be published in the proceedings of the Institut.
Eather, R.H., and S.B. Mende, "Systematics in Auroral Energy Spectra".
Accepted for publication. J. Geophys. Res.
APPENDIX 2
SATELLITE DATA:
Coordinated observations with the ATS-5 synchronous satellite
were acquired on five nights and with the OV1-18 polar satellite
on one night as indicated in Table I. Both of these satellites
contained similar experiments designed to measure the fluxes of
auroral electrons and protons in the keV range. The experiments
and some typical results have been described in references 5
through 9. They utilize channel multiplier sensors and either
magnetic analyses or foil threshold techniques to define the energy
ranges. The ATS-5 experiment provides a measurement of the
trapped electron fluxes at 6.6 RE in four energy intervals and
the trapped proton fluxes (integral) above three thresholds as
indicated in Table II. The OV1-18 experiment provides a measure-
ment of precipitating particles. The energy ranges of the OVl-18
detectors utilized for this study are indicated in Table III. Data
will be presented at two pitch angles; one for the group 1
detectors, (CME-1A, CFP-1B, etc.) and one for the group 2 and 3
detectors (CME-2A, CME-3B, CMP-3A, CFP-2C, etc.).
The ATS-5 data for the times of interest are given in Figures
3 - 54 on two different time scales - twenty-four-hour plots of the
fluxes are shown in Figures 3 - 44 in order to present the data in
the context of the substorm activity of the entire day. Then an
expanded scale plot of the fluxes at the specific times of the
coordination are presented in Figures 45 - 54. The ATS-5 satellite
throughout this period was maintained with latitude •2.40, and a
geocentric distance of 6.61 RE. The longitude varied from 104.7°
east on November 24 to 103.9° east on December 6.
The OV1-18 ephemeris data for the coordinated overpass is
given in Table IV and the fluxes as measured by the various detec-
tors every one second are presented in Table V for a 200-second
I
period approximately centered on the time of the overpass of the
aircraft. Figures 55 and 56 show the integral electron fluxes
and the average electron energy (for electrons in the energy range
0.8 - 16.3 keV) as well as the pitch angle at which the measure-
ments were acquired (1800 corresponds to the detector looking up
the field line) for the two sets of detectors, group 1 (Fig. 55)
and groups 2 and 3 (Fig. 56). The integral proton detectors
were at their background levels throughout the period of the
overpass. The CMP-3B and CMP-3C proton detectors were responding
at satellite times near 905,300 seconds and the measured flux
levels are tabulated in Table V. The CMP flux values should be
multiplied by the following scale factors: CMPA x 1.88;
CMPB x 1.92; CMPC x 1.30. The appropriate pitch angle is given
in Fig. 56 as a function of satellite time.
Table I
COORDINATIO N WITH ATS-5 AND OVi-18 SATELLITE
FliNo
£ght DateI. 1969
2 Nov. :
3 Nov. :
4 Nov. :Nov. ·
5 Nov. :
8 Dec. 5
9 Dec. 7
10 Dec. 8
TimeU.T.
12:15
01:05
00:4605:21
03:41 to06:39
10:51
08:3208:56
10:18
Aircraft AircraftLatitude (N) Longitude (W)
52052 ' 96°34'
55°25 ' 96038 '
55°45 ' 96°27 '
55045' 96°24'
(Grid PatternAbout ConjugatePoint)
55045 ' 96024 '
55045' 96°21'55037' 96°28 '
590291 103012 '
SatelliteCoordination
ATS-5
ATS-5
ATS-5
ATS-5
ATS-5
ATS-5
OVl-18
24
26
2727
29
Table II
ENERGY RANGE OF THE ATS-5 DETECTORS
Energy RangeDetector Particle (keV)
CME-A e o.65- 1.9
CME-B e 1.8 - 5.4
CME-C e 5-9 -17.8
CME-D e 1704 -53
CFP-A p > 5
CFP-B p > 15
CFP-C p > 38
__ · ·II··· I ·()· ·I· ·
Table III
ENERGY RANGES OF THE OV1-18 DETECTORS
Energy RangeDetector Particle (keV)
CME-1A e 0.8 - 1.5
CME-1B e 1.75- 3.3
CME-1i e 3.75- 7.0
CME-1D e 8.3 -16.3
CME-1E e 17.3 -37.0
CME-2A e 0.8 - 1.5
CME-3B e 1.8 - 3.25
CME-3C e 3.7 - 7.0
CME-2D e 8.4--16.3
CMP-3A p 0.40 - 1.2
CMP-3B p .88 - 2.6
CMP-3C P 2.9 - 8.7
CFP-1B p >9
CFP-1D p > 38
CFP-2A p >5
CFP-3B P >7.7
CFP-2C P >24
CFP-3D p > 38
I. : I: . ..I .. , I., . . : :I1 . i > . Tl : : - . ,. ;- - - - I - r - . .1
Table IV
OVl-18 EPHEMERIS DATA IEC. 8, 1969 (ACQ 4027)
UT(seconds)
36921
36971
37021
37071
37121
GeodeticLatitude
65.68
62.74
59.77
56.76
53.74
GeocentricLatitude
65.55
62.60
59.61
56.60
53.57
EastLongitude
262.36
259.59
257.29
255.34
25.36
SatelliteTime
(seconds)
905200
905250
905300
905350
905400
Altitude(km)
532
534
536
538
540
Fr --
.1
TABLE V.sWRITE DIFFE ,E:.JT IAL --LUX
-- i-~ ~ ~ ~ ~ ~~~C..C D -- E-- - Cm E-2 4---29:".5 2 00 , , 29+06 ·205*06 9 91+D 05 1214'05 266-5+ 04 4 ++04 484+0
2:290520~~~~~2 , · ¢,90 6 · 2,;.5+036 .991+05 ,121+0.5 .2b66'+044 4+ 6
'229~23 -+.~Z+0 L+ 6 .991+05 , 12'j,+ 05 ·266+a4 8+064, CD 5 ~~~~~484+062920, ·A.00 · 2(.+9 0. 9 9+5, 210 262~~~~~~~~~~,, 484+06'2'29155-2'05~~~,2,"9*Flp 9U 96 I ' +0 5 ,~i.'2 C'~5 ...28-6-*04-
8-64 ~ 4-84'~ 6-
2.29`~20A · 29+06 ·23+051 .9 91+ 05 1105 06279~~~~~~~ ~ ~~,,~29 ,9+I)6 25o6 .945 12!+05 .286+04 ' 484+0622952· ·7 3629+36D t .2!]+0 . 991+05 .24n5 2640 rl ~ ~ ~ , 219 ·260 .,484+06
2 2 9'h- 5 2 .426 .... .99 105 ..... ''i~ '' ....'286--f ' 4- 44+C6229 5 21342 +
'6, .6I9+36 11"' ·205+06484+It , ~~ ~ ~~. _-:+) 991'0-5 , 1210 .-266+04.- .. ,'f4
·~~~~~~~~~~~~~~~ -,, ~ -L '-27-9r,32_15, A 2 0 +06 ·2r,;.'06 .991+05 ,121 i+n5 .286-',4 484+-2'29~'5'2.1."I -- ~'-~~~~ +6 9914.-05----+ l- 2 .6-+-C 4--; 2 4-6 .- -q.+ 0 5 + --~~~~~~~~~~~~~~~~~~~~~~.41 ,-8'6..
2290;"5212 5 2-0+0e6 2-05 + 6 991+05 ,1I£2!"~5 .286+04 .484+062 29nSi 2: 9 + 0,l6 21.50 9 9 1+405 05 I 21'8 ~05~b6-2297-5221'4' · :-2'0 6 ,2-[~+5 · 9+65- , 1-2.i'(5 . ..2'66-+04- · 484+0~6229.05215~ ~~~~~~~1 .-62+ .0+ 6 .991*05 ,!2!'0 .+041229-~~~5221, 6- 9+0 6 2!~~~~~. 484+0622951 b2+0 2~ 9+5 I I ~ +0 ·~ ~ ~ ~ ~ ~ ~~~~~~~~~~~~~ 2 · , -- _·1 ¢5 ,266+04 . 4 84+06'229 g 524.1, 2· 2 +0 6 ,2. 29+3-4;6 . 991 405 , 1;UO5· 860 4'I0
229~5219.~~~~~~~ ~~~~~~ .2+6 .250 991 +0 , 12 2 8 +05+ 5 Z:.28+-04 . 484+ 06-
22935`221 , .29+0-6 .20 5 +26 .991 +0 o, 12!4'05 , 286+04 ,4864+ 06229S5222 .~29~~+0 6 .2!~+.j6 .99!+05 ,!21"+05 .286+94-29,-15 22:1~~~~~~~~~~~. 44864 +0 6
,5 -1:2 6+0-:.[_-7+-:3'5-----2;'-q -4'-+0'--2 2 9.) 5~ ~ ~~ 2:..3-'7 d6 ,9 -9'~'05 0 ,2. 0.n5 ,286+04 ,4 84+06
'22 9'C-523 I2~06'--7~ L, .2-.-4: ....I4'2Q+'5 6,' -'8 4-- .. 4-+$'~6---2293523350+6 2r.n 991,0-5 .12V"05 .286+04 870234 !~~~~~~~~~~~~~~,7494+0
"""9F2522:'~ 4529+06 2 U+[:5+6 -991+0,5 , 12i~+05 ,286+04 4 84 +0 6
229.52370 .452+B.7+07 244'7 9,+06. ,121.+05 .286+04 , 314+08229.').323 · 62 9,+086 . j,ll4+O . 5+0 ,- IL121*05 , 286+04 ,297+062-297-5243 69~6 .2!:; ,r, '45~[--q 6--'---%9'91-~-[l' ,121'`,5--.-2$6.'04 ...484'+068-
Z29~523]; ,221~"4+08 5+7 .99!44+05 .12,t+05 , 286+04 .- 857+0722905x2)4 . 07°+ 5&'+u6 .99 1+115 12.0 2_6. .. 104 ,. _ 1 ~'~ 4,-,.,~ 266+0-4 , 4 4i+7
2299l52]5, .456+07 ,2L',5+06 .996+04 ,t101. .991+05 1~~281+045 , 484+06'"9n52437 624+07 25- ,,+.-! -i4+C ~-' · . 2 U +0~~~~~~~~~O6 -991+0.5 , k2.+5 26604 l4....~~_r '29-23
',,,759~-0+7---. !-'+-.gf: · 99-'"-----i2 -- &'05 ...76"04-- . 744'6..
22901523'.o . 629+06 .2_-: 5+06 . 991'0-5 , 121*05 .286,04 , 464+067,9",1152 690 . .2r,5+06 -991+05 , 121+05 .286+04 . 4 84+6·~~~~~~~~~~~~5~j .-129T.~- I -", -O.---, -9 g~3 -- Z2-9 z6-60-4- -' 4 4 + O!,...
2292.5242 ', I : 20+07 :2. 25+06 : 991-J05 ',121+0 ',3 286+04 : 450+07022 9OJ5 24.2 .4,51+n7 , 2C5 7+0 - 99!+05 ,12!+05 , 286+04 , 14+0 7
229Q5245. .629:12+06, · 2:35+06 . 991+05 , 121+05 :266+04 .4 82 022915254t; : '2+0 :6+04 744
', , , !
. .. I . I
229S5255. .7.04+O .69 7+057 .159+ ,6 12 J + 5 ,28 6 +04 .555+08229!52-,· ,6;+ 0 , 5.9o+'3g8 .496+G7 ,372'n15 .226+ G4 ·775+082Z?- :52.57- . :,'!o2+0- 6 47 + 06 422+07 I,6- .75+0229n325.~~~~~~~~~~~~~2'A0 '.75+08-2 92 52', · 23n+.oa ,6 25 +97 539 , 12'6]5 .266+0 . 26 . 68+0o229e5259, . !]9+ 0 o9,z+] .991+05 , 2 + 05 2 . 6 04 , 105+08...229 - 3 26 n- ... ..-- 9 3'7--9"0' 7 ..... , 5~; 7 S 'a: ...99i"i-05 ........,"- 2, ;"103 '6 i 04 - , 254+07229i05264, , 29+06 ,2.'5+06 ·991+05 ,12 i+5 .286+04 ,484+06229 5262, ? .2+06 .2 5+nb .991+05 ,1 2i 5 6266+C4 ,484+06
2T2'9 '-5 2+0 .2 6 6'~04 ----- O-6-4229i3264. 9+-5 -2-5 - 9.1q-Q2 -421+; 2tX.4 q2291 :,4, . 29+06 .2, 5+rl6 .*91+[ 5 ,121+'5 · .26'04 -,484+06
229~'5265. ,652°+06 ,2 5 +!6 .9 91t 0 5 ,t 21+05 .286+04 ,484+06229]~5267. , 34+07 . I-+7 .991, J5 , 1i-d-: ..-- -6-- -l .5 , 5C4229.,.26 . -7°+07 ,216+27 9:91+05 ,"'.+05 286+04 ,592+07i29~ 526, ·?72P2+,7 .129+07 .9S1+05 ,121+05 ,286+04 ,952+07~:-9,;.26g, * t7¥:+07 -F--7¥ 0 244+06 , 24 ;'D 66- .-- -21-i] 8
229C5270, .299*+0 , 55+7 336 ' 06 ,121+Q5 .7a6+Q4 ,257+382290527%. .·57+t08 ,395+07 .244+06 ,12~ +05 .28k+04 .297+08-229q-5272.Z 9-) >_27· . !-, P d 4 ]{+7- . 2-44+05 -,12-f-+05.2E0- -7 2 f8+-6 5 286- -
229:5273, · -26+6 ,2-2+07 .336+06 ,3.21T05 .286+04 lo5+229;15274, .. 51 +07 , 85+ 7 15t906 ,121+Q5 .2R86+04 *952+07,2'9':275, · S +'-- ,%- + 7 · 4 + 06 , 2 7- · .- -- 9 7' ..9.+.d229n5276, o+3+ ,38+L7 .105+37 ,121*05 ,286+04 ,257+06
22905277, . 0 4+0 ,5 j3+97 .539+06 ,121+ J 5 .266+04 ,168+08~2g]5-527;2,· . ,]37+~5 i'+ -0 6 , Yfg+ 075--- .22b64,'-,-06+2T2~9~~52 7'', . -3 + C8, 2~: 05 . 404 -2l- C-' -
229E.5279, · 4F'+8 ,395+07 ,336+06 ,121 '05 ,266o04 342+06:29n5280D, .75 5 +,8 ·166+0i .167+07 ,121+05 · 286+04 ,952+0(
-2-9 _,5 - r?- =5 - 3 3-7+-17 f -- 8 a3-+<+(¢4- *-s9+0&
22905282, . 12+gt6 , 274+ 0.1 ,29+067 , 7 C21 +0)5 .286+04 -,515+C8229~52 283. ."°+08 .8 896+07 , 134+07 121+15 .286+04 ,257+082"29'^'8:' .. 7'+'3f4-8---. i-+-n-;--~]'~~ ·..1.....+O../ , _4 J."'- (,5 . .3+O- 66~~t55*of+t) 4 ' --~f6-4-Ci':O -- 2~~ 3~5 2 ~~i3~,~~--,:?,7T~~C7 ---- -- "0t2290528f5, 1Ch+OC ,129+[:7 4 }4+06 121+D5 .26+04 ,128+00229n5256. . 14r'+08 ,22+..7 .775-06 ,12i 5 .28+04D . 237+(]8
-2----29:582l B. ,-r---7-4-+-
-
-
- -.'
· 77 -D1]-6'----- 2 ai --- .286;G'-4" --, 57 + 0 ....2293528;. .964+07 ,483+07 .906+06 ,. 2!+05 ,286+04 .257+08.2295!_289 . *_06+08 ,43+07 ,.434+06 , 121+05 .286404 ,14i+0'2'29 -59, · - 1" T 7 , 47 375 --C-- I1 + 5 ....-; 86-+-0- 4 ... ..'229_5291 , 584+07 ,48h3+07 .336+06 ,12i+05 , 286+04 857+0722925292. . 39f+07 ,4.3+07 .539+06 ,121+05 26tO604 ,%15+0829 2 529-.-, , 4"-6-+'~- ,-b'Sc-' .---6 0--6-- 1-2 J.
- + 0 S , '--'86-0-4 -. 2 3+ -u229[i5294, .293+07 483+07 .336+06 ,121+Q5 .2 B6+04 ,!84+08229n15295. . 20 7 31+07 .3 7 33S6+06 ,12.%+05 ,286+04 200+06-2'-29.0 529 6 . . 245-.'1"-07 - -.- · 3--6--- 1-2'+ .28 6-+_0-- - -, 7 + h'.rl.22935297, -201+07 ,318+Uj7 .159+06 , 21+Q5 .286+04 , 257+8229 ,529R, . i5+07 .282+07 *336+06 ,12%+05 286+04 .23 +n8
-7--'229Cgi3'5, , p-'-'--- '+7--9 ,-+---, I8'6;FO0-:4 - -- 16a3+06--'
CHE/ E __C MEA-,T _C P1E/A c61 11 CtfF1D
.. . ..
