observed and simulated depletion layers with southward imf · and boundary layers; magnetosheath;...

AFR'S-ATR2005 11060

Annales Geophysicae (2004) 22: 2151-2169 AASRef-ID: 1432-0576/ag/2004-22-2151 Annales© European Geosciences Union 2004 DISTRIBUTO STATEMENTA Geophysicae

Approved for Public ReleaseDistribution Unlimited

Observed and simulated depletion layers with southward IMF

N. C. MaynardI, W. J. Burke2 , J. D. Scudder 3, D. M. Oberl, G. L. Siscoe 4 , W. W. White1, K. D. Siebert',D. R. Weimer', G. M. Erickson4, J. Schoendorfl, and M. A. Heinemann 2

'ATK Mission Research, Nashua, New Hampshire, USA2Air Force Research Laboratory, Hanscom Air Force Base, Massachusetts, USA3Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA4 Center for Space Physics, Boston University, Boston, Massachusetts, USA

Received: 16 June 2003 - Revised: 21 January 2004 - Accepted: 9 February 2004 - Published: 14 June 2004

Abstract. We present observations from the Polar satel- 1 Introductionlite that confirm the existence of two types of depletion lay-ers predicted under southward interplanetary magnetic field The existence of depletion layers near the magnetopause was(IMF) conditions in magnetohydrodynamic simulations. The first suggested by Midgely and Davis (1963), who reasonedfirst depletion type occurs along the stagnation line when that the magnetic field draping around the magnetopause sur-IMF Bx and/or dipole tilt are/is present. Magnetic merg- face would be constrained to flow in one direction whileing occurred away from the equator (Maynard et al., 2003) plasma could flow in all directions. This leads to local mag-and flux pile-ups developed While the field lines drape to the netic field intensifications and attendant plasma density de-high-latitude merging sites. This high-shear type of deple- creases. Zwan and Wolf (1976) explicitly calculated plasmation is consistent with the depletion layer model suggested distributions in the vicinity of the magnetopause to model de-by Zwan and Wolf (1976) for low-shear northward IMF con- pletions near the subsolar stagnation point. The model doesditions. Expected sites for depletion layers are associated not allow for magnetic merging (Dungey, 1961) and applieswith places where IMF tubes of force first impinge upon the to cases of northward interplanetary magnetic field (IMF).

.. magnetopause. The second depletion type develops pole- Two mechanisms cause depletion layers. First, deflectionward of the cusp. Under strongly driven conditions, magnetic by the bow shock around the magnetopause causes plasmafields from Region 1 current closure over the lobes (Siscoe to move along the magnetic field lines away from the nose.et al., 2002c) cause the high-latitude magnetopause to bulge Second, compressional forces exerted on magnetic flux tubesoutward, creating a shoulder above the cusp. These shoul- squeeze plasma away from the subsolar magnetopause alongders present the initial obstacle with which the IMF inter- draped field lines. This results in enhanced magnetic fieldsacts. Flow is impeded, causing local flux pile-ups and low- coupled with decreased plasma density. They predicted de-shear depletion layers to form poleward of the cusps. Merg- pletion factors, ratios of the post-shock to local densities, be-ing at the high-shear dayside magnetopause is consequently tween 3 and 4. Analyses of IMP-6 measurements showed de-delayed. In both low- and high-shear cases, we show that the pletion factors that varied from 1.4 to more than 2 (Crookerdepletion layer structure is part of a slow mode wave stand- et al., 1979).ing in front of the magnetopause. As suggested by South- If merging is occurring at the subsolar magnetopause,wood and Kivelson (1995), the depletions are rarefactions on plasma flow in the X direction does not completely stagnate,the magnetopause side of slow-mode density compressions. eliminating magnetic field pileup. In a sense, the existenceWhile highly sheared magnetic fields are often used as prox- of a depletion layer is an indicator of a locally closed mag-ies for ongoing local magnetic merging, depletion layers are netopause, since magnetic merging would carry away theprohibited at merging locations. Therefore, the existence of a magnetic flux and prevent its buildup. Depletion layers aredepletion layer is evidence that the location of merging must common near the nose of the magnetopause when the IMFbe remote relative to the observation. is northward or nearly in the direction of the Earth's dipoleKey words. Magnetospheric physics (magnetopause, cusp magnetic field (low-shear condition). Depletion layers haveand boundary layers; magnetosheath; magnetospheric con- also been observed for high shear conditions (IMF clock an-figuration and dynamics) gle greater than 600) (Anderson and Fusilier, 1993). Mag-

netic merging is commonly believed to be the primary means

of coupling the solar wind energy into the magnetosphere.Correspondence to: N. C. Maynard It is important to understand why some high-shear magne-([email protected]) topause crossings have depletion layers, since their existence

20050620 138

2152 N. C. Maynard et al.: Observed and simulated depletion layers

seemingly precludes merging, at least locally. In this pa- Motivated by the observation of a density enhancement inper we explore the causes of high magnetic-shear depletion front of the magnetopause (Song et al., 1990; 1992), South-layers by comparing satellite observations with magnetohy- wood and Kivelson (1992) argued that a slow MHD shockdrodynamic (MHD) simulated predictions of the Integrated must form in the magnetosheath behind the bow shock. De-Space Weather model (ISM) code (White et al., 2001). pending on pressure anisotropy, it should stand in the sheath