S`T cr]EIA CMEJ O CMDC flb ~ ELA\~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
229n5355. .45+07 ,2i5+06 *991+05 ,121+05 ,286+04 484+06229n5356. . 40 o06 ,2! 5+0n 6 .991+05 ,12 . +05 ._ 286+4 4 84 %29m535~7~~ . . 62~o -06~- .~jl~i DX ,91 p5 , (~L~r _ _ ,.286+04 , ,_618+0622.9- 357' . 56 . 91j-5 t*4 ,5+72,29.,5357 , ~;20+07 ,27!+0jc6 .991+05 ,121'+5 .26+04 - ,6144+06229i535 , 29 +07 ,6L, 9+1 0 21+i05 121 ,. 04 ,50+07
229S~n361 ... 62.+6 . u2i:b+Ci . 991+05 ,12X1+['-5 266+04 , 484+0672Q!.2 9 7 f-5 3 +6 ,2 07 299!05 ,12i+.n5 , 26+04 ,484+06..2... r"9360] . 9.....;-!?(i'¥-7 n , +2! 6'-:; ' ...-........ ,.. ..... '+0 + ' -'""'22905361 . 629+06 .2L:5+06 . 9 91"05 ,121+05 .26 6+04 ,484+062 29 5362., 6 2 .29+06 , 2i5+06 .991+05 ,121_+E5 ,286+04 484+06
Z ZT 9',-5366~.--bi . 2-9G6-0 ,.'2 ~-;> .'~~99i J-0'5' .....1~2"i'+ 05 . 2-- 8'¥-.E 4 - -4-8-4'64,-0-6229,5367, ,629+06 . 215+06 . 991+05 ,121+05 , 2-6+04 ,.484+06
229n5'6 1 . F 25+D6 9 2 6 + r 6 .99t 1 05 1 .21+05 .. 86+04 4 l84+G G2 9 -------. , w-;--5- 2 +O 91 + , 3;2l f' . 290 -4 84+06229r5376. , 29+06 ,2(]5+06 .991+05 ,121+5 ,.286+04 ,484+06'22 9': 53'7"6-, . ~ 2,9'+C 6----2. ~]5+6 *i~~ .... ;9'9-1-;-'5 .... ;12 S +'O5 .... ;2 ' 6' ': 0'4 _ -- 4 8'4 + 0- ...
.2.5.37.. -2--^+ ,. m+C,6 . -91!+_0 5 · '~ + 2,6+04 ,484+062295 3J36, . . 2°+06 ,205+06 .99t 405 ,1.21S-05 .286+04 ,468+06
-..-29' 5 .. 4] -- 2i.. 05'---;C 26: 6:' ~-- E-;x48 i-06-- -
229n537,0. ,29+06 fn. +06 .991+05 121+05 .286+04 484+0622915371. ,.S9+06 .20,5+06 , 991405 ,121+05 ,286+04 ·484+06':2-29.53 7~. . '29 --0'6.-~5-~j---]-2] ... .;-99Si]~-¥0- ....;i-~12+5 --- ]-2 6¥~2 504'- ---48'4+-0-
229n5373, 2+ ,2+205+n6 .9951405 ,121+.'5 .26+04 ,484+06229)537, . 9+n6 ,2u4+06 ,991+05 ,121'. +Q 5 286+04 484+06-9 -5'3 7 - 9-*''-8. +2 0 . 9 - 05-- 1 i.+' 5--- ,- 6 6'-0-4-- --. 4- 4 + 6
229n5376 . 2Q , . !'5 2 , 6 2-604 , 44+06229S35376. ,6290+06 ,205+06 .99+0 21+5.5 .266+04 484+06
-- t-- -Li ;. 3 F;is;--i: .cs T6-- 2ii. ;1 () . -; 4; t U 9 - - --- w ; 2 i: 1+ j5 , 2 t h + 0 4~. -,- 8: -us I! G 6
22905377, ,629+06 ,2f5+06 ,.9914G5 ,121+05 .266+04 ,484+06
-- 229] 5-37T, ~. TQ-2 9 ~', 05',,7~¥--"--99''5 ..-S2~ E ...26+:-bA-4- .----48-4+-..
229,5379, 629+06 .25+06 991+05 , 121+05 ,286+04 ,484+046
_ -a - q ,> , Fi4 , * + ,2i 40 6 . ,10 - 05.2 4, , - +06
229r5381. .629' 06 ,2C5+n6 .9·9!+5 ,121+05 .266+O4 .484+06229,5381. .52'~i6 .2 ~:05-6 .-991405 ,121+ 5 .266+04 484+
·2 "9538#d 529+06 ,2[;+06 991'05 121+ 05 2 86+04 484+06229~538 5, ,3629+06 .2(!5 +c,6 .991+05 .,12105 ,26+04 , 484+06
22 9 .Bif> 3 ?,, .~2',-+-,27754:56- 5 ....- ;T 2'i-+5 .; 2'6 ''4 - 4+ o6 ~ .....
2295385.1 .. 29+06 .2-:5+06 . 991+05 .121+05 .286+04 .484+0642953869 , .429+06 ,20!5+06 .991+05 ,121+05 ,286+04 ,484+06'2 K9i.-5 3 Y'. . c 29s+-0-6--7,2 ! i +]0-6---- --. ~-----.-1-+'i -5 .2-$62-7 + 0-4 -- .. _.84+0-- ' ~
22925388, .5-29+06 *05+o6 .991+05 ,2i2+Q5 .286+04 .484+06
229`539. · , 29+06 .-2L,5,+0 .9°1+05 *121+-5 , 26+04 ,48-+06
E29:,3-55 9 o , .6-29t6 ,+o§-+0-6----- ~'i~6--*-_99-i1=d 5--0<.-- 2 J-+ 0'5 ,.286.-4'-- ,-' 48+-06-
22905397, . 629+06 .205+06 .91+05 ,121+05 ,26+04 ,484+06229S5392,, .629+06 .2, 5+06 .991+05 ,121+05 .26+04 ,484+06
5.. 2-9:'9 C 99';0 5 1 2 +-0- --- *9 l--7-2-5--4 0 6-Ei 4--
-A- 8 ;4 ,+-'-
6 -
2959 290-, . .
~~~~_ _ _ _-,-+6 910 ~2+5, 8~0 440
229,05391, .629+06 .2-5+0i6 .991+05 'le12+05 .286+04 04,48+0)6
2290.53927, .629+0 6 ?,205+06 .991+05 ,!21+.05 ,286+04 , 484*06
2-2915395, .829+06 .2':]5+C6 .991405 ,121.+r05 , 286+04 , 484+062~9~559~~~~6 2, 9 +-2'9;F-¢-6 , -+Z r~ ~ +~i ...-9gT-f ---- -2 -+-05- .- 86-+-0-4-- :?]-4 8,1 4 +'6 ...
.~~~~~~~~~~~~~~~~~~~~~~L .
- 2037 :690 250 910 11+5 2-60 t4F 0
*__ _ 1 ~_
+t_
JC
ST C,1P3A CMP3B CMP3C --- ME3B CME3P CE2D.229'530]' C 55t+05_ '35+05 'Z35+.45 ,642+07 ,160+07 ,~77+0651+C~~~~~~~42'2z9~ 30f. 1; '5'5 { +' 65-- 0-6 ~+05 -1 07+'6'.., ,58 +9 0 ... 131.0.__ .4?0229'5302. ,55i+05 ,710+05 ,480+05 --- ,589+07 160+ 7 ,907+05
...... 2?29..' 530 ._.55i+05 .3.60+05_ _..346+ 05 ,589+07 ,212+07 .i31+062 9?.5 304 . 55.i1+05 .360+U5 ,138+05 .589+U7 ,231+07 .282+06
229r5305, .551+05 ,206+05 ,138+05 ---- 642' 07-- -1-600 o7 -- i77+06'
229n^306 .551+05 ,206+05 .13n+05" 332+07 117+07 i77+06--- 9 -2- 539'7'. --,551+0-5 ,-20--5+ 5--, i38 +0 5 -,492+07 ,131+07 ,110+06
229:.5303, . 551+05 ,206+05 ,138+O 0-- -,406-07-- ---,i45+07 -- 153+06229153,09, .551+05 ,206+05 ,138+05 ' ,332+07 , 31+07 ,226+06229 -531 .---- 55i+0-5 20%+U05 2'1+'05, ,332+07 ,117+07 282+06229,S. '1 .t 551+05 ,206+05 138+c5 -- ;-208107 145+-07' 226-229,5312. .551+05 ,206+05 ,138+05 ,236+07 ,683+06 ,153+06
2.9-]_f 95-0'- 20-E+05 , i-3 8 +-Ob .298+07 ,683+06 , 131+062295314 .551+05 ,20o6+05 ,138+05 . .-- ' 20' 8-+07 ... ;-397+-6 .--. 563+05229,5315. .551+05 ,206+05 ,138+05 ,298+07 ,793+06 ,728+05
-2'- '~. 3 '6 .... 5'5'-¥-551+ 36'?00 S'5- .......~'1- 8 l -05-: ,266+07 .10 4+07 .907+0522905317: 1551+05 ;535+-U5 1 3 8 + 05 ---- 29807 .--.-..- 0- 4 07 ....4 44--" 8+-0' 5229.0p31~._ ,551+05__,4ju_ l8G 3+7 *&+6 1+0 ZE9?5 S1>3 7. 51+05 ,206+05 ,138+05 '236+07 ,683+06 :158+0512'971 53'i'7--_- ~5 -~5~:j-!_05--T2a6-0-~-0'5:3R+1 , l'ag0" 20+07 ,581+06 , iDB*O5229.5320, .551+05 2106+U5 ,138+ 05 --...298+'-07 .--- . ..2 7+ ' ,'158+05 '22905321, .551+05 ,206+05 ,138+05 , 182+07 ,683+06 ,!58+05229n'532-.- , f+' 05 .. 2'0641 .1..- i 3- 05, ,29+07 ,683+06 .158+05229 ..5323. ,551+O5 ,20h+r'5 ,138+05 r 'r-029-7 2 3 ...T9+7 ....6 ...;72' +05-229n 3324 551+05 20h+05 138+05' 236+07 583+o6 i58+052'29.!5 3'25, .. '5 i--+ '
-...... :-~'06 2""3 0- C 3 .' 1f38 + '*'~ 182+07 '314+06 _ 265+ 5
'2290532' * , .551+05 , 535+05 . 138+05 .--,.236+'07- - , 237+'06 , i58U05229n5327, .55i+"05 ,71O+05 ,138+n5' 208+07 ,58!+06 , 158-05 .3.2'299-32: -- T55i+'5 ,. .r.6+05 .. .. 383+05 182+07 ,237+06 .265+05 .22905329. .55%+05 ,206+05 , 138+05 -5 ,-236+07 -..-- ,314-,'6 -, 563Q5'- .229.5330 55i+05 2G6+05 136+05 1266+07 237+06 t58+05
-- GZ90Yi?5.331.- - 55 1+ *C -- ,ZOih ·C5-- 1t3 +G 5- ,513t0 7 ,397+O6_ *1558+05229t.533-", 5i+-5 32 -505 C538+CD ,5 +G?-------,397-o-6 - 5229'5333 ..55i+05 .2OA+05 $'38+-05
-13 - +U7 .314+06 ,'5'·
29&nj38, -- t51'C- aO5--, 6 5-§;22 1+0 .-- ,113+07 ,398+06 ,1585+0522905335, 55'5 ,i5+U5 +133+05 8 85 -- '586+07-- .--,397+- 6-, i'"58+05229"533, 55i+05 ,20++05 ,138+05 ,158+07 : 165+06 , 158+--
Z29- '182+~~~~~~~~~~~,t807
229 "5337 237;---- 55:+rj ,0- ... 06'5o .., '2+05-' 112+07 ,98 0+0,5 , 58+ 05229..5335, ..55-i+.05 ,535+U5 ,138+05 ...1i3+07 ,165+. .58+2290533,. .55i+C5 ,20,5+ ,' 138+05 ,158+07 ,165+06 ,158+0 5
2 9 -i. 533P-3 355 1 + 0 5 + 05....]-0 ,1 ,3-8 5-- ,1t6+07 ,237+06 , 58+05
229 ~533~. , ·551+o5 ,ZD35+u5 , t3 S+o05 .-t1 ~ .....`~-b506.~--.~~ 5
9,-,~~~~~~ ~~~~~~~~~~~~ 3Q 39 o7 ....; + +0-~ .. .... 158-+05-
229.0.53423. .55'1+05 ,2036+05 ,138+05 , , 2+07 ,237+06 ,158+0
'29:i53343- 1515 -+C8 -- 2 0 6-Ui- t13 38 g5- 8.15 7 92374- 6 *158+05 ,' 229l53~%- -' .- 56¥5+5- ....- '',¥d5+ .... '3'8¥'05' ; !i58+07 ,732+05 ,158+05
229,7534! · ,551+G5_ ,206+05 ,138+05 .... ;1B+07U6 ,..t65- o .+06 5_+O 522905342' .55:+05 '206+0 5 , 138+05 i358+07 ,314+06 ,158+05k29-0-~3-4~j- -T-sfb5 ......20~-'r''is-~---T1 3 8'n- 'i - ' 'i~+7(140 5
2297534 7 t , 55i.+05 . 20o+05 ,138+05 ..~.~ f~-- ,1+07 ,237+06 -,1i58+05'
2290534 . , 55i + 05 ,2 0Z 6+5 ,13+C 5 .. .1 7...
- 4>229.r5335 , -- 5-57-l+C5- * 2Li+!5 * + ,, 1123+7 -, 980+;5 158+05
229r5353 . 55_+05 .206+05 ,138+ni ~, -3U7 -- ,9 05 -0 i3
55-+05~~~~~~~~~15~' . . . . . ]72 .. . . . ... 158'+0"
%29r:>351. - ,';51'05 w ;t:3^ ,138 + ;_ ' 92),k'5 '15
- .1~ 5 -- . t+t.5 - 13B+.5- , 31+06 , 6752+06 .158+052 2-9n-i53-1 ....55 ]_ 5 5 ....- J6'5C5 .. .. . 5 ,- 3 ,l :i O 5-.
-29n533q. 9~~~~~~~~135207 ,316+06 , :5B+05
22953a54. , 551-05 , 535+5 ,138+05r ,2+f7 , 732+05 2h+5
-- ~292'95339. ;5i'G5 ... .....13F'C5, 1.8+07 ,9+5 ,158+050c,22905350/j ' .55{+5 ,2605 ,!38+.C5 -
~~;5 +!j 0, *~~~~~~~158+05~.-290~ 351 ·, 5+5 ,26U 180 - 29+07 ,98,+0,5 .158+05
22 35 58. ,3~i+06 ,732+05 .. 58+05
22905353 5!052,6+5 1~ .... i+U67 ...... ,-"735 ....... '
.55i+05! 2+05 ,I I 05- ------i292, ,5+0 +0 5 ,138n ,5 182+06 ,732+05 ., 158+05
--91'53 ~, . .- - f .-...... "'i'...22~~~~5 Oi . 3 .,: ,13P, -I3+b7---'7305'-6+-5
- ,s15+07 314~+06 · i58+05229053.55 7 551+ +5. , C60+05 '238+05 __5a_6__+_56..
__8.0+_05 ,15_8+ 5...
-~~~~~~~~~C_sT __ c¢ e _cene-I c C/3 ,Cf3d ,_CCsT~~~~~~~~~~~~~~~k-MS Cm62LD
229 5357. 55i+05 ,V60+05 , 138+05 ,562+06 ,980+05 . i5g1 05229i~535;_. 555{+05 205+05 ,138+05 , 40+0U6 ,732+05 ,158+05toZ9~'5355~-7 ,55-'f:¢-5 ... ;Z06+'0-5 .1...,i38+o05 ,381+Q6 ,732+o05 .,58+05.
29 ,-536. ,. 551+S5 ,206+05 ,138+05 - 4--, -4+6 ... +05 ,158+052'297!5361 .55i+G5 ,26+05 ,138+05 ,214+06 ,732+05 . ,158+05- .2 9 ..;536 ?,";---, 551 ¥- 5.-...' -, 5-30 ¥05 ...- 346+505- . , 214+0t ,732+05 .158+05,: 2 9 573 6 ]. ,, + rTb0 210 - ii j-,- ---0~ gu~~,:'29?!363 55i+05 206'Q5 ,221+05 - 5.2-4+0b .732+05 · {58-'--05--E2i05364, ,55i+ - ,206+5 ,34h6+05 214+06 ,980+05 * 58+05f29~ 53'6,-; 7---51:51 ..--.. ;-a~.--0- , f - 1T5--' , t 381+06 , 732+05 158+05229.9536. ,551+05 ,206+05 9138+05 -- 56¥2'00 ...732+-5 ...- 56+-052?2905367 ,551+C.5 2206+05 ,138+05 ,214+06 ,732+05 , 58+05
-~53T'--,55' 05 ..... -+0 .... '38+ -- ,214+06 ,732+05 , 58+05,29j5363., ,55{+05 ,535+05 ,138+05 .51 -+0 6--,'-65-0-6 -,158+05---
229g[5370 .55{+05 ,206+05 ,!38+05 ,214+06 ,732+05 1583+05"- 'a 9-{'5 3 7 f.J~5 i'-%+- 05 ..-. ,Z....-6:-055 --.. f38+05 ..1 ,24+06 ,732+05 ·t58+05'229o5372, .55i+05 .206+05 ,138+05 ---..-24+U6---, 732'O5---- .58+05- .-22935373, .551+05 ,2 06+05 ,480+05 ,214+06 ,732+05 .158+05
-29-37-4-;-.--55-:.........206---05 .. ---5.--- 214+06 ,732+05 ,158+05229-Si537 5 . 55t+0.52064+05 ,1383+05 -"9562+06-- 732+5 . ..5i58+ 5.. 05229n5376. ,55i+05 ,26+05 _,138+05 .214+06 ,732C05 .158+05
'9^537?,',5'i'54 .... 2'O-- +U-)5 ' 138':+0-- 562+06 ,732+05 . 58+05229.53713, ,55i+05 ,205+05 ,138+05 --T2i4+06 ...,732+05 ..... 5P,+oS--Z290537, .551+0-5 .-205+05 ,138+05 .214+06 ,732+05 i158+05
~Z9'-533st-';---5'5+5-....-~+-0 .... ,-38+5-5 : l. 14+06 ,732+05 . i58+059 ?Qr53m, - 551+, ) 2¢5+U5 ,138+ 5 .21O+06 ,732+O5 _ 06+05a29 S3a, , +55i+05 ,2n§+05 ,221+05 - 2i 4-+06--,-732+ '- ...5. .5.2Z-9.538-, 5_5105 206+05 138+c5 ; ,214+U 6 ,732+05 .158+05
P29' 5 3'--5 -
" :-........ " 18 :¢ -05 .3 52!+06__ .732+Q5 *158+05
.29.5384,. .551+05 ,360+05 ,138+05 4 ....;'24+06. ..-73205 . .. '58+5 ..229C5385. 25ai+5 2n6+05 _ 138+05 : 14+U6 ,732+05 : 58+05
-2 ~5 8 , ,>. 55+i35 ,3 .++,5 ,t+i 214+06 ,732+05 ,158+05-2z9.L5387, .5=+C-,5 *706+05 .1383+05 -ffi-.>1-4+-h ,3+C- *g+5
Z-r'9X.:538;:. , - ~5{+0b-
........;O'C-20'6+Q5 ,.138+r5 ,214+U6 ,732+05 i58+305ZZ439X ,10> t6'. j-- ,184"5 t2111+u6 .732+o5 .15r+05
293559p - ,551+W5 ,20h+05 *1 8+C5 42 14 + C, 6 , 732 + o 5 ,-- 5 i Of0 5 -295.39, .55i+05 ,206.+U5 , 221+05 7il4+0u ,732+05 i5. +o 5 :
-- R2-9-n t 3 -2, t * =:> -- 5~-----ac&-0 5----- -,--1 -+05---- .214+06 ,732'05 i5s , U52?9(- '593i , 5 5 + ,035 6 ~" 5 13;8+r,,5 IZ i 0 05--~ +!5-- i t ~~229539;, ,551+;05 X205-+(5 *138+o5 v214+06 732+05 158+05
{RZ9^53' -- 5 . .'i0 , 0+Cv w1 5+[15 *,21+S ?72 . 585
-2 9~~-'.~53-, .'7 55n ifJB1, a- -- ]5:,2 0 , 3 .3, 214+06 t732+05 ,*15F+05'Z2935390, · 551+05 ,206+05 ,138+05 ... '1'4+06 ..732+05 .. -50 °
k29,?~393, ,55i+'05 ,206~-05 , l3a+O5 ..2 ~-'¢:¢O 6--- ... 7 32 %O~~ ~~ 5 ... :1! + 0'5---
'
229n5397. .51+{05 ,206+05 ,138+05 ,214+U6 ,732+05 .158+05.`:29'-339'5--5-]-55f-~ 56... JF ~+J5 .. ~'3 '5.. 24+06 ,732+0)5,1+0
229 C539, ,55{+05 7206+05 ,138+05 - ' S2i--U6 3 272+0 . , "158+t'5g29053997 .551+C5 :206+U5 ,138+05 6',214+6 ',732+0 158+05'2:'53 Z9i4 yaT-- 5 55i*-,5i5 ........, Y06+~cU 5 ..... --~,-y~38 +'~,-0 .. ,562+t06 ,732+05 , i58+ 05
2;2.90353 99, , ~551+05 ,2n6+O15 ,;138+05 -- T2~'14:0' ..... 6;~-,7 32 +-,5~ ...... 'i5'8 0 5 .....
- , + i . ,~~~~~I
*W~ D')S`T APPLY IVL7-IAPLICArlfV Fu A Cro - 5fi TE n 7-
12.
!
ST C,'1P3A CIMP3B CMP3C C"CT1E3B ..CME'3-C7-
-CMFE2D--2297.b2>Po , .55{+05 360+05 9221+05 _ 214+06 732+o5 ,158+05
2-9 5234. .551+05 9360+05 1383+05 i2.4+06 732*+05 158+052.7~9!'520%3 · .55{+05 ,360Il+0 ,23B+0 ? _24_+.~ 6__, 73 2+0 5__- ...i5. +0. __....52G2. .551+05 ,206+U5 138+05 .214+U6 ,732+C5 158+05~' 2 9 : 7t0-* ! .~ · _ _ t 3 - --- 14+C6 .7 2+C515 052qr q
.S 52 0 3~ . .,55{+005 ' 206+U5 ,138+r5 .214+C6 ,732+C5 ,158+05
~ 2'9:'~ 5.P. 4-~----;'5 5{` $5----~'6C~'05-U ,151+ l:35 ,_214+06 __72 C~_rA0e-2,.if2' 3 , 24655i+05 *35+Un .138+Ov0 ,732+n5 .58+0522 902D~ a ,55{+05 ,~5U 138+05 ]2 -t- -ZC-O .6--, 7 32, a'+05·'S*O22945205. ,551+05 .206+05 ,138+05 214+06 732+5 15+ 5
-- ti-2~-9I-nS2-7--. 55i·C+--0-i~5 -;-d-F0- *-3^+S5,l+j ,?2 )_ 15R+rD52e29nz~2G-~. ,55i+5 12O~6+U05 ,a+f5 :.,214+6 ,7320-+Q5 gi58+05S2."529 ?._-.-551-+0- .206+"05 5, 1 38+05_, 214+Q6 ,732+05 ,158+C52,29..5'l~. *551+,5 . 206+05 , 138+05 , 214+06 ,732+05 .i5a+05
,2-~n52: , .55if ': ,_13 -+5 .. ... 4....+-6 ,732- -:-..i5.. "'
~29..'-:!2 . .551+u5 '35+U5 i38+o5 2i4+u6 732+05 " 158+Q.5229052lt ,551+ 5 ,-206505 ,13o+0,5 ,214+06 732+n5 .i58+05
229:95 214 . .55i+05 ,206+05 ,138+05 '2f-+-2 -6--4T732+05 . 15 .. +052 29G-521... ,514+06532n
%29'S215 . 55iF0 ,2b56+[5 ,138+5 , 214+06 732+05 .156+05
<12 9;5213-.~~~~.55it+n5~ t206O5-+0Di---- -- 3 B e 5 i1 4+0 6 ,732+G5 ,15A+G5v'2$%1217 .551+05 * .26+05 .138+052R9-.952' 3'. .55i'+05 '206+o05 1.. +05 , Z14+G6 ,732+5 ,158+C5
2- -2-91 -2T~7~-12 .5i u 1;05--'-7;2 ;J9+tJ5 , L3 ni i38+n5__ 214+ 6 732+o5 1i56+05
22g~!52~~~~14 , 2554+06 732+05 ,158+05 ''6--]T6..
279 1n.2r17. .551+t .005 ~05 .i3r840: ."-2- ,13R36§0i08 58+0229 n221. .55i+05 ,206+u5 ,138+05 ,214+06 ,732+05 .158+0522gg_5.2 '--- .....-~; 5051-+O5---- 20b-+ .. . .... ,i80 , 214+D6 ,752+05 ,158+05229n.527. .551+05 ,360+0;5 ,l138+O5 -2-i-44+ 0 3,i7-2i+ ,58+052293 221· · 55{+05 ,2o6+05 ,_ 38+05 ,214+06 ,732+05 ,158+05-2"gi-52 1'T . ;.55 '5- - -2C- O+d-O , i~ 3 --$ ', 2 4+U26 , 732+05 , *158+05229;522., ,551+05 ,20 6+U5 ,138+05 21,732'%4'4 .- t+--5 --
122g5227. 551+05 ,235+05 138+05 _ 214+06 ,732+; 5 ,15+05Zv9 ; 2 2T- . 55~1+'-q% ,h+ ? 06+05 , 5 ,2,4+U6 ,732+n5 .1F58+05
2 25 1225, · 551'n+,S5 2,6+U5 2,.+Q~C.5 2 13-4 '~0-3-----1i-732+-5 ,5i'5 R+.U"9n23r5 551+g5 , 206+05 138+05 __ 24+6 732+ n5 . '58+ 05
29.5. 224 ,55sI5 , 5 , 07 ,2237+h +5
22,95232. .551+05 ,205+05 ,348+05 ; Zf4'+O 6----~7 5 2 + _ ,i5a+ C.
229'n523 i7. .551+05 20+ ,+05 .2142+067 ,.732+05 1 59+05229: C2-. -- '---. -- ]-?- .Z : 05-' 05 . I'-- 1 05 -C ..,92i4+U 6 .732+05 .158+05229:35229, 5 5 i+G5 ,206+05 2213+05 -13 +U7 .... 73 +r '0 ?---- + 5---- 229n523'6 :55i+05 205+05 :221+05 ,929+06 ,732+o5 t158+05
2 H-9- p 2 ;r-f- ; 55 a + : 5 : 25 C 6-- +2 O -3 5 .6s; b -15 -05
229':5'23~ t ,,55':'~'~ 5---]-20-5"~05 .. . -5 '~5 .,~3e+~rj r;-a ~25+07 2,37+06 . 5. +o52729 5232, .551+05 , 26+05 ,346+D5 --4+ ...-----.. 732 +!C 5---,1-5&+5
229n52339. .95i+5 ,2-06+05 _,13F+n05 ,2+76 ,732+05 .1S+052,97Pi52 347,--.' 55i + .. 2 6+u5 .1..Ti+05 ...3.,+06 ,739+05 -. 58+0522952 .55+C5 ,Z06+U5 ,346+05 -3+-0' . . .. ;732+i--...i5+ .. 8+
< jv97524Z, . 551o~ ,-t:~o5t 5 3221+o5 23 +Q6 57 2+g5 . 5.+9T229!52?3, 26U, 551 Q5 , 535+05 , rj-ln , 1+ . 732+O5
2290.52436 ,51J 205+UC ,221+C5 .4+ ,732C5 15+5~229>5+5245, 20317+x005 1+05 ,9t29+068 , 732+r05 .158t052-2-9.525-;3v% .... 551+i'+05)- . 2: 56i ;'i' 4..¢ 5O-r--' ] 740~- 2w 2+ 732+05 . 15jg+05229n52347, .55i+05 .9206+U5 ,134 +0n -'1 i4'+";16 .- 732+5. ' 55+ ...229!52439. .550+05 ,o60+05 ,138+05 ; 14+06 732+l5 158+.05
- 2-92-529,-; 5+, 55ttj--,~j-*~· IiC~l)-;6-- aro~ 40 -;Q+ , 5 62t~ cU 7 ,73+nD .j -t;41
22ig::52-:, .=5 C5 ,-i- 75 "67+i .732+.5 *.58.05
E<!91525 1 .5i.? . 11 . U 5 .lie ii ,2 5 +. 1? 7 4s1 +i o6 s 7 2+rl: j t¢8+QD
9-27-157;25 2 f40 "51u5 ': '20'-. 6+05- .-- .3..i +-5 3+ ,732+05 .,158+05-29:5241. 5 ,551+05 2.'36+ 3421+U5 ,34+05 -14C i'+'6 ..... .i5 5 .0-29r52542, 551+05 ,3 60105 . 221+05 :214+06 :7O2+,j5 . 58+05
2-2-9-?,'5'2W3 ,5'5'1~5 .....;'555'~-05 ......]'Y'5£, 05 381+06 .732+05 .1-58+05
2 2.9-n;-52445 , ,551+0 5 ,22 53+05 ,2201+2 05 122+CiP' ... 911+. 615 '5.. .2295245 , 31755+635 ,360+05 ,480+05 6297+618 ,752+c5 4215+.05
~2-290 5-- ,,5+5 .... 3-5 I....., +4 6+ 0!--- 2 -1+0 ,732+05 . i5B+0522905247, 9551+05 , 9g4+05 ,480+n5 :'240...
22905248,~~~~~ .5+05 ,360,+05 ,25+Q.5 ;:214+06 :7+0: 1+5'2-2 9'0 52?- g, ...55] ]5---" 0% U ..... ,6+0 .. :, ,20 732+05 . ~58+05
229:,525!, .55t+05 ,399+0:5 ,766+05 .,562+0~6 ....... '732+0!5 ... 1'3+05 ...2E ..g5251: '53~ '1+J6 f, 25 +'.'I 5 ,74 0+;J6 ,732+n5 . 3 + 05-
2'29{?552, -. 55~+:]5.......;-3 ~0+0 05".- i 3F+'1+5 3,351+06 ,732+G5 .15.q+05
X. 9 5 2 5' 551£5 ,'/+5 , 221+C~5 ,214+06 ,9 0+05 5-+0~2Z9-,~5-2 J- I- 2 0 6 +0 122+08,911+06 , i58+05
229.r_.5256, ,55.{-+0-35 ,206+05 , 4GO+G-5 .597+08 , B20+G7 .421+06
__ST' c_ l Ce3A cP33 CfnP3C _CME31 CME3C CKE D
.229.525 7 . ,55i+05 ,156-06 ,143+06 .4 8 2.i'- , .445+o0 ...'-158+U0529"'55:I . ,5514'05 , 132+06 ,124+06 -,642+07 ,117+07 1i58+05_2 9 -5 25'. , ....;55'51+05 * 156+06-- , 915+05' ,208+07 ,314+06 .158+05,-9 .52.! .551+05 1710+05 480+05 -- ..92 5 -6 ...- 98+ 0"5 "158+t]5 ...