AMPTE/IRM data indicate that depletion layers are com- flow ahead or behind the intermediate wave (rotational dis-mon at a low-shear (<30') magnetopause (Phan et al., 1994). continuity) at the magnetopause. A standing slow modeWith a high-shear (>60') magnetopause they identified no wave would enhance the density and decrease the magneticsystematic behavior. Anderson and Fuselier (1993) reported field, opposite to the predictions of Zwan and Wolf (1976).that depletions could be found for all orientations of the IMF Southwood and Kivelson (1995) recognized that the observa-but that decreases were small when the IMF had a south- tions of Song et al. (1990, 1992) and the mechanism of Zwanward component. Anderson et al. (1997) defined a parame- and Wolf (1976) both manifest slow mode properties, namelyter D=ERIESW as an indicator of merging efficiency. Here a fluctuation in AIBI=-aAn. They suggested that the twoER is the reconnection electric field and Esw is the solar models could be reconciled if the slow-mode waves were de-wind electric field. D=1 corresponds to no depletion while tached from the magnetopause. Behind the detached shock,D=O corresponds to maximum depletion. They showed magnetic fields should deflect toward the magnetopause. En-that the merging efficiency was a factor of 3 larger during hanced magnetic fields and plasma depletions develop at theAMTE/IRM (Phan et al., 1994) than AMPTE/CCE (Ander- nose, earthward of the plasma compression at the wave front.son and Fusilier, 1993) observations. This result was ad- The J x B force of the current in the wave results in a netvanced as a reason why Phan et al. (1994) failed to detect force that deflects flow away from the nose. We note fur-systematic depletions during high shear situations. They as- ther in this vain that the wave discussed by Southwood andsociated the cause to a 3-fold higher P for the CCE events. Kivelson and the depletion predicted by Zwan and Wolf mayHence, they expect that high-shear depletion layers occur be viewed as one half cycle of a slow mode disturbance thatwith high solar wind densities. Farrugia et al. (1995) con- should be expected in front of any locally closed portion ofcluded that depletion layers were possible for high magnetic the magnetopause.shear whenever the upstream Alfv~n mach number was low. Region 1 current streamlines close through the high lat-

Maynard et al. (2003) used Polar and Cluster data to show itude boundary layer of the magnetosphere (Siscoe et al.,that merging often occurs at high latitudes. They described 1991, 2000). These streamlines come out of the dusk sidedetailed characteristics of an event on 12 March 2001, in ionosphere, follow magnetic field lines to near the mag-which a depletion layer was observed just outside of the netopause in the equatorial region, curl up over the high-magnetopause while merging was occurring poleward of the latitude magnetopause to the dawn side near equatorial re-spacecraft. The event occurred during a high-magnetic-shear gion, and then follow magnetic field lines back to the iono-interval when the IMF clock angle was -140'. sphere as morning side region 1 currents. A similar loop

Wu (1992) was first to report depletion layers in MHD is located in the Southern Hemisphere. Both loops con-simulations. The layer was thicker but the depletion fac- tribute to the weakening of the magnetic field at the sub-tor (1.2) was less than predicted by Zwan and Wolf (1976). solarmagnetopause and the increase of it in the lobe. UnderMore recently, Siscoe et al. (2002a) used ISM simulations strongly driven conditions, the lobes bulge out sunward andto demonstrate the systematic variations of depletion layers the cusps move equatorward (Raeder et al., 2001). Siscoe etwith IMF clock angles. Depletion factors >3 appear for al. (2002b) describe the bulge (or deformation of the mag-all cases with the shear <90'. The thickness of depletion netopause boundary) located above the cusp as a "shoulder",layers decrease with increasing IMF clock angles. Wang et which is the terminology used here. The lobe magnetic fieldal. (2003) showed from MHD simulations for northward IMF is nearly in the same direction as the draped IMF; hence, thisthat the depletion layer existed all around the dayside and be- is a locally low-shear boundary encountered above the cusp.came thicker away from noon. It was also well defined in the in the following sections we demonstrate that the depletionnoon-midnight plane past 400 magnetic latitude. In this pa- layer reported in Maynard et al. (2003) occurred near a veloc-per we wish to emphasize the generality ofZwan-Wolf deple- ity separator. ISM simulations show that the observations oc-tions and related effects at all locations on the magnetopause curred in a region where depletion is expected. We then usewhere the local magnetopause is "passive" (not merging) and ISM simulations to show that under strongly driven condi-particularly at the subset of such locations where the IMF tions with southward IMF, low-magnetic-shear shoulder con-first encounters the magnetopause as a blunt body. figurations develop poleward of the cusp. These shoulders

Siscoe et al. (2002a) also pointed out that in ideal, incom- impede the flow of magnetic flux toward the nose, requiringpressible MHD the stagnation point becomes a line along the field lines to drape around the shoulder before they canwhich the plasma velocity is identically zero. In the absence merge at the dayside magnetopause. In so doing they cre-of merging, the magnetic field that passes through a stagna- ate a depletion layer above the cusp. Polar measurementstion point lies on the magnetopause surface and is an MHD confirm this ISM prediction. Both types of depletion layersmandated stagnation line (Sonnerup, 1974). As such it is a are possible under high-shear, sub-solar magnetopause con-velocity separator line along which the plasma flow diverges. ditions. The first is tied to merging away from the sub-solar

N. C. Maynard et al.: Observed and simulated depletion layers 2153

region. The second type inhibits dayside merging and is a ionosphere/thermosphere. The simulations discussed herepossible mechanism for understanding the saturation of the contain specifically selected parameters and simplifying ap-ionospheric potential under strongly driven conditions (Sis- proximations. Finite-difference grid resolution varies from acoe et al., 2002b, c). few hundred kilometers in the ionosphere to several RE near

the computational domain's outer boundary. At the magne-topause, resolution ranges from 0.2 to 0.8 RE. Explicit vis-

2 Measurements cosity in the plasma momentum equation was set to zero.To approximate nonlinear magnetic reconnection the explicit

In 2001 Polar's apogee (9 RE) was near the equator. As resistivity coefficient v in Ohm's Law equation is zero if cur-a consequence, for long intervals in March-April the orbit rent density normal to B is less than 3.16.10-3 Am-2 . In re-

s k i m m e d f r o m s o u t h t o n o r t h , a l o n g t h e d a y s i d e m a g n e - ge n n sd w i t ht p e r p e n d i c u l a ri c u r r e n tt d e n s i t i e s 0 a b o v e t h I n r e -

topause. Thus, variations in phenomena observed by Polar gions with perpendicular current densities above this thresh-old, v=2-10 1° m2s-1 . In practice, this choice of v leads to

are primarily temporal rather than spatial. Information about

radial scale sizes is lost. However, Polar closely monitors non-zero explicit resistivity near the subsolar magnetopause,and in the nightside plasma sheet. Dissipation, where needed

magnetopause responses to temporal changes of the IMF and to maintain numerical stability, is based onthe partial donor-solar-wind pressure. Several sensors on Polar are used in

this study. The Hydra Duo Deca Ion Electron Spectrometer cell method (PDM) as formulated by Ham (1987).

(DDIES) (Scudder et al., 1995) consists of six pairs of elec- In the following discussion we present the results of five

trostatic analyzers looking in different directions to acquire simulations. The input solar wind parameters for each runhigh-resolution energy spectra and pitch-angle information, are given in Table 1. Because of their negligible impact on

Full three-dimensional distributions of electrons with ener- the results and in order to reduce run times of simulations,

gies between 1 eV and 10 keV and ions with energies per routines in the ISM code containing thermospheric hydrody-ratio of 10 eV q- to 10 keV q- were sampled ev- namics and explicit chemistry between ionospheric and ther-

charger atio.os. 10e electo field were sarvey et mospheric species were not activated. Ionospheric Pedersenery 13.8 s. The electric field instrument (EFI) (Harvey et conductance is 6 S at the pole and varied in latitude as B-2 .

al., 1995) uses a biased double probe technique to measure It is uniform in longitude. No Hall conductance was used.

vector electric fields from potential differences between 3 or-

thogonal pairs of spherical sensors. This paper presents mea-surements from the long wire antennas in the satellite's spinplane. The Magnetic Field Experiment (MFE) (Russell et 4 Depletion layers with northward IMF

al., 1995) consists of two orthogonal tri-axial fluxgate mag- To set the stage for the depletion layers when the IMF hasnetometers mounted on non-conducting booms. The electric southward components, we first examine conditions on 31and magnetic fields were sampled 40 and 8 s-1, respectively. s ar d ucomponents, we te e Itions ong31Daapresented in this paper were spin averaged using a least- March 2001, during a period when the IMF was stronglyData resents in tis northward and Polar's orbit was skimming along the daysidesquares fits to a sine function. magnetopause near the equator. Data from 08:00 to 11:00 UT

The Advanced Composition Explorer (ACE) spacecraft are plotted in Fig 1. Figures 1 d-g present energy-versus-timemonitors interplanetary conditions while flying in a halo or- a re ot in energy-me RAustspectrograms of ion energy fluxes measured by HYDRA atbit around the L 1 point in front of the Earth. The solar wind all pitch angles and parallel, perpendicular, and antiparallelvelocity was measured by the Solar Wind Electron, Proton, to the local magnetic field. The plotted numbers are the av-and Alpha Monitor (SWEPAM) (McComas et al., 1998). A erage ofd2f/dE/dS2 over solid angles in which data weretri-axial fluxgate magnetometer measured the interplanetary taken. Some investigators integrate over solid angle and re-magnetic field vector (Smith et al., 1998). port f(d-f/dEd•2)d•2 as the "omnidirectional" energy flux.

The entire velocity distribution at all solid angles must be3 The Integrated Space Weather Prediction Model sampled to make such a determination. We avoid interpo-

lating and report the average of the integrand over all direc-The Integrated Space Weather Prediction Model (ISM) op- tions sampled, which at a 13.8 s cadence covers 12 * 6=72erates within a cylindrical computational domain whose ori- directions distributed over a unit sphere. Figure l a, the blackgin is at the center of the Earth. Its domain extends 40 RE trace, shows Bz measured by Polar. The green trace indi-sunward, and 300 RE in the anti-sunward direction, and cates By. In Fig. lb the blue line indicates the solar wind60 RE radially from the Earth-Sun line. In simulations de- density measured by ACE and lagged by 38 min. While thescribed here, the cylindrical domain has an interior spherical lag time may vary minute-by-minute (Weimer et al., 2002),boundary approximately located at the bottom of the E-layer we have chosen 38 min as providing the best average match(100 km). The cylindrical to spherical interface is at 3 RE. over the plotted interval. In this case the lag time is close

ISM uses standard MHD equations augmented by hy- to the advection time and is adjusted by matching clock an-drodynamic equations in the collisionally-coupled thermo- gles of magnetic fields measured by Polar and ACE (Song etsphere. Conceptually, as one moves toward the Earth, equa- al., 1992). Matching clock angles provides reasonable lagstions transition continuously from pure MHD in the solar for both B and density, except when IMF Bx is the domi-wind and magnetosphere to those proper to the low-altitude nant component. Figure Ic compares the magnitude of the


Table 1. Simulation input parameters.

# Solar Wind velocity Solar wind density IMF magnitude IMF clock IMF Bx Dipolevelocity (km/s) density (protons/cm3) (nT) angle (degrees) tilt (degrees)

1 350 5 5 135 negative 02 350 5 5 180 0 173 350 5 20 180 0 174 350 5 20 180 0 355 350 5 50 180 0 0

3/31/01: 0900 UT: Bz north depletion layer at nose200 ... .1000 B ....

0 -, - -- -- .. ... ... ... . .. ... ... ... .. B ... ... .SM

- 100 Magnetosheath Magnetopause Magnetosheath By-GSM-200

200 N - PolarE 150

1 0050 b Shocked N - Ace

Xl -200 113 -•B Polar

150100

5pDepletion Dep. Depletion Shocked 1BI - Ace10 107103 410ý A W 106,,t ,@, > -O

10 107

0 0• 107

5ý103." • 106

10• 105

08:00 08:30 09:00 09:30 10:00 10:30 11:00 time (UT)31Maor2001 dote•

-68.99 -69.33 -69.71 70.11 70.54 70.98 71.44 ILT1131 1135 1138 1142 1145 1148 1151 MLT7.53 7.93 8.29 8.59 8.85 9.06 9.23 R7.8 8.0 8.3 8.6 9.0 9.4 9.9 L-10.2 -5.7 -1.4 2.7 6.6 10.4 14.1 MAGAT

Polar at nose near 0° MLAT and 1140 MLT

Fig. 1. Example from Polar of depletions layers with IMF Bz northward. Polar was located at 00 MLAT and 11:40 MLT. (a) The blacktrace is the measured Bz at Polar. The green trace is the measured By. The larger value of BZ just outside the magnetopause is a signatureof a depletion layer. (b) The measured ion density at Polar (black) compared to the properly lagged (38 min) ion density measured at ACEupstream in the solar wind (blue). Plasma densities attributed to ACE have been multiplied by a time-varying factor appropriate for density

jumps predicted by the Rankine-Hugoniot relations for the subsolar bow shock and by an additional compression factor when Polar wasclose to the magnetopause as predicted by Spreiter and Stahara (1985). (c) The magnetic field magnitude measured at Polar (black) and at

ACE (blue). ACE magnetic field measurements were multiplied by the time-varying Rankine-Hugoniot factor appropriate for the magneticfield jumps at the subsolar bow shock. (d-g) Ion energy spectrograms showing the total, parallel (pitch angles 0-30°), perpendicular (75-1050) and antiparallel (150-180O) ion fluxes ((cm 2 -s-sr.-AE/E)-I). Three intervals noted by X, Y, and Z indicate the data on which the

regression analyses of Fig. 11 were performed.