2"9 53 2, _ 55+rU5 535+U5 13++05 , 214 + 06 732+05 .158+05---2 9" :5 262 - .. 551+0S- . . 9+- 05 ,766+05 ,214-06 ,732+05 ,158+0522""'"9 "6' . 55i'+05 .710+05 ,221+05 -- 2- -6 , 7 2-+-o6 158-+O5--229-5264. .55l+05 535+05 ,625+05 , 214+06 ,732+05 .158+0542 2 . .. 6 51107+06 .929+06 732+05 ,15 05229',.56f:, .551+05 ,303+06 ,254+06 ,-9';,--0- 7 ,- 2-'7+C6 .,-158+0521 9-7 27 .551+05 ,504+06 ,310+06 ,236+07 .314+06 i5B+05229-n52Z"- ,--55-+-55 ,5504-Ob-- ,373-06 ,298+07 ,732+05 .,158+05229 520°. ,551+05 ,504+06 ,40B+06 ,4680-7 ,3- 4+G6 .56]3+05229r5271, ,551+05 41. +U6 ,254+06 ,642+07 ,683+o06 .265+052'9-~'27-I, ,-4-i--5 ,2'3'f-+¥'6 .1'3i-0'65 642+U7 ,683+06 1·5.8+U52.90527', ,55i+o5 , 238+U6 ,205+06 .6407 ,68306 ,t58+05229.52-7, .551+05 ,lal+U6 ,205+q6 ,.68+07 ,486+06 .563+0522'9 5?7-74'- , 55 +5---o5-,1-B-+06 ,162-+-0 .266+U7 ,237+06 , 58+ 05229o5275, 55st+05 t181+06 ,162+06 -5B-9'O-'7---,7 9 35-+- , !0+-o06229n52-76 .551i05 236+ru6 *183+06 , 25+U7 ,79.3+06 158+05-2 29' 7527 7 ,---T5 5 1 +' 5'TZ .28+0-6 ... _ 2 4 +06 ...... ,642+07 , 793+06 .158+05229'52 7;1i, 55i+05 , 15t+06 107+06 ..- 5--It~~~~~~~ ,4o0--58.--'0-6 - 56+-'-5 ..229n5279. ,551+05 ,.t99+05 ,107+06 ,894+07 ,104+07 .153+06229; _ 1.-- -. 35-5't ' ,06+ +.-1-406. ,337+o8 , 252+07 .131+06
92 ?.,_8 % ,551+05 , 710u'5 ,766+C5 ,4 '8 ,1+7 ;253+0----29~5282 . 55i+05 ,71n+05 766+o5 ,.252+06 ,231+07 .226+06
-- 2'29'52~-7 '-,-55r+'C5 ,....-53 05 -- ,-346+ '5--- . 94+07 ,793+C6 15p+05u229~5264. .551+05 .56+0U6 ,766+05 --T539-67 .,-6-83 +¥6 .72 +05... "54 85 55i+05 132+U6 107+,q6 40,6+07 ,793+0 .·408+UD-2 9~ ;5'2F ,i+'~-O; ....;' -D5- 3 ,D i.Z835+U5 -12- ,699+7 ,104+07 .563+05229,5267. 55i+05 , t!32+06 107+06 --% ' _+-07---7 .-1-.5+T----5 '+-- 05 -229n52~a, .55j+05 , 132+g6 ,124+06 ,968+07 145+07 ,i77+06_2.. I. .. ., - 5' + .. .--13+6 -. ..-7 +06'0- . 760+07 160 +07 C+Ee., - t- I U. I 0 I O. ~~~~~~4Q8+05229r590 52 55i+05 , 18%+i6 ,107+06 --.- 58.9+- 7.-- . ,-1 81+-0- 7 ---.-I0- +30 .A2295291.* ,98+06 ,*13.81+06 ,t24+06 ,642+07 ,104+07 , i58+0j
2- i952 * ·-- ,145+0- , 5-'5 -'6---- . ,539+07 ,117+07 ,265+052295293 . ,551+05 ,11g+06 ,766+05 -,5 89+0 ...- Q.4..+- .. +0. .-22905294. .55i+05 ,710+U5 ,7605 5 ,589+07 ,104+07 ,563+05
22sc ~9...,9 . ;~,~·- 5iC EZ6-+' ----- o 0+7 05 ,b699+07 ,117+07 4$a0A+05229?5296, , 55+05 ,206+015 ,625+05 2- 5+7-----~- -257 -7- 2i-729 ,'5297. 55 i+05 .206+05 ,766+c5 . 25+07 ,17 7 6+1 753+U6za..n2~--, ,55i'-5 .... ,20,6-+05-. -65 "+-C' ..,76g+07 . 145+n7 153+0622905299, 551+05 t710+05 ,?21+05 -6 CT -,i 7 6-- ,7+7.---' 2 5 3 .. 0 6
- i
- ~ Mv-57 A1$ 2PALY /VLlLfrSFFAC'roRl 5,ET 71%r'
,/
I
.. o
.:·
K too - :,
UT( .r ( )
·: - ' .
sO a--- "~S. )-,~ .
U'g ¢SEC)
goas . . . --. I .
t IGO--'----- ------. _.____' : ... .- ,. t o
I I · - 2 :
r4
0 - .~. y
.'1 oooo. 20000. 30000. 0000 50000.
wT¢( SEC)
-n
LI
I D(D(.)co
' -
.,, · . .D
lD s 9 ; o~~~~~~~~~~~~~~~N
: e________________u
. S S~~~~~~~~~~~~~~~~~~~~~~~~~~-
·~~~~~~~ 0·~~~~r
· e'0~~~~~~~~~~~~'
. ,¥ ',' .' ....
:~~ '' : ·-:
" .'· '~' ' : :"· Ii
, .. , -. , -~~ # I e-; - -f~~~~~~~~~~~~~~~ . ,r v
e0000. ibooo. I ooo0 O.
r
I
TII
i
o00 -
41MU
I
a
(3
$2:-f
IZ.J
on
.. - .''*. *- .
- I i' &,
· -%° I -
' . · ·
0-" oo000. I0000. 3oooo. 4oo000
UT( SEC)
I
I
11
II
I� I0
0
, {,4.. .. .
. . .
I
sooo.
Cl)~~~~~~~~~~~~~~~~~~~~~~~~~c
; . '.~ '-
, . 3
IO 't ' ' . ' .· .
aI0
so- ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~I.'.......
X ~~~ ~ ~~~~..^ , .. '' ,, ' .' .
rp 50-:--I-
- ' ' ': ' .". ,, ,:
.,0 .O 4 0 'o00 80.: . '
o 1 I _ '& _( 1o.OO z.Ob 4.00 6.00 8.00 10.00 1Z.00 14.00 *1.00 16.00 to.ob \ t.Oo *4.00
UtT(HR)
4 ' ici . I _ I I I I I i i I I I
\ .~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
-4[)
IAr
Co
co
Im
o~~~~~~~~~~~~~~~~~~~C
- ~ ~~~~~~~~~~~~~~~ . _,_
. ' '" ' , ' ,' .''.' ",'', ,.'.' ', ,'. l
* , .*
I ;:~~~~~~~~~°e
·
, . ._ _ _ ~~~. . _' -
'~ ~ ' '' . .9-,
:.' ' . % ' ,'. o
: ._- .
~~ 'I· '' ''. h-_
* . -.- .- ,
** I?.. ..e ~~~~~~.
' ' -' ' ' *~~~~~~ ~ ~ ': -...
. ~~~~~ ~~~~~ .~ ' .,. . ,3
-'.,-' ".'. ' i' I; .......~~ ~~~~ ~ ~ ~~~~~ * "]-'- *z' *,.- '. !:---- -L,; ,~, ^ ''I ' an:, 'a't ' '; ' HI l I' 0.00 ' Z.00 4.030 .00 6.00 10.00u BC~ )
150
IO-
IU
in
0-
-17-
II
(.
ji
12,00 14.00 16.00 i6.oo0 2J.00 I 2a.oO
-.4(')
I
(D
:0)
I~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~I.
(i~~~~~~~~~~~~~~~~~~~~~~~~~)
I~~~~~~~~~~~qj) ~~~~~~~ ~ ~ ~ ~ ~ ~ N
I . _ ... , __. _____________________ , n
B,~~~~ . ,
O~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~ " '
Co--~~~~~~~~~~~~~~-
siI
t MI
(~50"
-t1. . *'sr . .
\~~~~~~~~~~~~~~~~~~~~·- A .
o9 so- ~· -%:.M 00.. ... ......
;O A 0. -O1.. oo0000. 2000.. 3000.... .
~~0000. ZOODC). 30000, 400o00, ~0000 600rC)O ' ?C003; .... o
za~~~~~~~~~~~~~~~~~~~~~'J · E&)-
_·L�______I _�_______ I
60-_ -
0)~~~~~~~~~~~~~~..l
1- " - - _olJ
(~~~~~0I, 0
O~~~~~~~~~~~~~~~~~~~~~d ~ ~ ~ ~ ~ ~ ~ ~ ;' I I\
., . ' .- (
Xo.--
ci)~~~~~~~~~~~~~~~~~~~~~~~~~~C
\ ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~ o
~0 . .:.
c~~~~~~~~~j~ ~ ~XO,~~~~~ .- t~~~~~~~~~~~ . ... ,. .3'
·c -
e~
4. _ .. -o
. .,..~ . , ...
* V ~ ,~i.
, ...
o - ' .1)oa0. 0ooo0. '-ooo. 40000. Soo0. 60000. 10000. .oaoo.
uT(s C)
I3000. A. .. I
--IIcn
- ~ ~~ ~ ~~~ : *
~''"--~~1------------ - ·---------I A- -- 7 - --- (· -
- -: - --- - - : --~ n
r I
t~~~~~~~~~
-:. · ._- --. --
.o~~~~~- .o o - - _ --- - -o
, ..a 5 3 .
.'.I
.
. I
_ .
I I..... L"- - I - I --- -
bo000o. 20000. 000. 40000, . o0oo0. 60000. aoo000. eoooo.
wI
I
VI
aoN-20
.A
I-
0
I
I
60-
40-
·.
.-
. -r
I
30
I
3sI
Q(
qj
N
UT( SEeC)
Haw
l
- . '- . .A
014
lu
OBI~~~~~~~~~~~~~~~~~~~~~~~~~~O
e A o - \0# S % A w
\sI . .o
I~ e1 ' ~
. . _ ' . - 3
~~~~~~~~~~
..,, ,,. l
lO- .. .. : ' ,, . X,
t)~~~~~~~~~~~~~~~~~~~~~~~~~~~t
o~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
\ .. .. . .. ..~, . , ... :... __
\ a0L~~~~~~~~~~~~~ .. '- .. ,~. ·: .I ~ ,,
,~ .i , ~ .
d.od ' '.oo 4.00 6.00 .c o.O0 12,00 14.00 :.00 1... *^.;'
- · WTCHR)
Ir~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~-
4o- - -- _ O ~~~~~~~~~~~~~~~~~~~.. .4a ~~~~~~~~~~~w
BO - '- '-' ' .'', fi In (P45 I I: Ic~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~r~'- -'
ed~~~~~~~~~~~~~~~~~~~~e
I3 . ',
.. . ...,~- _.; .' ;.
· '.* . ..
Cog ,s ': .. ., ,,
C i '1 ''· ' c-~~~~~~~~~~~~~~~~ .'..:. , .i. X 1'UT a e , ,·~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~.,ol~~~~~o __ z~~~~~~~.,, '~.oo s.oo eo oo zo so eo 6G
,FLI ;' J.'~
--
VIe) o~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~I
Vow t
d 4 24__0 - ------
..,
Of- 1.....
0 ~ . . ~: .... j_~ .. , ~,,~..,~~c.. t . ."~;~e, '-~-~-.~,,,,C,(4~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
o0oo0. 30000. 40000. 50000. *' 0000. 0000. ... 7 - ST o 'T. -r sk O~~~~~~~~~~~~~~~~~~~~~~l r
C;)
cD
CaCO
O
- ...
,: . :
_~~~~~~~~~~~~i
3ooco. 40000.
UT-r( S c)
.. .*
I 5000D. 60000.
5 .
10
'!6
I
tn
VI14
c)S.
qI
.
0-11000c. 20000. 7ooo0. oooo.
II
M
- I
-i
'~~~~~~~~~~~~~~~~~~~~~~~~~~~NWMY-lP*AY'~~~~~~WAM.W-,4C~ I
ao >
14 U-
t4)tn ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ (
C:D
(i)
E0. . 0 5. . o.
I ( E.. **
to '
_ _ JiSO. Zooo. - Soo~o, ....
UT¢ Nc)
aa~~~~~~~· ''0t, .....- CM
s I '. : ' '', '
X . ,.
' ' . ,- .
' I . ,
0~ · I I I
I -0. R0oom0. 300oo. oo400. i Soo. o0000n. rou0 . l 'OO.
UT¢ SE C)
I
I
I.
tJ
CA
. o.n10o00
UT(R)
-.-
ao
!ao i MR.00
_p--~~~~ I I I I I I I I -
. ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~'tHCU)
In
m
CJl
.. ~ ~ ~ ~ ~ ~ ~~~b
U3
j~~~~ ~ ~ ~ ~~~~~~~~~~~ * :,
'"*'1 - ·.' ** *
;~ ~ ~ ~ ~~~~~~~~.~ ... 8
I X1 -.o
···~ ~~~~
.
Qw g l
.': . --
i.. .. *..~~~~~~~~~~~~~~~~~~~~~~~~~~~~~¢.* e.
0
o. o.
~, .'..
· -.. 2
- - - -- ** H~~~~·~ e .
.- .. ~~~~~~~~~~~~~~-._:
0~~~~~~~~~~~~~~~~~~~~~~ I-rl I I
0.00 _.0 '.00 .. 0. '.0010.00 1,.00 14,0 16.00 ~ 0. ' , ._
~~~~~~~~~~~~~~~~~~~~~~·.;.
e~~~~~~~~~~~~~~~~~H
l~~~~~~~~~~ -. *
_~~~~~~~~~~~~~~~~*, ": _ 1 .... ., .*- .3
*:~ ~ ~~~~~~~~~ ''*
- :~~~~~~~.
*': . .-,*
_ ~~~~~~~~~~~.
S~~~~~~~. .~. '/,:'.",-, ,, · ,-I, * .,,'f.-A.-T'.:.. ...
", !' ' -.- ' Iw:R , I · - ' .:0'", ~*" "~ "
-,, *: ..... l'__.
at
14
I
U
IlI .
AD
*2.00 14.00' 15.00 *od.Gi3 2J.i0 1 2a.is 24 via)0.00 I 2.00 4.00 5.00 8.00 0.00O
UT (HP%)
| ~~~~~~~~- 3,.n l~~~~~~I
r~~~t~~~~~~~~~~~~~~5: ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ (-
. . . A~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~I.m
CD
:3·2 ~ ~ ~ ~ ~ ~ OfC~~~~~~~~~~~C
'IT
~~~~~~~~~~~~~~~~~~~~~~~.. .m o.
: : °a
.. ..o ...
.**.
t. · ° ' '° °' · · :~~. 4. .. ·
, ~_. . . . .. ... _,:- . _io. ._ _'6'"......_ '-' ....
_' , , , , wv' °9|= MDI, ;-a*;e 0.-3000. 200o. 30000.
1 . . .
40000. .003. oo.0 Vo" . O'O.
A-T C's' c) . .. -
IS5
kI
(3
Io10-
65
IJ.
0
r
7T
g,~~~~~~~~~~~~f ~~~~~ ~ ~ ~ ~ ~Ll
' . 0
(D
tU 4-m 3
_ 0 . .....
'-t' *', ,*
..... _ IO. zoooo. o0O0. <00000 *o. 0. ooo o60000 0000 o
U-rCsEc)
ES 6-E - -_
-R ,- -C : - : .
,,, .)
a,~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~-
\al -- ..\'U ;
-: '- , : .
M~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~I I
0,a' -'.
:.: ,-
*~~~~ . :' . , - ¢,' 4:;. . ,.
* : ,. .oot.10. 30000 . ,:'. 4000. .000. . c. .0000.
. ),,.,,'
f
-- ' "I
'~~. ! .. ..... ............. .... _
-I
( . .II)
01~~u
8 (~
0~~~~. .............. _ .. - . ... :_, :;..---_ ; .
4X~~~~~~~~~~~~~,: ',-;:,,, . '.,.
ra 4-'.*.:. :
t ~~~~ ~~~~~~~~.' ...-. -:.-,. :.. .. 1..'; ~ ... .,: , *-, .:. ~:: . '. ':.·,: :'
'.vs~~~~~~~~~~~ . ~ ~ ~ ~ ~ ~I..
be *- . V : '- ..
·. ,: ' ' .' ;· j~ ..-l :. · . .ii. , i ,
lo- v s tI l | I-I
cJ~~~~~~~~~~~~..~ · .
43
·.~',~~ ';' -'1~
·· ~~~~~~~~~~~~~~~~.",:: .~i',? ~''~
z I : :'.
"~~~~ 0
0 .9 ~~~~~i. -,.·~
*· 'Y n* 1~
*1 ~ ~4 zi .j!::2:.
*1~ ~~~~~~~~~~St * I
.9 ~~~~~~~~~~~~~~~~~..
o ~ 6%ij3~1(H 1 I oo0oo. 20000. 300Cl0. 40000.
uTCc,)eoono. O. i 0o00.
I
-J.
-t
W
~... .... .. I ,,e
CO(A)
CO
a)
o
cce
.~~~~~~~~~~~~~ ----- ----- . .,....e
8 "~
.Xr'
t4~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~o
u~~~~~~~~~~~0,0 2.t .0 0 .0 00 200 100 1.0 60 O ' .0 .
. .. 1i ' :
. ., , , .
h~~ ~ ~ ~~ ., ;.. _ . . . _ . _ ,.
.~. : "..(:' .".' · . '.
|~~ ~ ~ ~ ~~~~~~~~~~~~~~~~~~ .Y ,si. ''. . ,~~o. A,,
1t. , , , .
m~~~~~~~~~~~~~~~~ . ,........'.,.. ,. ... _... ... .. ,'_.,;_..,. ,,:...'......-AFg
~~~~~~~~~~~~~~~~~~~~~~~~ .' ,~, :~. ~.. . , . -.. .:'s.~Uw~~~~~~~~~..... · . .. ~ : . . k..~ . ~ .m~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~.1 4-
\ . . . . .. .. ..U' ,,,.R)
o;oo ' 2.0b 4.00 6.00, 6.00 *o.oo 12.00 *4.00 Is.oo se.o r t.w *2.00' t4.o
* ~~uT(FR
Vb .· - :' -
l : . . - - , ' - · _0 +_ ~~~~~~~~~~. . - .