3/12/01: Separator depletion layer - +By IMF clock anglenear 1400

100 :

50 BZ.GSM0 . B

-50o Magnetopause /By'GSM-100

2050 N - Polar

l5O b Shocked N - Ace

80 IBI - Polar206 • Shocked 1BI - Ace

1°3 l• d • -1061024 -- & 7,:,... . -0

g r 106

103 M 6> 105

1 i

10 "10r200 1 "te

10 5 1 1312= 135 3110

109. 9 1

10.50 4 17. 21.4 24.9 imeLT)

P1o0l a 180 M2 1 MLT

r. 3 0 130 13201 1 1 L

91 5 9. 041,1, 10

10. 10. 6782. 49 MGA

Polar00 dotno cite LTan 31 L

Fig. 2. Example of a depletion layer for negative BZ and positive By in the same format as Fig. 1. Polar was located at 180 MLAT and13:12 MLT.

magnetic fields measured by Polar and ACE with the same improvements with a simple change. Hydra densities weretime delay. To make the comparisons with Polar data, it is calibrated against those measured by ACE during the inter-necessary to adjust the ACE density and magnetic field for val between 12:30 and 13:00 UT when Polar was in the solar

effects of the bow shock. The ACE magnetic field and so- wind.lar wind density have been multiplied by time varying fac-tors calculated using the reduction of the Rankine-Hugoniot At the location of Polar the imposed IMF turned north-

equations by Whang (1987), which predicts the jump factors ward near 08:20 UT and the magnetosheath ion distributions

based solely on the upstream conditions. As such, the values became increasingly dominated by the perpendicular fluxes,represent the expected magnetosheath density and magnetic or "pancake" shaped, as antiparallel and parallel fluxes disap-

field just inside the bow shock. All factors were calculated peared. The magnetic field's magnitude increased by a factor

for the conditions at the nose. Typical factors for density of 1.7 above the shocked IMF (Fig. Ic). The density de-

range between 3 and 4. The magnetic field factor is more creased (Fig. lb) relative to the adjusted solar wind density.

variable, depending on whether the shock is more perpendic- The lower density and increased magnetic field just outside

ular or parallel. They range from 1 for a purely parallel to the the magnetopause are the predicted signatures of depletion

factor appropriate for the density with a perpendicular shock. layers (Zwan and Wolf, 1976). The pancake ion distributions

ACE density measurements were adjusted to allow for lati- are a natural result of the Zwan and Wolf mechanisms. This

tudinal variations of the compressed magnetosheath plasma, trend continued until 08:54 UT when the spacecraft crossed

as prescribed by Spreiter and Stahara (1985). No further ad- the magnetopause into the boundary layer, marked by an

justment was made on the ACE magnetic field since their abrupt change in ion spectral characteristics and a decrease

compression depends on several factors, negating possible in B and Bz. During magnetopause crossings with no deple-tion layers, the magnetic field is expected to be larger in the


Particle source compared to dawn-dusk velocity ~140' clock anglePolIar/EFI ... 2001,/03/12

F 5

2 0

-15,,

S 10 - Boundary layer Magnetosheath

0) 0-, ,1r fr -l00~

-10i(n• -l a b c d--15

100 us

-50

- I DO Dawn-150 *1

1146 1147 11 4B 1149 1150UT

Particle sources S. H. * N.H.

Fig. 3. High resolution (40 Hz) measurements of the 2 components of the electric field in the spin plane and the resulting drift velocity alongthe spin axis, which is roughly in the Y direction (toward dusk). The letters refer to panels in Fig. 8 of Maynard et al. (2003). The circulardumbells represent intervals when fluxes are coming from below the satellite, while the diamond dumbells represent times when ions arecoming from a Northern Hemisphere source above the spacecraft.

lower density boundary layer. Polar crossed back into the de- The examples with southward IMF components that fol-pletion layer at 09:22 UT as the increased density observed low show data in the same format as Fig. 1. Evidence for de-by ACE (blue trace in Fig. lb) rapidly pushed the magne- pletion layers include (1) ion distributions favoring perpen-topause inward. The depletion layer was quickly crossed, dicular pitch angles, (2) densities at Polar below the shockedand at 09:35 UT there was a significant increase in density ACE values, and (3) increased magnetic fields above theand a decrease in magnetic field. We return to this point in shocked ACE values. Ion distributions. in.the sub-solar mag-Sect. 7. After 09:40 UT the plasma density at ACE decreased netosheath become more pancake shaped as the magneticand the magnetopause expanded to closer to the location of flux piles up in the stagnated region.Polar, placing the satellite back into the more depressed den-sity of the depletion layer, where it remained for a consider-able interval. Compared with shocked ACE measurements, 5 Velocity separator depletion layersthe maximum increase in B at Polar was by a factor of 2.Note that at both ends of Fig. I c the magnetic field magnitude Maynard et al. (2003) identified a merging event at high lat-returns to close to the shocked IMF value, while in Fig. 1 a itudes during the Polar magnetopause crossing at 11:48 UTthe Z component is southward, favorable to dayside merging on 12 March 2001. Accelerated ions and Poynting flux car-with no depletion. Hence, variations in measurements at Po- ried by Alfv~n waves were observed coming from polewardlar reflect temporal responses to boundary motions and the of the spacecraft, on both the magnetosphere and magne-solar wind drivers. However, we cannot use Polar measure- tosheath sides of the current layer. After crossing the magne-ments to determine the thickness of the depletion layer. topause Polar entered a region of low plasma density within