0 9
x .- ,', . " , , . .
q~~~~~~~~~, . -, 0,
~~~~~~~~~~~~~BJ~~~~~~~~~~~~~~~~~~~~~- I J
I ·. .j
· )
'~~~~~~~~~~~~~ .. 3a~~.~.~
* *
.·'.~ .. >-~5r *
C).00 Z~r~ 4.00 6.00 6.00 10.00 12.00 14.00 16.00 %c6.00 2,) .00O ~.. 2 4.uO,
UTCHR)
40000. 50000.- ooe c) ooooVT 'sk C}
CI
I..t .
ras
r
8
I
t)I(3!
MnIQ
(4
AA
1
N
U
0S
04
4
a
0
UrT (SE C)
3o
ao0
go
Ba
(AI
4J
Q
!
9.a-
-.
0
30
tC : .. .- -* . .
t 20-..
(Z '
-' ~_.lOO00. 20000. 30000. 40000. , 0000. 60000. :0. .
I-UT(I I I EC I. 0000. 0oooo. 0oooo. 40000. 50u0o. 60000, *00. * aoo.
LrTr sec)
LU
cro~~~ .
At-0-
9% . .:.--.*.N...- .-. I,~ , ."r.: ' '. . __ ... - : *. '-:" ...
_ _ _lacko 20000. 3oooo. 46000.-oo .:... Tl
s~~,ocs~ 20. . 3000.. S C. ) . ..
A)O~~ , - __- . . s' ;
muo00. 20000. 1oo0oo0 dooo. 40hoooi ' ~)L10. tooOO~ &u.~
UTs se)
--4()I
L1
ww
(A
CO
co
C)
I-
..
w
-l 1
I I I iIo.od ' 2.00 4.00 6.00
I IBo00 o t10.00 12.00
UT(H )
I I14.00 16.00 t.00 20.00
30'-
I4tJ
tli
U%
10-
· ...?_ .. -..--.. ~-.
···.f.~·--~-. .i ~~~~~~·r-..r.......... ;.. ...... _.
O-4
Itt.00
I*4.00
I
aO--
. . ...
. .. ... Z:. ... : . . _
. .o : .
o.- . -
- -
..
i I
t0-
10I
iI
0Of
o0-
0-
T
_
C
I
(
: (
,J~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
-.-..~~~~~~~~~~~~~~~~~~~~~~~~~~I~~~~~~~~~~~~~~~~~~~
T! .lrw .. ' P. ' ;
. . ...
':.:;- ...... ....*
- * -:. . .- *2~* .* . *
*-: .- *e -g . -_~~~~~. .. ff .--. *-.?.-,.--...: -:_... _--*:. . _-.. .. .,:-S. .. _._ -.. _.__
*-' " "'.' :.'...- * ' ,4. ,- -
r . .- ·. ~~~~· i
I. - II !! .I I I I, ,I
r ., .~~~~~~~~~~
0.00 2.00 4.00 6.00 6.00 10.00 12.00 14.00 16.00 16.00 20.06 , ZZ.O
VT II )
i)
-Q
L).0
.0
.0
'1-c
24 . 0
q
H
- l l --A
:
IT T -- I
I " .- .- . -
I
.. --_ "
.... ._. .". ._ .. -.: _:- -
: . -.
-"1
.I
,,l
:~~~~~~~~~~~~~~~~~~~~~~~i 'I jj i , ii
i,-.
C
C
A2:'a'C N
IN
-:~~~~~~~~~~~~~;
°oP . .
- ~ ~ ~ ~ ~ ~ ~ ~ A
*· .- '.. .-t.-.-.- . -.
-·C~"
_~~~~~~~.. ... I -!~ -....- .,......,..
l
50000. 60000.20000. 30000. 40000.
.lvCs 'cj1~~~~~~~~ .r (J ($ C
tooo.
30
" 20.
.I
I
"e, IO-
ri
D
3
33
0
wro
10000. .ooo . .. , _ *
__I__ __
I
I
Im~
rl
JT (SESc)
l
I
ic
N-
-aP .
UT(5EC)
QctIx
V)LU
I
lI"
C,N
1
9I.tbJ
O
IrPI.
6~~~~~~~~~~~~~~~~~~~~~~~~~~~~~0~~~~~~~~0)
(A.060-- .. .. -n
(A)Q4 40- . _., _ 0
U9 . 0.j . .UJIUTr',,.))1
.c ~~~~~~~~~~~~~,Q .' ' ' .. w
0 AO
.. '. '.. .'
* 21. ... , .i· .'
, . ' .'_ ' . . ; ; - --. -,. · . .
0A~ . · -. I 1-0- . o , - s OY. .
10000' . 0000. )ooo,. 40000. 2 sa· ', 0000, ooo. *oooo
UT(sEC)
U , · . I so
rii,, 4£.
Z.7- f·~··L' ·A M
o " IIt7' I
O. O,.
0.00 2.00 4.00 6.00 °.00 10.00 12.00 14.00 16.00 18.00 20,00 te.00 V4.00
UT(HR)
40~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~,
~~~~~~~~~~~~~~~~~C ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~'.
o~~~~~~~~~~~~~ ' . ' . ' ' -41 .' . : 1 .
-ni
oxe
s,!,0 ' - -I
6~~~~~~~~~~~0 ~ ~ ~ ~ ~
~-'. ' ...
i;~~~~~~. ' S . '~'' ,-· ' ..'FF:Ht I ;L c- . ..... . .- ... - .. n.. e
, ~ ~ .,=;:--~~~~~~~~~~___- -..\~~~~~~~~~~~~~~·-? .
r C ¢r.'s!.-'F~I''-,' '""' : ;
'
0.00 2.00 4.00 0.00 8.00 10.00 12.00 14.00 -b.00 1?.L0 20.00 22.X 24.0,.
JtIA) I 1 I- , -I --F -
w 40' ~ -a w
J o
I'
t ~40-~~: .....
w ~ uC~l . . M~
t" ·' · o . ' -'.d -·. .-
·~ ~ ~ ~ ~ ~~~
1 .... .. . F
s ....
o . ' .~~~~~~~000 'obo 0' ' :E
-a - r a,_^f*IL' '_ __ ___ __ ____
Ok,_ 4i '1
(3~~~~~~~~~~*00 250. Noo 7. _-1
L* T SEC) ,.. -
10-' --.
co
S- c
1an ~ ~ ~ ~ ~~n
8- . -
mC
..
t 000. .00. 3'o00. 40000. 30000. .600. .OOOO .) oO-
(3'e9 ~ -- . , .U ..Jtwr. . ..
' 1 *
1ovoe. 2ocoo. 3oooo. 0oooo. 5o000. 60000. 0000. ! boos.
UT(SC )
0 41 o13~~~~~~~~\... ., ".....1
,i, .-' ... Iz
4 . ,_ ,_ __ __ I·
0000. 20000. 3o ooo 40000. 50010, 0 . O .' t:-
UT(S EC) u~~~~~rs~~~~~~e )6OOJ
ant~: X --: - tra- ] i·- X-r- -- I11., ... :.,...... : . .. ,. ,:' . 1 , , , . , I
.I ' -- . ' '';''T ' , ' * ~~~~~~-.e
O,)
16~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~1
o
N)
o~~~~~~~~~~~~~~~~~~. ... l
. .; ai)
8~~~~~~~~~~- .: (D
-U
~~~~B "~~~~~~~~~ :: · ,. I0 o~*. . ' .
9~~~~~~~~~~ a:.o , .· : ·, · '
0~~~~ ~ ~~ ~ ~~~~~~~~~~~~~~~~~~~~~ 4- -- _.
- . . ' "-'-" -' - · · ' ' .' ...... ~ .11 , , :
s :I :- ., .. ~ , :\
, ~.o. .- 000. : :. '
\~~~~~~~~~~~~~~~~~~~~~~ .. ' _ . . . -, , 'i
W 4_ _ . - .: .. -. . .:Q..'.. _0,-~~ , , ,* '1 I t . ,; I ' i
00Ct0.I (,cO . 30000. 40000. I 650000. ?booO. I ·00oo.
-- ,~~~~~~~~~~·· i
"-'~'' I i ... I IJ I i I
ry I~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~Ian~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~-
QI~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
: C;
(L~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~" .o ···-
" C:
(4J~ ~ ~ ~ ~ ~~~~~~~~~~~~:
·-~~~~~~~~~~-r
~ *.
2. ...
4--0 t~do r.00 6' 0.00 10.00 12.0 14.00 :6.00 16.0 10.0 33.00 34.0
wr(HRP~t.)
It ' -.- (,jI' -. ,
~l .l l_ ' |.:
I~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~ ·
' ... I ' _. ^ SW ...
- _ .. :;. ,--I --.o -~~~~~~~~~~~~
. ,. * - , .t. .. .1*
.. ' " .
*· £
O- . , .I I I I I I I i i I I I0.00 .O 4.00 6.00 .00 10.00oo 12.00 14.00 t6.oo00 t.OO 20.00 22.00 24.oo00
UT(fR)
LODo CAo
I 0
!
4.~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~.
I( i . . e
.. .... . .e
44p
C-t '1
8 . - '
: .. ,. .. <.. . .-. ~ ,,··., ,~ ~ ~- , ..
0 . .oo. .o .
14~~~~~~~~~~~~~~~~~~~~i: .:-: · -- . · N
O .
10000. 2oo0. 30000. oooo. 0. oo. 7oo o ' _oooO_.
''-'."'c)
Fig. 45
ATS-5 328-$969
IO,107
' I . -- ' 107
_106
! -.. ,._ ., _, _ .10'
!: . - -. :u... . , ' l..
]rOGo
42500. 43000. 43 500,
VTs (sec)! 1 - I
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
I
acIuI
!
of
U
it
Q3
14
Ii'
U
ujriIZ
4
i
t
g4 UUe C DUOe A3S00.! 4UUU0
Fig. 46
ATS-5 330-1?(oqI
· I I I· I . I I I
In0
,10c
4lOg
.' * . . . aO
10c
W * ~~~~~~~~~~~~~~~-I¢~~~~~" ~. ] .'' l
g
10
to'I0'
.', ' . 10y
.. " ' .. . ,. i0
.... !. --.. , . .. . .- __ ....,~,~/ro ~
105
1 -I0. lOs
it +
r . . - A- - I - -' - - -- - ---- -%
4 tIit),I 4 5u.
*1,o10
,I0'
,iO~
416
X
QA
Iin
VI
N
r I
j,
(4
9o.
I I u,7 O I .I- .
1 P 5
UT(SEC)
I · I
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
- I:! til.
13 tloU.
5 3 5rio
, I
-ji
I II II I
I
I
IL
I I. ·I'
i~~~~~~~~~O
. ~ ~~~~~ . ' *; . · . Io~:. . ... o·.
10 6
. *- ,. t . loG
/Os
t10"
i0';
,. * . 10iOT
~~~~~~~~~~~~. .
IOL
10c
,10c
-. . .. 6. | g . X | . X . ,_~~~~~~~~~~~~~~~~10
'000. *S00. 3000. 35O00, 4000.
UT(SEC)
Fig. 47
ATS-5 331-1969
CMEA
CMEB
,CMEC
CMED
CFPA
CFPC
CFPB
:tu
UI
\I
d
W.
4'
I0
'4
Uj(A
14
inI
f4
W
IN
,00. 1 00.
I
Fig. 48
ATS-5' 331-1q69
-_'UI I I I I
.L.
!0
,..._ --. . _
B:~ ~~~~~ *
It
.!t
a ,
1·W~ ~ age WU
.u, U. p~uu. VU~u. ~ uu -- .'1
<~~ I o l u ' v u . -4 ~ u 4 zu,.... Fuu -- ....... uu,-Gxu
.UT sEc)
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
,lof
to" .10';
ic
-10" L I0
{J,s Li)
o 7 I
104
,IoS
,7
q)I
'7 U(j6 LU
I
IS ;Q'
I
ii
I I*P"2"s V~ToP-t
8I
t
.I
.II
I
I
! I
I I:. .. . I..
Fig. 49
ATS-5
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
333-1949
-
,10c10
I0
,i0
t10
' . ' * /0O
10
10I0
.· ;,.' .-i- I 10
10'10
:.~~ , ' . N~10
I0
10
J .Jo0 13. 4 0 '4.3u4
/02
,10 7l O9
4. I U
UT(HR)
*1
6U4qj
s IQC
7 ()
7 uj)I
it
77 14
)6as
of
or
s
)7
)a
5
to
UI
U
IV)
I'
U
N
-- . 016WmRb···1~L*r-ladd~i I-Y~·B--Sx---l·-·~ ·rYI~ ·Y~bbLI~LI-
_.
T-
l l I I
Fig. 50
ATS -5 333- 1969
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
I-J L
!
I . .71-I, " - 43 I
II .1 4)
UT(HR.)'I 14I , 5
.~..,~I,..~`. *'t_'~~`~-~~`*`~~. ,
l09
iO7
to,I O
lor
IOg
10"
v - -~~~~~~~~~~~~~~~~~~~~~~~~ . .~ ;I0
. ~~~ ~~. ': - - ~ ~lo"
yS _- ____,_,'10''..';;irP·i~·"~·ii~
l08
IoY
!0 6' . ' ' . 10'. ', . Xo6~~~~~,
~~~_-_-:..__- _- _ - .... _:. :b,'Oo
. . - . ___ ~~~~~~~~~~~~~~~~107
,10-~
°OrI . . ~~~~~~~~~~~~~~~~~~~10s
3
I, I
2rU
I
I1
UI
i 5.t O)
··r =- -e --- I.i
1.bI
a
M.'
a I
a �
dr
a 04 p
LZt
I! r
4
Fig. 51
ATS-5 333-1969
70
' AM i i .- -- l l!l
~~4~~~~~~~10
Bra'
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~._._. ... o g'
107
i · J-Fw~~~~~~/lo6
10
. . . .~ ~~~~~~~~~~~~~~~~ .lo~
.107
907
· - .. . ~ 06
,/05
10%
-_-, , , _ _.. - . .. ..... _-. 10"
~~~...... ... O G
I0 5
9.IU '
: . ~~~~~~~~~~~~~~~~~~~~~~~~~10$
~~~... _- -,-- ._ -~ . --. w-=- -- -.--_-_. ,--~--,, a _ · 107 I ~
' .--' . - . . of~~~~~~~~~~~~~~~~~~~~~'~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~,,, ,,lti~luI.1. 15.3t~ 1F .. ~r...
UT(HFR)I .' a
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
NJ
I
ui
14I
tII
ac
(3U,
8(3
%
I
1,
(-3
Q
I
14
%.
9.,
-l .
Fig. 52
ATS-5 333-19G9
16 .10 I6. -za 6.3 Li
UT(HR)-. . . -.....d... A ._ - ... .......
lo"106
10 9
,fO~
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
I4:U)I
Iqj
N%101
105'
J09
JI7
F,
IiO'
i!0
I0
10
_0!
U)I
,lv,I-I
N9-
,I
If
G. 40 -,16.50
~~~/ ~~~
rs
-- ~~~~~~~~ --- - - T
I
r
ill
I,
ATS-5 339-I9 9
-L-.q.
I
· ,v10
109
I0o_ ___-_ ballo
*. I.*~ * lQS~ 10
i10.:.,..'._~- ~.=.: . .",v~'~.~ °
10 * '
UT(RI)rIPPR11.00 1t.10
Fig. 53
i
,ot
106 X
CS0
,IO IL4
la" C
CMEA
CMEB
CMEC
CMED
CFPA
CFPC
CFPB
N
c)thI
IIul
g4
r.
9.
10 4 -- = - -too WON -- -
' '--- ~-- --- '.- -' -_.--- ' i1 o,,q.....
W.,
l t
0
Fig. 54
ATS-5 341-67
CMEA o
CMEB ,o0 :
. . o'
Igj
CMEC .
CMEDlO5
CFPA , o'
I
CFPC :'0. i
I o
CFPB -. ..
"go.... I0 00....... I ~ , J00ooo.'
z'fooo 2~,l, , o,. (oSECo. ),oo
UT (SEC)
Fig. 55
HIGLO CME OUTPUTS GRP 1 ORBIT
905250 905240 905250
ELPHT, SEC
905330 905340 905350 905360 905570 90530O 905390 90540C
ELPHT, SEC
A4027
'/o0
.0°
Fig. 56
HIGLO CME OUTPUTS GRP 2,3 ORBIT A4027
*1 /0 9
/0 6
4 /OI s
r
-~~~F·-.I i [.F i
i i,.f. .t~~~'-~--~.-- ; . ! -;··
. t: " ,. LI ' I
f? i ii· i i :i·;'iT
I. . i i :
, ,:L!:. i-.