the magnetosheath. Figure 2 presents HYDRA and MFE


data from Polar for this crossing (some of which is repeated Zwan and Wolf, 1976). Positive IMF Bx causes flux to en-from Fig. 6 of Maynard et al., 2003). Figure 2 is presented counter the stagnation line north of the equator first, enhanc-in the same format as Fig. 1. Figures 2d-g show ion energy ing the flux pile up at that point. Note that if componentfluxes in spectrogram formats. Figure 2a presents IMF By merging had been occurring near the equatorial region, noand Bz components measured by Polar as being comparable flux pile up would have developed as field lines would havewith an average clock angle of -140°. A positive IMF Bx been immediately dragged in the dawn or dusk direction.also was present. Note that just outside the magnetopause To explore this scenario, we utilized an existing ISM simu-crossing the parallel and anti-parallel ion fluxes were very lation (Simulation 1 in Table 1) with equal magnitudes for allsmall. Perpendicular fluxes dominated but at reduced levels IMF components; Bx and BZ negative and By positive. Thecompared to those detected after 12:15 UT. Figure 2b com- negative IMF Bx places the first contact point to the stag-pares the density measured by Polar with that measured by nation line south of the equator on the dawn side of noon,the ACE satellite. Here ACE data were lagged by 63 min, comparable to the observations at Polar on the dusk side ofwhich proved optimal for the magnetopause crossing as de- noon north of the equator with IMF BX > 0. Figure 4a showstermined in Maynard et al. (2003). Ion densities detected ion velocity vectors and contours of Bz in the YZ plane atjust outside the magnetopause were less than or comparable X=9.9 RE. The tan colored region represents the nose ofto those of the shocked solar wind as observed by ACE. B the magnetosphere with positive Bz; the color blue indicatesremained above the shocked IMF value until a major IMF negative Bz and open field lines. In the region of open fielddecrease occurred near 12:18 UT. The maximum enhance- lines noted by arrows, Figs. 4b and c show decreased densityment of the magnetic field was by a factor of 1.9. Reduced and increased magnetic field, respectively. The simulationdensities and corresponding enhancements in B are clear in- provides the signatures of a depletion layer in the region ofdications of depletion layers. Note that the density minimum the first contact with the stagnation line, comparable to theobserved at 12:00 UT does not correspond to a change in the Polar measurements described above. The depletion in den-solar wind density, but to an increase in the total magnetic sity of about 1.3 is less than measured but comparable to val-field (Fig. 2c). Temporal changes in the depletion, such as ues of 1.3 and 1.2 reported by Wu (1992) and Lyon (1994),observed at 12:00 UT, most likely reflect a small movement respectively, in depletion-layers simulations with northwardof the magnetopause, placing the satellite deeper inside the IMF, using other MHD codes. The depletion is localizedlayer. south of the equator and primarily in the vicinity of the stag-

Signatures of accelerated ions appear in three of the nation line, although it also extends across noon with some-four particle distributions shown in Fig. 8 of Maynard et what weaker levels of enhanced B. The negative Bx in theal. (2003), to demonstrate that merging was occurring at high simulation places the first contact point south of the equator,latitudes to the north of the spacecraft. The accelerated ions in the prenoon sector (Fig. 4). Had the simulation run within the other example came from the south. This suggests positive IMF BX, the first contact point and strongest sig-that Polar was located near the velocity separator line, or the nature of depletion would occur north of the equator in themagnetic field line that passes through the stagnation point postnoon sector. This compares favorably with the locationat the nose. Sonnerup (1974) showed that in incompress- of Polar. The presence of IMF Bx can enhance the depletionible MHD the stagnation point stretches into a line along B. as does dipole tilt. Maynard et al. (2003) showed that theLater, Siscoe et al. (2002a) demonstrated this effect with the merging site moved off the equator and away from the pointISM code. On the dawn (dusk) side of this line plasma flows of first contact with increasing dipole tilt. IMF Bx >0 at Po-toward dawn (dusk). To test the conjecture that Polar was in lar serves to enhance the effective dipole tilt and increase thethe vicinity of the stagnation line, Fig. 3 plots the two electric depletiorr. Siscoe et al. (2002a) showed that the depletion isfield components measured in the spin plane of the spacecraft minimal when IMF Bx =0 and the dipole axis is vertical. Theand the velocity along the spin axis calculated using those simulation has a current-dependent, explicit resistivity at thecomponents during the magnetopause crossing. The spin nose, which favors merging at that location. In the simulationaxis points close to the dawn-dusk direction. The intervals the neutral line moved away from the subsolar region, indi-over which the particle distributions shown in Fig. 8 of May- cating a strong preference for high-latitude merging when thenard et al. (2003) were taken are noted with square (circular) dipole is tilted.dumbbells for distributions originating north (south) of the If IMF By had been negative and Bx positive, the de-spacecraft. The letters refer to the labels in Fig. 8 of Maynard pletion layer would have been located on the dawn side ofet al. (2003). Where the particle source was south (north) of noon in the Northern Hemisphere. Such a case was observedthe spacecraft or from the Southern (Northern) Hemisphere, briefly at -11:30 MLT (near 08:00 UT) on 16 April 2000,the velocity was toward dawn (dusk), as anticipated. This is when Polar was moving northward and toward dusk alongconsistent with Polar being located near the stagnation line the magnetopause. Figure 5 displays similar quantities toor velocity separator. those in Figs. 1 and 2 between 06:00 and 11:00 UT. Polar ini-

Since incoming magnetic flux in the magnetosheath drapes tially crossed the magnetopause at 07:10 UT. Approachingover the magnetopause before reaching high-latitude merg- the current layer on the magnetosphere side, Fig. 5a showsing sites, flux pile up must occur near this stagnation line that the angle of B rotates to -45' as the current layer is en-and a depletion layer should form (Midgely and Davis, 1963; tered and then to 900 IMF orientation on the outside of the


Ion velocity vectors and Bzaon open on closed

field lineslines

Negative BZ

-10 -50

1-() Bz (nT) Magnetopause-20 -12 -4 4 12 20 nose

H+ number density X= 9.9 REDepressedDensity

Magnetosphere.o -5 o 5 nose

13 14 15 16 17 18

Fig. 4. Results from a MHD sim-Enhanced B Magnetic field magnitude ulation with a constant IMF input ofmagnitude equal magnitude negative Bx, positive

By and negative Bz. The simulationoutput is presented in the YZ planeat X=9.9 RE, which just contacts thenose of the magnetosphere. (a) Veloc-ity vectors are overlaid on the planecolored with Bz. Brown colors indi-cate closed magnetosphere field lines,while blue colors indicate open magne-tosheath or boundary layer field lines.(b) The plane is colored with the pro-ton number density. (c) The plane is

-1o .5 GSEY(F,) o 5 B (nT) colored with the magnitude of the mag-..... I netic field. A ttention is called to the

6.9 13.0 19.1 25.3 31.4 37.5 region below and to the left of center

in each panel, where depressed densityIMF: - Bx; +By; -Bz and enhanced B are seen on open field

lines.


Strongest depletion at

4/16/00: Separator depletion layer - -By clock angle near 135'

1005 Magnetopause crossings0 a. BZ-GSM

_-501 0•.......... • 1 By-S

N -Polarb Shocked N - Ace

80 X Yg 13 - Polar60

28 Depletion Shocked B3[ - Ace

10 Um 107

103 -106

10 105

10,2 107

S1.`. f >mll ,10 10

10-

10 - 'r 106

102 0 rR% 105

06:00 07:00 08:00 09:00 10:001:0 tmeUT1 6Apr2000 date

70.79 72.01 73.27 74,62 76.09 77.73 ILT1115 1123 1132 1142 1153 1206 MLT865 9.03 9,25 9.31 9.21 8.94 R9.2 10.5 12.1 14.2 17.3 22.2 L

15.1 22.0 28.9 35.9 43.1 50.5 MAGLAT

Fig. 5. An example from Polar located prenoon at 300 MLAT and 11:32 MLT in the same format as Fig. 1. The signatures of depletionare seen briefly just before 08:00 UT when IMF By is negative and comparable to BZ. Subsequently, as the magnitude of By decreases,antiparallel ion fluxes and the total ion density return from merging somewhere below the spacecraft. Depletion is seen on the dusk side ofnoon for the opposite polarity of By near 10:00 UT. Three intervals noted by X, Y, and Z indicate the data on which the regression analysesin Fig. 12 were done.

current layer. This rotation in the boundary layer is consis- pletion encounter was brief, becoming most intense after atent with MHD simulations (Maynard et al., 2001). The IMF flux transfer event at -07:54 UT. Soon after this By returnedand Polar B quickly rotated from a clock angle of 900 to a to zero, and the depletion interval ended as ion densities mea-strongly negative Bz, concurrent with an increase in the den- sured by Polar increased to the adjusted ACE densities.sity. At this prenoon local time and 220 magnetic latitude,the magnetosheath density followed the adjusted solar wind A second region of depletion, identified by enhanced B

density, but at a slightly lower level. The magnitude of B in- and pancake particle distributions, appears in Fig. 5 after

creased. However, the ion fluxes were strongest in the direc- 09:30 UT. Polar was located near magnetic noon and at a

tion parallel to the magnetic field. The ion temperature was magnetic latitude >40'. By was positive, similar to the con-

higher than that observed in the magnetosheath after the next ditions of 12 March 2001. Figure 4 shows that the region

magnetopause crossing. The solar wind density decreased of depressed density and enhanced B extends to noon from

near 07:30 UT, and the magnetopause briefly expanded to the the maximum near the velocity separator, suggesting that Po-

location of Polar at 07:35 UT. Beyond this second outbound lar accessed the depletion region. The depletion increased

magnetopause crossing By became negative and comparable with time as evidenced by the increase in B and the de-

in magnitude to Bz. At this time the velocity separator lo- crease in parallel and antiparallel ion fluxes until 10:10 UT.

cation would be prenoon in the vicinity of the satellite. Near The density remained relatively constant near adjusted ACE

08:00 UT evidence of a mild depletion layer is seen in the values; however, the electron pressure and temperature (not

density and magnetic field (noted by the blue bar). The de- shown) decreased commensurate with the increase in B.Near 10:20 UT an increase in the solar wind density pushed


170 tilt IMF Bz =-5 nTMagnetic field vectors

Effects of increaseddriving with dipole tilt:

Narrows distance___between cusps

-5

Creates a shoulder-10 1above cusps

GSE X (R,) o

B (nT)0 25 50 75 100

170 tilt IMF Bz = -20 nT 350 tiltMagnetic field vectors Magnetic field vectors10•

.... 1'

b c

5

w0 r

-5 -5J

-10 -5 a 5 10 15 20 -10 -5 0 a 10 15 20GSE X (R,) OSE x Cs,

0 25 50 75 100B(nT) 0 25 50 75 100 B (nT)

Fig. 6. Simulation of the effects of increased dipole tilt and increased magnitude of the IMF. All panels show the XZ plane at Y=0. Thearrows show the direction of the magnetic field and are colored with the magnitude. (a) and (b) have the same dipole tilt but change the IMFdriver. (b) and (c) have the same input driver, but change the dipole tilt. Note that the increased IMF driver compresses the cusps togetherand starts to build a shoulder of enhanced magnetic field above the cusp that is tilted toward the Sun. Increasing the dipole tilt increases thesize and strength of the shoulder.

the magnetopause toward the Earth, away from Polar, and a 6 Shoulder depletion layerssharp increase in density was seen at Polar, located at mag-netic noon and about 450 magnetic latitude. This sharp in- ISM simulations predict a second type of depletion layer withcrease was similar to that observed after 09:22 UT on 31 southward Bz when the IMF strength increases. Maynard etMarch (Fig. 1) and the two results will be compared in al. (2003) gives an example of merging moving away fromSect. 7. the equator with increased dipole tilt, with a purely south-

ward IMF. Recall that IMF Bx adds or subtracts to the ef-fective dipole tilt (Crooker, 1992). Figure 6 shows the ef-fects of combining dipole tilt and increasing the IMF mag-

Velocity-separator depletion layers are more localized nitude. Figure 6a shows magnetic-field vectors colored withthan those found under northward IMF conditions, which ex- the magnitude of the magnetic field for simulation 2 (Table 1)tend all around the dayside (Wang et al., 2003). They cannot with 170 dipole tilt and a -5 nT Bz as the driver. The magne-form if the merging is confined to the subsolar region. Thus, topause and cusps are evident in the vector patterns. Increas-their presence indicates high latitude merging. We reiterate ing the driver to -20 nT in simulation 3 (Table 1), shown inthat Polar provides no information on the thickness of a de- Fig. 6b, causes the cusps in the outer magnetosphere to movepletion layer. Due to the skimming nature of the trajectory, toward the equator, shrinking the dayside magnetosphere atwe lack knowledge about its exact relationship to the magne- sub-cusp latitudes. A shoulder, or a region of open field lines,topause. develops above the Northern Hemisphere cusp and extends