" ', }
[ . L-,-
I!I4
I .
. i I ii , t-
i i |.I'..
f ,. -
(.!
i :~.!I £ tL~ ,-*-. _- :-: LP.-t P - ·-t- -r -?--]--" -· ---j': I
' -1rt'T Fir rF~T'F
I-
? ~--rI'-i L-LL i Zat -!- -N,-Ti-r,| ! 1 !El
-. ~ -t- ' tj ·L LI
'1:II I ' I i ' I
9,05200 9052200 9052 905230 90524^ 905250
ELPHT, SEC
i.-
l .
905510 905330 905340 905
ELPHT. SEC
r'TT _! ', ,
!,-Ti it, *! _'- '.p--.- 2
. _ ' _ _ S e. -!r .. V ; . t,-:-x D
··, ~ ~ ,
9052?0 905;'e,0 905290 930r i-.~~~~~~~~~~~~~
gO: G'
,4, -L44- ~ .I - L.L-~*-I+----41-t·
n5.....I � . , , . , - , , L - - -I -9AII
I,,
i !
i;L!'r Ii
_ , I!
i
; .,. i,.li
9u0c5u0
I l; !
. -, T-tI IL! i I
I .,.4--i.,
I I -i-1
t , r:.t| .6 e
-,T,1 Tf
i.i,i-; .
:. .. _,.! r:
' ! I !
t . ii .
APPEDIX 3
High Latitude Particle Precipitation, and Source
Regions in the Magnetosphere
by
R. H. Eather* and S. B. Mende*
HIGH LATITUDE PARTICLEPRECIPITATION,
AND SOURCE REGIONS INTHE MAGNETOSPHERE
Presented at Advanced StudyInstitute on Magnetosphere-Ionosphere Interactions, Dalseter,Norway, April, 1971.
R. H, EATHERDepartment of PhysicsBoston CollegeChestnut Hill, Massachusetts 02167
and
S. B. MENDELockheed Palo Alto Research Labs.3251 HanoverPalo Alto, California 94304
* Physics Department, Boston College, Chestnut Hill,Massachusetts 02167
+ Lockheed Research Labs, 3251 Hanover, Palo Alto,California 94304
Abstract
In this review we present averaged properties of precipitating
auroral protons and electrons (as deduced photometrically) and compare
these with direct satellite measurements of similar parameters.
The various distinct types of precipitating particles are defined
and related to their-source regions in the magnetosphere.
There are two distinct types of proton precipitation. On the
nightside, the proton aurora locates equatorward of electron aurora
before midnight, and overlaps electron aurora after midnight. The
most probable source region in the magnetosphere is the ring
current, and gradient drift may sometimes extend this region through
the dusk meridian and as far around as midday. There is a second,
higher latitude zone of soft-proton precipitation on the dayside,
which has its origin in magnetosheath plasma penetration through the
cusp regions.
There are three distinct types of electron precipitation.
On the nightside, there is a broad zone of soft (-1 keV) precipitation
that extends from the equatorward side of the nightside oval and up
to invariant latitudes of -800; the probable source region is the
plasma sheet via loss-cone drizzle. The auroral oval on the night-
side is generated by higher energy (-5 keV) electrons that super-
impose on the low-latitude side of the soft zone. The most probable
source region in the magnetosphere locates between the inner edge
of the plasma sheet and the center of the plasma sheet (near neutral
sheet) in the tail. Gradient drift of these electrons extends
this region through the dawn meridian and past noon, resulting in a
precipitation region locating just equatorward of the dayside oval.
The third region of electron precipitation coincides with the high-
latitude dayside protons and results from very soft magnetosheath
electrons (<300 eV) penetrating the cusp regions. It is these
soft dayside electrons that generate the dayside oval.
These multiple zones of particle precipitation, with their
distinct and somewhat independent sources in the magnetosphere,
comprise a much more complex picture than the simple concept of the
auroral oval would suggest, but at the same time they provide a
basis for a clearer understanding of high-latitude precipitation
phenomena.
1. Introduction
This review describes how ground-based optical techniques
may be used to determine the type, flux, and energy of precipita-
ting auroral particles. Recent experiments along these lines
are described, and we arrive at a number of new conclusions on
precipitation patterns and source regions in the magnetosphere.
Comparisons with satellite data facilitate the identification of
these source regions.
This paper summarizes the essential features of a review
talk given at the Magnetosphere-Ionosphere Interactions Conference.
2. Spectral-Photometric Measurements
Within certain limitations, ground based or airborne
measurements of auroral emissions can be used to determine the type,
energy, and flux of precipitating particles. The technique uses
mainly 4861 HB, 4278 N2+ and 6300 OI measurements; the HB intensity
is used to estimate the proton flux and the proton contribution to
N2+ and OI excitation. The residual 4278 N2 + intensity then gives
the total energy influx of precipitating electrons; at times when
this residual is zero, airglow corrections can be made to the OI
intensity. Finally the ratio 6300/4278 (proton corrected and airglow
corrected) gives a measure of the average energy of the electrons.
There are certain precautions to observe in applying the
procedure, such as van Rhijn and extinction corrections, perspective
effects, lifetime effects, etc; but one can obtain confirming data
by measuring additional emissions such as 3914 N2+, 5577 OI and
5200 NI. Thus careful photometry can be a powerful technique to
study the details of energetic particle precipitation.
Relevant conversion data from emission intensities to energy
are shown in Figure 1. The conversion from 4278 N2+ intensity to
total energy input would be independent of electron energy in a
pure N2 atmosphere (for electron energies 2 100 eV), but because the
fractional abundance of N 2 varies with height, we must use the cor-
rection factor as a function of height (or electron energy) as
shown in Fig. la. Figure lb shows a theoretical curve (Rees,
private communication) relating the 6300/4278 ratio to monoenergetic
electron energy for an assumed model atmosphere. In practice, we
have a distribution of precipitating electron energies, and the
variation of 6300/4278 as a function of 4278 intensity (or total
energy input) is shown in Figure lc (theoretical curves, Rees,
private communication), for various energy spectra peaked between
0.3 and 10 keV. Thus if we assume a spectral form and measure the
6300/4278 ratio and 4278 intensity (for electron excitation), we
can uniquely define the parameter a giving the peak of the energy
spectrum i.e. a measure of average electron energy.
-1- -2-
3. Dayside Precipitation Patterns
Results from airborne experiments aboard the NASA Convair 990
have been published (Eather, 1969; Eather and Akasofu, 1969;
Eather and Mende, 1971). Only four north-south passes were made
near the midday sector, so statistics are limited. Averaged
latitude distributions of 4278 N2 + and H8 have been published
(Eather and Mende, 1971), and are replotted as a function of oval
co-ordinates (invariant latitude minus latitude of theoretical
position of equatorward boundary of the auroral oval, see Eather
and Mende, 1971) in Figure 2. Note first that the peak average
4278 intensity is only 70 R (which corresponds to subvisual aurora).
4278 intensities of -300 R were observed in individual events, and
such auroras were weak but visible. This average 4278 intensity
is lower than nighttime averages by a factor of about 7. The peak
HO average intensity (-8 R) is also less than nighttime averages
but a factor of -3; note too that the proton precipitation (HB)
locates on the high-latitude half of a broader region of electron
precipitation.
Figure 3 shows the 6300/4278 ratios (electron excitation)
plotted in oval co-ordinates, and indicates a number of important
results. There are two distinct types of dayside precipitation: a
region equatgrward of the equatorial boundary of the auroral Qval
where high energy (t 5 keV) electrons precipitate, and a region
poleward of the equatorial boundary (i.e. in the position of the
oval) where soft electrons (s 200 eV) precipitate. (These energies
-3-
are derived from the ratios in Figure 3, the intensities in Figure 2,
and the theoretical curves of Fig. lc.) This same effect may be
seen by looking at the details of particular north-south flights
(Figure 4). It may be seen that for invariant latitudes less than
about 77° , the 6300 intensity shows no relationship to the 4278
intensity, whereas above 770 the two curves show similar behavior.
Both Figures 3 and 4 show that the division between the regions of
hard and soft electron precipitation is very sharp and that there
is little overlap of these regions.
The red auroras excited in the soft precipitation region
have been photographed in color, and there is a clear distinction
between these auroras and the more typical green aurora further
equatorward (Akasofu, private communication).
Comparison of Figures 2 and 3 shows that the protons preci-
pitate in the same region as the soft electrons. An examination of
the Doppler profile of the emitted Ha radiation shows that these
protons are less energetic than on the nightside, so probably have
energies s 3 keV (Eather and Mende, 1971).
These deductions from photometric measurements agree very
well with detailed particle measurements from the low-altitude
satellite ISIS-1. Figure 5 shows spectrograms for electrons and
protons plotted against invariant latitude (Heikkila and Winningham,
1971), The low-latitude, hard-electron precipitation, and high-
latitude, soft-electron and proton precipitation, with a sharp
transition at 730 (Kp = 5) are all clearly shown. For quiet times
-4-
(Kp - 0-1) the sharp transition occurs at higher latitudes (- 77.50)
so that the soft precipitation of electrons and protons covers the
A range -78-81° (Winningham, 1970; Heikkila and Winningham, private
communication).
The coincident precipitation of low-energy electrons and
protons in a region adjacent to a lower-latitude region of hard
electron precipitation led Heikkila and Winningham (1971) and
Eather and Mende, (1971) to suggest that these particles may
penetrate directly from the magnetosheath. Such a penetration
through the dayside neutral points would imply that the lower-
latitude, hard-electron precipitation occurs on closed field lines.
There are a number of recent satellite results associating
high latitude precipitation of soft electrons and protons on the
dayside with direct penetration of magnetosheath plasma through
neutral points (or "polar cusp" or "cleft") (Heikkila and Winning-
ham, 1971; Frank, 1971a). A summary of satellite observations
of dayside precipitation, and a comparison with photometric results,
is presented in Figure 6. Consideration of the experimental data
(and remembering certain limitations on the energy coverage of some
satellite detectors) leads to probable average energy influx of
-0.1 erg cm -2sec -ster-
1 for soft electrons, and -0.05 erg cm 2sec 1
ster-
1 for soft protons. The spectral peak seems to be typically
100-200 eV for electrons and -300 eV for protons. A summary of the
average features of dayside precipitation as shown in Figure 6
is presented in Table 1.
Table 1
Dayside Aurora
Average Energy Input
(erg/cm2sec ster)
4278 N2+ (R)
5577 OI
6300 IO
4861 H8
Hard Zone I
Electrons Electrons Protons Total
0.1
85
-200
20
0.1 0.05 0.15
70
-250
1250
-30 100
-80 330
-30 1280
10 10
-5--Sa-
Soft Zone
The lower-latitude zone of hard electron precipitation has
been discussed by Hoffman (1971) and indirectly by Frank (1971a).
This is a broad, diffuse and steady region of precipitation occurring
on closed field lines; the average energy flux being precipitated
is similar to that in the soft zone (-0.1 erg cm 2sec 1ster )
*and it seems clear that these electrons gradient drift from a
nighttime source region (see full discussion by Hoffman, 1971).
The width of the precipitation region is much broader before
midday than after (Hoffman, 1971; Eather, Heikkila and Akasofu,
private communications) and often extends only a few hours into the
afternoon sector (Hoffman, 1971). This extent into the afternoon
would probably be a function of the nightside source strength and
the loss rate along the drift path.
It is interesting to note that early satellite results
from the Lockheed group (Sharp and Johnson, 1969) showed a second
zone of proton precipitation coincident with the hard electrons
(Figure 7). This zone was not detected photometrically by Eather
and Mende (1971), nor has it been reported by other satellite
experiments. However it occurs in the same region as the trapped
ring current in the dayside (Frank, 1971a) so it seems a likely
explanation is that on some occassions, these trapped ring
current protons do enter the loss cone. Indeed the second proton
zone is probably entirely analogous to the hard electron zone in
that it has as its source a gradient drift from a nightside source
region. Such protons drift through the evening sector towards noon,
and their extent into the dayside would be a function of the night-
side source strength and the loss rate along the drift path.
Apparently the source strength and/or the loss rate near noon
are only occasionally strong enough to give measureable precipitation.
It appears then that we have a quite satisfactory picture
of dayside particle precipitation and the various source regions
in the magnetosphere.
The only significant discrepancies between the satellite
and photometric experiments listed in Figure 6 concerns the geometry
of the polar cusp as a function of altitude. The low-altitude
satellites and airborne photometric measurements show that the soft
zone typically covers some 30 of latitude (i.e. -300 km) and that
the protons and electrons precipitate right across this region.
Higher altitude measurements by Frank (1971a) indicate that the
width of the soft precipitation region of protons, when projected to
ionospheric heights, should be 10-200 km, with an average of -100 km
Frank (1971b), and that these protons precipitate in a sheet located
poleward of the soft electron precipitation. An explanation of the
narrower widths observed by Frank might involve the limited energy
range he considers (700-1100 eV), or uncertainties in field-line
projections. A more serious question is whether the protons precipi-
tate separately and poleward of the electrons; this certainly is not
the case at low altitudes and it is difficult to see how the situa-
tion could be different further up the field lines. Again Frank has
compared limited energy ranges of protons (700-1100 eV) and electrons
-7--6-
(300-500 eV), so an energy variation with latitude could distort
the picture, and if total number flux or total energy flux were
considered, the situation may possibly be more in agreement with
low altitude measurements. We must await a more detailed presenta-
tion of Frank's data to see if a problem really exists.
4. The Daytime Auroral Oval
The question arises as to what is meant by the auroral oval
on the dayside. The oval has been determined from all-sky camera
photographs, so represents aurora which exceed the sensitivity of
the film used. Typically all-sky cameras will just detect about
2500 R of 5577 OI, so respond to energy inputs -0.1 erg/cm sec ster.
In Table 1 we listed the energy inputs into the hard and soft zones
and the expected optical emission intensities. Table 1 is based
on average energy inputs. The normal, high-speed black and white
films used in all-sky cameras (usually Tri-X, 2080, or equivalents)
are panchromatic films and hence quite red-sensitive. Thus these
films would respond preferentially to auroras in the soft zone
(see Table 1.), even though these may be as much or greater energy
input into the hard zone. Even so, the average soft zone energy
input is only just at the sensitivity limit of the film, so we must
ask what is the statistical spread about the average energy input
in both the hard and soft zones? The soft zone auroral forms show
a lot of spatial structure and are often short-lived (Eather, 1969;
Eather and Akasofu, 1969; Lassen, 1969) and this dynamic behavior
this also confirmed by satellite measurements (Hoffman and Evans, 1968
Burch, 1968; Heikkila and Winningham, 1971); in contrast, the hard
zone seems much more steady. Indeed specific events would have to
exceed the average by a factor of 4 to exceed all-sky camera sen-
sitiving in the green. In the soft zone, the 6300 intensity on the
average is near the all-sky camera sensitivity level.
We conclude that the presently accepted dayside auroral oval
represents the soft-electron and proton precipitation, and Hoffman
(this volume) has independently arrived at a similar conclusion.
Fig. (3) confirms this as it shows the soft zone locates in a 3-5°
band just above the equatorial boundary of the oval. However, hard
electrons locating equatorward of the oval deposit as much or
more energy into the atmosphere. As they probably result from a
gradient drift of nighttime electrons, the concept of a continuous
auroral oval might be more applicable to them. Thus we question the
usefulness of the concept of a continuous auroral oval. It is a
very artificial notion that only has meaning in terms of peak
response of black and white all-sky camera film; this peak response
evidently comes from "normal green" auroral on the nightside, and
from "soft red" aurora on the dayside. These are two types of aurora
have entirely different source regions in the magnetosphere, and
there is no obvious topological connection between these regions.
We strongly recommend that the use of the auroral oval as a
means of ordering high-latitude geophysical data on a 24 hour basis
be discontinued, and that instead one keeps in mind the various
different magnetosphere source regions of precipitating particles
that are summarized at the end of this paper.
-8- -9-
5. Nightside Precipitation Patterns
Statistical results from all NASA Convair expeditions in
1967-68 and 1969 (some 40 flights, each of -6 hours duration) were
used in this analysis. Figure 8 shows average 4278 N2+ (electron
excited) and HB intensities in oval co-ordinates, and for night
hours. Figure 9 shows the corresponding 6300/4278 ratio plot.
(The difference between the two curves "average of ratios" and
"ratio of averages" is discussed by Eather and Mende, 1971, but is
not important in our present discussion.)
The previously reported nighttime soft zone (Eather, 1968,
Eather and Mende, 1971) is evident in the peaking of the average
6300/4278 ratio above the oval position. The peak ratio of -5.0
corresponds to about a 500 eV peak in the energy spectrum (Figure lc).