Shoulder Depletion with Bz = -20 nT and - 350 dipole tilt

Ion velocity and log B Magnetic field lines and velocity magnitude3

a b2 It Velocity

Increased B minimum

-2

-3 -38 7 8 9 10 11 12 6 2oSE X (RE) Log B (nT) V (km/s)

0.5 0.8 1.1 1.4 1.7 2.0 20 56 92 128 164\ 200

Magnetic field lines and mass densityOpen-IMF

2 Decreased boundary

" density

NOO

-2

-2

Ion mass 3 Ion mass-36 7 8 9 10 11 12 (kg/m 3) density (kg/r 3)

GSE X (RD) density (k/MSdesty(

4 8 12 16 20E-21 0 4 8 12 16 20 E -21

Fig. 7. Details of the shoulder depletion layer depicted in Fig. 6c. All panels display the XZ plane at Y=O. (a) Ion velocity vectors overlaidon the plane colored with the log of B. (b) Traced magnetic field lines with the velocity magnitude as the background. The yellow field linesare open and connected to the Northern Hemisphere ionosphere. The green field lines are open to the solar wind on both ends. A velocityminimum is seen just inside the open/IMF boundary. (c) Mass density and (d) mass density with the traced magnetic field line overlay. Thedecreased density and the enhanced B seen in (a) are co-located at the open-IMF boundary.

sunward of the sub-solar magnetopause. In part, the shoul- one foot in the Northern Hemisphere ionosphere and greender results from strong Northern (summer) Hemisphere re- if both ends connect to the solar wind. The change in colorgion 1 currents that close through the low-latitude bound- marks the open-IMF field boundary or "outer separatrix" ex-ary layer and along the high-latitude magnetopause. Fig- tending to an active merging separator. Because of the dipoleure 6c shows the shoulder expanding with increased dipole tilt merging occurs below the equator in the Southern Hemi-tilt to 350. Green colored vectors extending out into the mag- sphere. Thus, the Northern Hemisphere cusp contacts thenetosheath above the cusp indicate the presence of a large magnetosheath south of the equatorial plane. The light pur-magnetic field and the possibility of a depletion layer. The pie in the region near X=9 and Z=l-3 RE indicates an in-shoulder represents the first point of contact between a purely crease in B in the shoulder region at the outer separatrix.southward IMF and the magnetosphere. Magnetic field vec- The green region behind the outer separatrix in Fig. 7b rep-tors in Figs. 6b and c are seen to drape around the shoulder. resents a plasma velocity minimum that occurs in a stagna-

tion region where velocity vectors turn poleward and mag-Figure 7 displays plasma densities and magnetic fields netic field lines are swept back over the magnetopause. Fig-

observed near the magnetopause poleward of the Northern- ures 7c and d show plasma density contours. Magnetic fieldHemisphere cusp for simulation 4 (Table 1), depicted in line traces are also overlaid in Fig. 7d to highlight the outerFig. 6c. Figure 7a plots velocity vectors over contours of separatrix by the change from yellow to green magnetic fieldthe log of the magnetic field. Figure 7b traces magnetic lines. The reddish color overlaid by the separatrix reflects de-field lines over contours of the magnitude of ion velocity, creased plasma density in the depletion layer. The magneticTraced field lines are colored yellow if they are open with


Shoulder depletion from Bz = -50 nT and no dipole tiltMagnetic field lines and lo B Magnetic field lines and magnetic pressure

Increased Band magneticpressure

4 0 S6 GSE 6 7 a 9 Magnetic(Eo X (9, pressure (J/m

3)

0.5 0.8 1.1 1.4 1.7 2.0 0 4 6 8 10E-8

Open-IMF boundaryMagnetic field lines and mas ensity Magneti field lines and velocity magnitude

6

Decreased d sdensity

4

Velocityminimum 2

0 I 9 on mass 0 OGSE 3 4 8 9X (9,) density (kg/m3) GSE X (RE) V (km/s)

1.0 1,8 2.6 3.4 4.2 5.0 30 84 138 192 246 300

Fig. 8. Shoulders develop above both cusps in simulations with no dipole tilt, but with exceptionally strong driving IMF (50 nT). The panelsdisplay a region of the XZ plane at Y=0. Magnetic field lines displayed are open and attached to the Northern Hemisphere ionosphere. Thebackgrounds in (a) and (b) are the log of B and magnetic pressure, respectively. (c) The plane is colored with the mass density. (d) Velocitymagnitude provides the background. The depletion layer signatures are highlighted by the arrows, and their location relative to the open-IMFboundary is provided by the traced magnetic field lines.

flux pileup and the decrease in density are clear signatures of poleward of the cusp and are caused by the shoulder. Froma low-shear depletion caused by the shoulder, symmetry with no dipole tilt, a similar depletion layer devel-

ops poleward of the Southern Hemisphere cusp.

If the system is driven even harder, shoulders can develop

in both hemispheres with no dipole tilt and a purely south- The major magnetic storm on 31 March 2001 allowed anward IMF Bz. Figure 8 displays such a case with a driv- empirical test for the existence of shoulder-depletion layers.ing field of -50 nT (simulation 5 of Table 1). This run is Figure 9 provides data for 05:00 to 08:00 UT in the same for-north-south symmetric and only the Northern Hemisphere is mat as Fig. 1. The IMF has a magnitude of 45 nT throughoutshown. Figures 8a and b show the magnetic field and mag- this period with a clock angle near 160'. At this time, thenetic pressure overlaid with traced magnetic field lines. Blue dipole tilted back toward the nightside in the Northern Hemi-colored magnetic field lines are open with one foot in the sphere, emphasizing the shoulder in the vicinity of Polar atnorthern ionosphere. Only the first IMF (green) field line is southern high latitudes. Note, this is a Southern Hemisphereshown, which with the last blue trace defines the outer sep- pass in which Polar transitioned from the mantle into the higharatrix, as indicated by an arrow in each plot. Note the in- altitude cusp and then to the magnetosheath. As evidencedcrease in magnetic field and in magnetic pressure around the by the continuously negative Bz in Fig. 9a, Polar enteredseparatrix. Figures 8c and d show the density and velocity the magnetosheath poleward of the cusp at 06:20 UT, with-magnitude overlaid with the traced magnetic field lines. De- out crossing the shrunken dayside magnetosphere (cf. Figs. 7creased plasma density and velocity are associated with in- and 8). At Polar's prenoon location the magnetic latitude wascreased magnetic field magnitude. All of these features occur only -26', consistent with the predicted compressed dayside