An alternate presentation (Figure 10) shows the percentage occurrence
of peak energies of <1 keV and >5 keV - the >5 keV precipitation
maximizes in the position of the auroral oval, whereas the <1 keV
precipitation locates at much higher latitude - in fact -90%
of the occurrences of precipitation in the high-latitude soft zone
are of <1 keV electrons. A plot of percentage occurrence of 4278 N2+
exceeding 0.5 and 50 R (Figure 11) shows, by comparison with
Figure 10, that the soft precipitation is typically low intensity
(<50 R). It is also interesting to note that there is a broad
region centered on the oval where there is measurable precipitation
virtually all of the time.
Various considerations led us to suspect that there may be a
systematic relationship between the 6300/4278 ratio and the 4278
intensity i.e. between average energy and total energy precipitated.
The ratio 6300/4278 are plotted versus mean 4278 intensity in
Figure 12. The plotted numbers (1+1) represent 40 latitude
intervals centered from 80 equatorward of the equatorial boundary of
the auroral oval to 120 poleward of that boundary (so for example the
numeral 6 represents the interval 0o-2° in oval co-ordinates).
There are no points plotted unless the number of data points in the
appropriate latitude-intensity box exceeded 5.
We have drawn a division line at an intensity level of 50 R,
and note that for 4278 > 50 R, there is a reasonably systematic
decrease of the 6300/4278 ratio with increasing 4278 intensity, for
all latitudes. For 4278 < 50 R, it seems this relation breaks down,
but a reasonably systematic increase in the ratio with increasing
latitude becomes evident. We interpret these results as follows:
(1) there is a low level (<50 R) of precipitation occurring in a
very broad region from below the auroral oval position to well
poleward of it. such that the average energy of precipitation
softens with latitude (from -1.SkeVto s 500 eV).
(2) Higher intensity precipitation superimposes on this low
level precipitation, and locates preferentially in the position of
the oval. This precipitation is characterized by an increasing
average energy as total energy input increases.
-11--10-
6. Variation of Total Energy Precipitated with Mean Energy
We conclude that the so-called "soft zone" does not just
locate poleward of the auroral oval, but extends right across the
auroral oval itself. There is a gradual softening with latitude
throughout this broad region. Energetic electrons precipitation
superimposes on the lower-latitude half of the soft zone, and gives
rise to the visual auroral forms that make up the auroral oval.
As the 4278 N 2 + intensity in the oval increases from 50 R to
up to -10 kR, there is a systematic hardening of the electron
spectrum.
The division of Figure 12 into two intensity division
(<50 R), and our interpretation in terms of two distinct particle
observations, is not as arbitrary as it may seem. In Figure 13
we have plotted the occurrence frequency of a, where a is the
parameter in the spectrum used in Figure lc, and is a measure of
the average energy. It may be seen that there is a definite
indication of two separate particle populations, one between
s200 eV and -700 eV (our soft particle spectrum), and a wider
distribution locating between -1 and -10 keV. Note that a
exceeds S keV only 11% of all cases. However, if we exclude the
low-a distribution, then for those more energetic electron
spectra that excite visual aurora, a exceeds 5 keV some 25%
of the time.
For this analysis, the energy spectrum parameter a
(Figure lc), and the total energy being precipitated were calculated.
The resultant plot of total precipitated energy 0 (ergs/cm2sec)
versus peak energy of the spectrum a (keV) is given in Figure 14.
(Note that average energy of spectrum = 2a.) The data have been
average over all latitudes and times, for nightside data only.
If these particles had been accelerated by an adiabatic
compression process with negligible sources and losses, then
Lioville's theorem prodicts that if we plot 0 versus a on a
log-log plot (as in Figure 14), then we should get a straight
line with a slope of 3. On the other hand, if acceleration was
by static electric fields, we would expect a slope of 1.0.
The plot of total energy precipitated versus a gives a
reasonable straight line, though there seems to be a flattening
out at lower energies. In this respect it is interesting to note
that if we subtract a constant 0.15 ergs cm 2sec from 0, a
much better straight-line fit results (Figure 14). It is tempting
to relate this 0.15 ergs cm 2sec- 1 (corresponding to -40 R of
4278 N 2+) with the average contribution of the soft precipitation,
and then interpret the remainder as the harder, 'auroral' preci-
pitation that superimposes on the soft zone. We do not claim to
have proven this suggestion in Figure 14, but it is consistent with
the rest of our results, and is aesthetically pleasing.
Figure 14 shows that for this particle population above about
0.5 keV, there is a quite linear relationship with a slope of
-12- -13-
1.3 + 0.15. We could argue that this is more consistent with an
electric field acceleration mechanism, but other ad hoc explanations
can explain with such a slope. For example, a combination of
electric field acceleration and adiabatic compression, or adiabatic
compression with strong losses of the higher energy particles,
could give a slope in agreement with the experimental results.
In Figure 14-we have also drawn in the o versus a relationship
8 -2 -Ifor an electron flux of 3 x 10 cm sec 1 It is interesting to
note that our results suggest that the number flux of precipitating
electrons increases by less than 50% for two orders of magnitude
increase in the total energy precipitated. The range plotted
extends up to about 8 kR. We realize that there are times (especially
at breakup) when very intense aurora are excited by much higher
fluxes of 1-10 keV electrons. At those times fluxes in excess of
1010cm lsec 1 have been reported. This must be a much more dynamic
and transitory process than the lower-level, steady-state picture
we invisage here, for IBC 1-2 auroras.
-14-
7. Comparison with Plasma Sheet Electrons
In Figure 15 we summarize plasma sheet data from 17 Re
according to Hones (1968). We have plotted his data (originally
published in tabular form) by performing averages as indicated
and assuming equal weighting for his latitude-longitude boxes.
In Figure 14A we see that the average energy of plasma sheet
electrons decreases from about 1.2 keV at the center of the plasma
sheet to some 0.4 keV near the edge. This has led us to associate
these electrons with our soft precipitation zone, as it shows a
similar softening with latitude. As the energies match fairly
well, we believe that the soft precipitation represents a loss-cone
drizzle of plasma sheet electrons, with no important acceleration
processes involved. If we assume isotropy, the -1 plasma sheet
loss-cone maps down to the ionosphere and carries enough energy to
excite some 10-50 R of x4278 N2 + emission, in good agreement with
energy inputs into the soft zone (Figures 4 and 12).
The data presented in Figure 15 were obtained for dipole
tilts between +200, so an effective broadening of the latitude
extent of the plasma sheet results. Typically the latitudinal
width of the plasma sheet near midnight is only -+3 RE, and the
sheet thickens to perhaps double this value near the dawn and dusk
meridians. According to Fairfield's (1968) model of the tail field,
we would not expect the edges of the plasma sheet to map down to an
invariant latitude that ever exceedsabout 74° . But we observe
soft precipitation up to about A = 79-80° , which we believe comes
-15-
from the edge of the plasma sheet. Certainly there are not sufficient
fluxes of low-energy electrons in the high-latitude magnetotail to
explain the observed precipitation. We are forced to conclude that
the edges of the plasma sheet must map dowrn to higher invariant
latitudes in the ionosphere that would be expected from Fairfield's
(1968) model. Independent studies of the thickening of the plasma
sheet and poleward movement of the electrojet (Hones, et. al., 1970)
also indicate that a given latitudinal interval in the plasma sheet
near 17-18 RE subtends a larger invariant latitude interval at the
ionosphere then that indicated by Fairfield's model.
On the low-latitude side, our observations of aurora at
invariant latitudes of 600 indicate, by comparison with Fairfield's
model, that these aurora occur on closed field lines. Vasyliunas
(1970a) has convincingly associated this equatorial boundary of
aurora with the inner edge of the plasma sheet, which he also
regards as being in a closed field line region.
We now consider the more energetic auroral precipitation (the
,50 R side of Figure 12) that excite the visual auroral forms.
Average energies are in the 1-10 keV range, and so exceed typical
average energies in the plasma sheet. The average precipitated
energy at the peak in Figure 8 is -0.6 erg/cm2sec ster, and this
also exceeds typical plasma-sheet energy fluxes, though there are
some discrepancies in reported fluxes. Hones (1968) and Vasyliunas
(1968) agree on the electron mean energy (-0.2 - 2 keV, average
-1 keV) but the "most probable" energy density given by Vasyliunas
is a factor of -3 higher than Hones' "average" values. In fact
Hones' maximum energy flux (-0.3 erg/cm2sec ster) is about the same
as Vasyliunas' average. In either case, both the average energy
and energy flux of plasma sheet electrons are significantly less
than for the precipitated electrons in the auroral oval, and it is
only the cases of very high plasma sheet energy fluxes (-1 erg/cm2sec
ster) that compare with average precipitated fluxes. Certainly
the energy fluxes associated with commonly occurring IBC 2 aurora
(-2 erg/cm2sec ster) are almost never seen in the plasma sheet.
The variability of plasma-sheet energy spectra is illustrated
in Figure 16A where we show a selection of published spectra;
Figure 16B shows three schematic spectra derived from Figure 16A
that represent typical "soft," "average," and "hard" spectra.
The energy carried by each of these spectra is .06, 0.3, and 1.0
erg/cm2sec ster respectively. The "typical" spectrum published by
Vasyliunas (1970b) seems to be nearer to the hardest of published
spectra.
The photometric data presented in this paper, together with
arguments presented earlier by Vasyliunas (1970b) and Frank (1971),
seem quite convincing in associating the harder, auroral-oval
precipitation with a magnetospheric source region locating from
the inner edge of the plasma sheet and extending down the centre of
the plasma sheet. We maintain that some acceleriation is required
between the plasma sheet at -18 RE and the auroral zone, and note
-17-
-16-
that a simple adiabatic compression would be entirely adequate to
provide the required energization (of about a factor of 5). We
note that harder plasma sheet spectra in Figure 16A were all measured
close to the earth (9-11 RE) than the Vela orbit (17-18 RE).
We are somewhat in disagreement with Vasyliunas (1970b),
who also views the auroral oval as an extension of the plasma
sheet to ionospheric heights, but he requires no energization in
the process. (We believe that loss-cone drizzle does occur, but
gives rise only to the soft zone.) Vasyliunas (1970a, b) cites the
contention of Chase (1969) that the electron energy spectrum in
post-breakup auroral closely resembles, in both shape and intensity,
the spectrum within the plasma sheet. We have examined Chase's
(1969) published comparison (his Fig. 2), and note: the total energy
-2in the plasma sheet spectrum is -0.3 erg cm sec, whereas that in
the auroral spectrum is -2.0 erg cm 2sec; the auroral spectrum has
a peak between 5 and 10 keV that carries 2/3 of the total energy,
and has no counterpart in the plasma sheet spectrum. Thus we
conclude there is little reason to contend these spectrums are
similar (even though they may appear so in a figure that plots 7 1/2
orders of magnitude of flux in a space of just one inch, Chase
(1969). A few more detailed comparison of plasma sheet and auroral
spectrum (Hones et. al., 1971) reveals that the plasma sheet
spectrumsare typically softer than auroral spectrums,especially in
that they do not show peaks in the 5-10 keV range as are often
observed by rockets; and plasma sheet fluxes are typically an order
of magnitude less than auroral fluxes as measured by rockets.
Vasyliunas also compares the averaged precipitated electron
flux in the auroral oval (Sharp et. al., 1969) with three OGO-1
passes in the plasma sheet. We again feel the "agreement" is not
convincing. First there is the problem of matching the plasma-
sheet data (at various estimated distances from the neutral sheet)
with satellite data at various invariant latitudes; we have discussed
above evidence that a given distance above the neutral sheet should
correspond to higher latitude than indicated by Fairfield's mode.
Second, Vasyliunas energy fluxes (-0.3 erg/cm2 sec ster) are about
three times Hones' average, and Sharp et. al. peak average flux
(-0.3 erg/cm2sec ster) are about half of Eather and Mende's average.
So if we compare data fron Hones and Eather and Mende, we would
conclude there was a discrepancy of a factor of six. This argument
reduces to the question of which data to believe, so is not
particularly profitable. But we feel the argument concerning the
differences in average energy of plasma-sheet and auroral particles
is quite convincing.
A few final comments should be made on the character of the
auroral precipitation. Figure 11 shows that there is always
measurable precipitation in the position of the oval, but that the
energy flux only exceeds .06 erg/cm2 sec ster about 50% of the time.
At higher latitudes where mainly soft precipitation locates,
emissions are detectable only -50% of the time and exceed 50 R
only 5-10% of the time. Thus in neither case is there a continuous
-18- -19-
There are, however, short-lived (few minutes) structured
(spatially) bursts of precipitation across the polar cap. Eather
and Akasofu (1969) showed from photometric data that the emissions
were excited by soft (<1 keV) electrons. Heikkila and Winningham
(1970) and Hoffman and Evans (1968) see similar features from
satellites. From the geometry of the magnetosphere, it seems these
electrons must come'from the high-latitude magnetotail, though we
know of no reports of isolated plasma "clouds" in that region.
10. Precipitation Patterns and Source Regions
We have tried to summarize the basic precipitation patterns
in Figure 17, for both electrons and protons. Figure 17A shows
the electron patterns, displayed on an invariant latitude - magnetic
time grid, with the auroral oval for quiet times (Q = 1) added
for reference. As discussed in Section 4, the oval on the dayside
locates in the soft zone and results from direct penetration of
low-energy electrons from the magnetosheath. Immediately adjacent
to it and on the equatorward side are the higher energy electrons
that have gradient-drifted from the nightside. Hoffman (1971)
associates these with Sandford's mantle aurora. The dayside
precipitation of these electrons does not seem to extend much past
noon, where it is thinner (in latitude) and less intense. On the
nightside, the auroral oval precipitation is shown, and has it's
origin in the region bounded by the inner edge of that plasma sheet
and the region of the plasma sheet
-22-
close to the neutral sheet. The wide, soft zone is shown extending
right through the oval and up to latitudes of 79-80° , and we believe
this is a consequence of loss-cone drizzle of plasma sheet electrons.
We know of no published data that allows us to connect the
dayside and nightside soft zones, though Frank (1971b) has published
a model showing a topological connection between the associated
source regions. The question marks in the figure indicate the
uncertainties in that respect, and the uncertainties in how far the
dayside hard zone extends into the morning hours. This extension is
probably very dependent on source and loss functions, and hence on
magnetic activity.
Figure 17B shows the proton patterns. The nightside proton
aurora has been discussed in detail by Eather (1967))Montbriand
(1969) and Eather and Mende (1971). It locates equatorward of
electron aurora in the evening hours, with the separation decreasing
towards midnight. In the morning hours, electron and proton aurora
overlap, and as magnetic activity increases, the electron aurora
maximum may move equatorward of the proton aurora maximum
(Montbriand, 1969). We believe the proton aurora has its source in
the ring current, and the ring current is filled by adiabatic comp-
ression of plasma-sheet protons. The extent of the proton aurora
(with a ring-current source) in the morning hours is not clear.
Gradient drift carries the protons to the evening side and under
quiet conditions they extend at least to the dusk meridian. Occasional
observations of -10 keV proton precipitation near midday indicates
-23-
that gradient drift may at times carry precipitation around to the
noon meridian, but this does not seem to be a regular occurrence.
We know of no experimental data that allows the connection of the
proton aurora at dusk to the hard proton precipitation at midday,
so we have dashed the connection in Figure 17B and indicated
uncertainty with a question mark.
The soft-proton precipitation from the magnetosheath gives
the main zone of proton aurora on the dayside. We classify this as
the main zone as it is a regular feature of the daytime precipitation
pattern, whereas the zone of harder precipitation seems transitory.
The azimuthal extent of this soft proton precipitation has not
been established though it clearly does not extend into the
evening sector at high latitudes. Gradient drift could take these
protons to the dawn sector and confuse the picture there, though
for these low energies we suspect the proton lifetime could be
considerably shorter than the drift time.
If Figures 17A and 17B were superimposed, then one can obtain
an idea of the complexity of auroral precipitation. With two
particle types, and a number of source regions and precipitation
processes, it is clear than any well designed experiment (either
photometric, rocket, or satellite) must measure a wide variety of
parameters to obtain the complete picture.
Our Figure 17A (for electrons) is considerably different
from the Hartz and Brice model, as modified recently by Hartz (1971).
Hartz implies continuous (24 hour) zones of "splash" and "drizzle"
-24-
type of precipitation, with the superposition of the magnetosheath
precipitation near midday (Figure 18). We would associate his low
intensity "drizzle" on the nightside with our soft zone (and point
out that it should extent up to higher latitudes -790), but on the
dayside we would associate his higher intensity drizzle with our
dayside hard zone. As we invisage different source mechanisms, we
would not connect these two regions. We would associate his high
intensity "splash" on the nightside with the auroral oval precipita-
tion, and his low intensity splash on the dayside with the high
latitude soft zone, and again we see no evidence to connect these
regions into a 24 hour pattern, as they have separate source
regions. We would prefer to connect the high intensity nightside
splash with the high intensity dayside drizzle as we believe the
latter results from the former, via gradient drift.
Finally, both photometric and satellite data show the dayside
soft and hard zones are adjacent to each other, and not separated
by a region of low or zero precipitation as indicated in the Hartz
model (Fig. 18).
In Figure 19, we have drawn a model of the magnetospheric
source regions, in the noon-midnight plane. This model is similar
to recent magnetospheric models (O'Brien, 1966; Vasyliunas, 1970bi
Frank, 1971a) though different from all of them in some respects.
The salient features of Figure 19 have all been discussed in the
preceeding text, so will not be further elaborated.
Acknowledgements: This review was written with the support from
grant NGR 22-003-018 from the National Aeronautics and Space Admin-
istration, Airborne Sciences Office.
-25-
Figure Captions
Fig. 1: a) Fraction of the total ionization cross-section presented
by N 2 in the Jacchia (1964) atmosphere, as a function of
height, and corresponding 4278 N 2 + emission per 1 erg/cm2
sec ster of electron energy deposited at that height.
b) Theoretical 6300/4278 ratios (column integrated) as a
function of 4278 intensity for monoenergetic electrons,
for a fixed flux of 109 elec/cm sec. (Rees, private
communication).
c) Theoretical 6300/4278 ratios (column integrated) for an
assumed form of the electron energy spectrum, with
different peak energies a, as a function of 4278
intensity.
Fig. 2: Average 4278 N2+ and H8 intensities as a function of
"oval co-ordinates"(see text), for dayside auroras.
Fig. 3: 6300/4278 ratios as a function of oval co-ordinates, for
dayside auroras.
Fig. 4: 4278 N 2 +, 6300 OI, and 4861 HB intensities throughout a
north-south meridian flight near noon.
Fig. 5: Satellite measurements of electron and proton energy
spectra for a crossing of the dayside auroral region.
The density of the trace qualitatively indicates the
spectral energy density as a function of particle energy
and time. (Heikkila and Winningham, 1971).
-26-
Fig. 6: Summary of measurements of proton and electron energy
fluxes, and mean energies, in the polar cusp.
Fig. 7: Lockheed measurements of the location of peak particle
precipitation; plotted are the number of auroral-zone
crossings with peak response in the 10 interval centered
on 0L (Johnson et. al. 1966).
Fig. 8: Average 4278 N2+ and HB intensities as a function of
"oval co-ordinates" (see text), for nightside aurora.
Fig. 9: 6300/4278 ratios as a function of oval co-ordinates, for
nightside auroras.
Fig. 10: Percentage occurrence of precipitation with mean electron
energy <1 keV and >5 keV, as a function of oval co-ordinates.
Fig. 11: Percentage occurrence of 4278 N 2+ exceeding 0.5 R (limit
of detection) and 50 R, as a function of oval co-ordinates.
Fig. 12: The mean ratio 6300/4278 plotted as a function of mean
4278 intensity, for 10 latitude intervals. The plotted
numbers (1-11) represent 40 intervals centered every 20
from 80 equatorward of the equatorial boundary of the oval
to 120 poleward of that boundary (eg. the numeral 6
represents 0-2° in oval co-ordinates).
Fig. 13: Number of cases of occurrence of a given a (defined in
Figure lc, and is a measure of peak energy for the
spectrum), per unit energy interval. Two separate particle
distributions are indicated.
-27-
Fig. 14: Summary of Hones (1968) plasma-sheet electron properties
at 17 RE. The 1800 curve is for the midnight sector,
and 1200 and 2400 for the dusk and dawn sectors. A. Average
energy B. Energy density C. Energy flux and resultant
4278 N 2 + emission if this flux was isotropic over the
atmospheric loss-cone.
Fig. 15: Total energy precipitated O (ergs/cm2sec) as a function
of energy spectrum parameter a, for nightside data. The
relation for a constant number flux of 3 x 108 electrons/cm2
sec is also shown.
Fig. 16: A) A selection of published plasma-sheet electron energy
spectra. 1-4 at 18 R E (Hones et. al. 1971); 5-15.9 RE,
6-10.5 RE, 7-15.3 RE, 8-19.7 RE, 9-13.5 RE, 10-10.1 RE,
(Frank, 1967); 11-9.8 RE (Schield and Frank, 1970);
12- Vasyliunas (1970) "typical" spectrum.
B) Schematic representation of typical "soft" (1) "average"
(2), and "hard" (3) plasma-sheet electron energy spectra.
Fig. 17: A) Electron precipitation patterns.
B) Proton precipitation patterns.
Fig. 18: Auroral precipitation patterns after Hartz (1971). Triangles
indicate zones of discrete or splash precipitation, and
dots indicate diffuse or drizzle precipitation. Precipitation
of magnetosheath plasma is indicated by stars. Intensity
is indicated by symbol density.
Fig. 19: Source regions in the magnetosphere for the precipitation
regions depicted in Fig. 17. (noon-midnight plane).
-28-
References
Burch, J.L., Low-energy electron fluxes at latitudes above theauroral zone. J. Geophys. Res., 73, 3585, 1968.
Chase, L.M., Evidence that the plasma sheet is the source of auroralelectrons, J. Geophys. Res., 74, 346, 1969.
Cornwall, J.M., F.V. Coroniti, and R.M. Thorne, Turbulent loss ofring-current protons, J. Geophys. Res., 75, 4699, 1970.
Eather, R.H., Auroral proton precipitation and hydrogen emissions,Reviews of Geophysics, 5, 207, 1967.
Eather, R.H., Latitudinal distributions of auroral and airglowemissions: the "soft" auroral zone, J. Geophys. Res., 74, 153,1969.
Eather, R.H. and Syun-I Akasofu, Characteristics of polar capauroras, J. Geophys. Res., 74, 4794, 1969.
Eather, R.H. and S.B. Mende, Airborne observations of auroralprecipitation patterns, J. Geophys. Res., 76, 1746, 1971.
Eather, R.H. and R.L. Carovillano, The ring current as a sourceregion for proton auroras, Cosmic Electrodynamics, 2, 105, 1971.
Fairfield, D.H., Average magnetic field configuration of the outermagnetosphere, J. Geophys. Res., 73, 7329, 1968.
Frank, L.A., Initial observations of low-energy electrons in theearth's magnetosphere with OGO3, J. Geophys. Res., 72, 185, 1967.
Frank, L.A., Further comments concerning low-energy charged particledistributions within the earth's magnetosphere and its environsin "Particles and Fields in the Magnetosphere," edited by Billy M.McCormac, D. Reidel, Dordrecht, Holland, 319, 1970.
Frank, L.A., Plasma in the earth's polar magnetosphere, J. Geophys.Res., 76, 1971a.
Frank, L.A., Comments on a proposed magnetospheric model, J. Geophys.Res., 76, 2512, 1971b.
Hartz, T.R., Particle precipitation patterns, paper at NATOAdvanced Study Institute, Kingston, Ontario (August, 1970). To bepublished in proceedings, Billy M. McCormac, editor, 1971.
Heikkila, W.F., and J.D. Winningham, Penetration of magnetosheathplasma to low altitudes through the dayside magnetic cusps,J. Geophys. Res., 76, 883, 1971.
Hoffman, R.A., Auroral electron drift and precipitation: cause ofthe mantle aurora, J. Geophys. Res., 76, , 1971.
-29-
0
Hoffman, R.A. and D.S. Evans, Field-aligned electron bursts at highlatitudes observed by OGO-4, J. Geophys. Res., 73, 6201, 1968.
Hones, E.W., Review and interpretation of particle measurementsmade by Vela satellites in the magnetotail, in "Physics of theMagnetosphere," edited by R.L. Carovillano, J.F. McClay,H.R. Radoski, Reidel, Dordrecht-Holland, 1968.
Hones, E.W., S.-I. Akasofu, P. Perreault, S.J. Bame and S. Singer, wPoleward expansion of the auroral oval and associated phenomena o Z min the magnetotail during auroral substorms, 1. J. Geophys. Res.,75, 7060, 1970. o
Hones, E.W., J.R. Askbridge, S.J. Bame and S. Singer, Energy spectra uand angular distributions of particles in the plasma sheet and w-jtheir comparison with rocket measurements over the auroral zone, wJ. Geophys. Res., 76, 63, 1971.
Lassen, K., Polar cap emissions, in "Aurora and Airglow," edited byBilly M. McCormac, Reinhold, New York, 1969.
Montbriand, L.E., Morphology of auroral hydrogen emission duringauroral substorms, Thesis, Univ. of Saskatchewan, 1969. O
Sandford, B.P., Aurora and airglow intensities variations with time 'N Lz Ztl 009 OliVand magnetic activity at southern high latitudes, J. Atmos.Terrest.Phys., 26, 749, 1964.
Sandford, B.P., Variations of auroral emissions with time andmagnetic activity and the solar cycle, J. Atmos. Terrest. Phys.,30, 1921, 1968. 3,?3s WD O / ) NOSSIn3 'N 3 LZO
Schield, M.A. and L.A. Frank, Electron observations between the o o o o o o o0 inner edge of the plasma sheet and the plasmasphere, J. Geophys. 0 C oRes., 75, 5401, 1970. o
Sharp, R.D., and R.G. Johnson, Distribution with invariant latitudeof electron and proton precipitation close to noon and midnight,in "Aurora and Airglow," edited by Billy M. McCormac, Reinhold,New York, 1969. w o-z o
Sharp, R.D., D.L. Carr and R.G. Johnson, Satellite observations of z 0 the average properties of auroral particle precipitations: °Latitidinal variations, J. Geophys. Res., 74, 4618, 1969.
Vasyliunas. V.M., A survey of low-energy electrons in the evening ' osector of the magnetosphere with OG01 and OG03, J. Geophys. Res., N
73, 2839, 1968.
Vasyliunas, V.M., Magnetospheric plasma, Review paper presented at _ST? Symposium, Lenningrad, U.S.S.R., 1970a. > 0
oVasyliunas, V.M., Lew energy particle fluxes in the geomagnetic tail, w 0
in "The Polar Ionosphere and Magnetospheric Processes," edited o 0 o 0by G. Skovli, Gorden and Breach, New York, 1970b.
-N Ad 03aN3S3O d-30- N01133S SSOH3 NOIIVZINOI 'V101 3O NOI.3V.*
0.1 1.0
X 4278 N2 INTENSITY (KR)
4278Na
0
Fig. lc
INTENSITY
40
o
Hp INTENSITY (R)
Fig. 2
(R)
7
6
COI"-
a:
00t0(D
0
I-
5
4
3
2 -
0.01 10.0
0 0 0
z
-4
-I
c
m
I
o
r
Cocza
,.,
I
I
4
o0I
0
t
S
0 UL u(
INTENSITY RATIO 6300/4278
ro o6 b b
72 74 76INVARIANT LATITUDE
Fig. 4
z
z
-4
-1
-4
C
I
0
0
0Cza
-C
P.
I
0
0
zo_
o
n 200
C-
z 160
+, 120, 80
oI
(n
z
o
cr
I-(nz
f-z
I
2.0
1.6zw
z1.2
o0o
- 0.8
0.440
oL
i·
iNVARIANT LATITUDE
81 8'
' '
," ' I
Re~r.OFig8 5OPY
Fig, s
_- - _
RET.
SOFT ELECTRONS SOFT PROIONS
TOTAL DNER;Y SPECTRAL TOTAL nDR;Y SPECTRAL(erg/o=2 sec Lter) PEAK (eV) (erg/mo 2 sec ster) PEAK (eV)
D .06Frnk (1970)
IFank (1970)
MID-ALTITUDEPOLAR CUSP
LOW-ALTITUDEPOLAR CUSP
IONOSPHERE
Sharp C Johnson (1968)
B.rLh (1968
Hoffman C Berko (1970)
Wexnik et. .1. (1970)
Heikkila $ Wimninham(1970)
Sandford (1964)
Eather C Mende (1970
PROBABLEAVLRX S:
, 0.1+
.06 * .3
.06 * .2+
.03 * .3
. 0.2
· .1
.03 (av.)
.2 (peak)
1000*
I lCo
. 700*
. 140
100-200
100-200
- .04
> .02+
- 300
. 700
< 4000*
.01 . .1 - 330
.05 S 1000
i- 13* Sigificant precipitation beloa this l1cr energy limit.
+ Probably contains significant oontribution fron higher eergies.
Fig. 6
wzLIU
>-(on,>
fr
I0'
10'
10
104i
6 s68 70 72 7q 77 79 3
//
///,
NIGHT ZONES
ELECTRONS PROTONS
I I I I I I I I I I I I I I I I
u 3 u 5 0 5NUMBER OF CASES WITH CENTER IN 1-DEGREE
NOV.9-tO,1965
0 5INTERVAL OF 8 L
10
.7
4278N. INTENSITY
0 0 0 0 0
H/3 INTENSITY
25 r-DAY ZONES
-j
a
C)
z:
z
I
20
15
10
SOFTELEC-TRONS
50 3
(R)
I
0
C0
z
z-4
r
-1com
z0
. I I I I I I I I ,
(R)
0 O
0
0 0
0 0
0 0
m
w
1- to
Ln
iN
_o C
33
N3
l88
no
03
9V
IN3
31
3d
I V
I to
O
J
8L
Z/0
£9
OIIV
! A
J ISN
31NI
w
-
U,
,x
r0
v .'
d\ F
0%
IIIII
I I
I
(D
-
0z0m-jZ0
.mw
0
I<
Z
Io>
I0
00
CIIE-
za z
-,bow
-
-7
PERCENTAGE OCCURRENCE 4278 Na
-_ N (C -w D 0D 0 o 0 0 0 0 0 0 0 0 0
I I
.98 76
5
I8 5179
I \ 7
4 9 5 2I 90 86
I I I I I I II I I I I I17 6789 9 II I I I Ill[ I I ~ f~l f I a-1 9~l 5,~p9.. -jqq-t.8 .
4
3
100 1000
'MEAN X 4278 INTENSITY (R)
Fig. 12
2
2D
z-4
r
-I
cm
o
Ir-
w0c20
;I
"I
H.oq
I0
o-
o_
I
09
o
0
7
6
' 5
oo
04
3i
2
i10I0
2
10000
I
I
oI I I I I I 0.1 1.0 10.0
MEAN ENERGY c( (KEV)
Fig. 13
AVERAGE ENERGY (KEV)
9 o o .- - -_o N A O oD 0 N
o
0 o
o CA 0 o C 00
ENERGY DENSITY
(eV CM-3 STER-
')
ENERGY FLUX
(ERGS CM" SEC" STER-')
0 0 0
N) P 4
I I I ZA 0
m0
>N U - w
0 ~ 0
m
z
APPROX. 4278) NINTENSITY CR) -
Fig. 14
-j
wI-
z
0
Z
a:W
Lii
z
a:w
a-
U
z
z
00
C)zm -
o e0"o
o O
r
-4c
i'n
w0
o400
10.0
0 TOTAL PRECIP FLUXx O- 0.15
W /0
az jx~3X108 ELEC./CM'SEC x
1.0X
-j //L /
- (KEV) O i.15 0.26
w~ELECTRON FLUX M E STER KEV)
- _
n.-
CD _
z _
o.I I.O
o (KEV) Fig. 15
ELECTRON FLUX (CM -
j
SEC-' STER-' KEyV - )
o0
mU
moO
0
_ 0
0
10.0
0,
10
ELECTRON ENERGY (KEV)
Fig. 16b
18
00
--- AURORAL OVAL, Q I
2/ "AURORAL" (I-10 KEV) AND 'HARD"DAYTIME PRECIPITATION
= DAYSIDE SOFT (0.1- 0.5 KEV ) ZONE
: NIGHTSIDE SOFT (0.5- 2 KEV) ZONE Fi-. !-,
- l0o
i>
y
I-
w
7uV)II
xo 1
-j
Z0
I-
iJ 10
0.1 I
18 0 I A 0
AURORAL OVAL, Q I
"AURORAL" (I-ZOKEV) AND "HARD"DAYTIME PRECIPI I TAT ION
ig . So
'~\\~~~~~~~~~~~~~~~~adal~\ '. .- ~~~~~~~~~~~~~~~~aaa~ ~;~·naaa~~·~~ : " aa'·
00~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
DAYSIDE SOFT {~,I KEV) ZONEFig. 17b
SOLAR
WIND
-1
ID
tD
"'' BOUNDARIES OF AURORAL OVAL
"AURORAL" (I -10 KEV) AND': "HARD" DAYTIME PRECIPITATION
NIGHTSIDE SOFT (0.5-2 KEV)In Z ZONE
PLASMASHEET
PAUSE
PROTON RING CURRENT
DAYSIDE SOFT ZONEELECTRONS 0.1- 0.5 KEVPROTONS ,5 I KEV
7NZ (PATCHES) -POLAR CAP AURORA?