IMF45 nT- clock

3/31/01: 0630 UT: Shoulder depletion layer angle near 160

400 4_4Mantle Cusp Magnetosheath BZ.GsM-200:••u•.. BZ'G~SM" --- --.--- -- - - - - - - -a

-400 /B.osM

. 200 A N - Polar150 bIO5 Shocked N - Ace

40- Depletion 1I1I - Polar300100 / C Shocked 1B1 - Ace

103. A 10 ...

10, •' • M 0d 106102 . .- 105107

o iiiiii 100102.e 105

05:00 05:30 06:00 06:30 07:00 07:30 08:00 time (UIT)31Maor2001 date

-73.03 --69.88 -- 68.77 --68.46 -68.50 -68.70 -768.99 ILT1053 1108 1115 1120 1124 1128 1131 MLT3.65 4.51 5.27 5.94 6.54 7.06 7.53 R11.7 8.4 7.6 7.4 7.4 7.6 7.8 L

-56.2 -43.2 -33.9 -26.6 -20.5 -15.1 -10.2 MAGLAT

Polar prenoon at -270 MLATand 1120 MLT - never enters dayside magnetosphere

Fig. 9. Polar data from 31 March 2001, showing a shoulder depletion layer located below the Southern Hemisphere cusp in the same

format as Fig. 1. Because of the strong driving conditions Polar crossed from the mantle into the magnetosheath, not contacting the daysidemagnetosphere. In this case the dipole is tilted away from the Sun.

magnetosphere and equatorward retreat of the cusps. The intensity of magnetosheath ions increased even more. The

magnetopause contracted to inside of geosynchronous orbit magnetopause boundary moved farther away from the satel-(Ober et al., 2002). Intense parallel ion fluxes (Fig. 9d) at lite at that time. Later, as the solar wind density observed bythis time are products of dayside merging causing plasma to ACE decreased and the magnetopause apparently expandedstream along the outer separatrix. Ions accelerated parallel to closer to Polar, ion fluxes measured after 07:15 UT again de-the magnetic field (away from the equator) and similarly di- creased in energy and intensity.rected parallel Poynting flux from Alfv~n waves indicate thelocation of an outer separatrix connected to a merging site at Later in the day, between 15:00 and 17:00 UT, while geo-lower latitudes (see black bars in Fig. 9d). The magnitude magnetic activity was still strong, Polar re-entered the mag-

of B in the magnetosheath at this location above the cusp in- netosphere poleward of the Northern Hemisphere cusp. The

creased on the magnetosheath side of the separatrix. Accel- IMF was 30 nT with a clock angle near 180'. At this time theerated 0+ ions were detected by the TIMAS instrument on Earth's dipole tilted sunward, emphasizing the formation ofPolar within the cusp and at the separatrix (not shown). The a Northern Hemisphere shoulder. Figure 10 presents Polarcutoff in 0+ ion fluxes confirms Polar's transition into the data in the same format as above. The change from posi-magnetosheath. Low density and lower energy perpendicular tive to negative Bz near 14:30 UT occurred in the magne-fluxes are measured between 06:20 and 06:40 UT. The den- tosheath and reflects a change in the imposed IMF direction.sity is comparable to the lagged ACE density. All of these At 16:00 UT the satellite was near magnetic noon and 470features indicate the presence of a depletion layer. As the magnetic latitude. The negative direction of Bz is consistentlagged ACE density increased near 07:00 UT, the energy and with the direction of the IMF and of open field lines above the

Northern Hemisphere cusp. Accelerated antiparallel fluxes


IMF 30 nT - clock

3/31/01: 1600 UT: Shoulder depletion layer angle near 180

1• - -- Magnetosheath0.~-' . a B1s

-50 B-S

10oN -Polar, IMF change bU40 V Shocked N - Ace

IB113 - PolarS• elt Shocked 1BI - Ace

10.3. d•i•- > .10 6

10 4 -7107

" 100

P-10o2" 105

l104 -11 10 7O3 g 0 O6

102 f 10510 0~ 2:;0

14:00 14:30 15:00 15:30 16:00 16:30 17:00 time (UT)31 Mor2001 ' dote

74.52 75.06 75.61 76.16 76.72 77,30 77,91 ILT1206 1207 1208 1208 1208 1207 1205 MLT9.40 9.29 9.14 8.94 8.70 8-42 8.08 R14.0 15.0 162 17.5 19.0 20.7 22.8 L34.8 38.0 41.1 44.2 47.2 50.3 53.3 MAGLAT

Polar postnoon at 470 MLAT and 1208 MLT Mantle ion dispersion

Fig. 10. Polar data from 31 March 2001, inbound above the Northern Hemisphere cusp showing a shoulder depletion layer. The format isthe same as in Fig. 1. In this case (later in the day from the data shown in Fig. 9) the dipole was tilted toward the Sun, as Polar crossed fromthe magnetosheath to the mantle.

of ions and Poynting flux were observed, indicating a cross- 7 Depletion layer structureing of the outer separatrix. Subsequently, the plasma densityand magnetic fields were changing, allowing for motion of Southwood and Kivelson (1995) suggested that density en-the magnetopause. Two other outer separatrix crossings are hancements and depletion layers in front of the magne-identified in Fig. 10. At each separatrix crossing the mag- topause were complementary parts of a standing slow mode

netic field was larger on the magnetosheath side. Through- structure. Two of the depletion layer observations discussedout the period when Polar was near the IMF-open boundary, above allowed us to test this hypothesis with both northwardthe plasma density was low and comparable to the lagged and southward IMF components.solar wind density, supporting our interpretation that Polar To make quantitative comparisons with this slow modeobserved a shoulder depletion layer. Near 16:45 UT the ion concept of depletion layers and its surroundings, we havefluxes became more characteristic of the mantle. The in- tested whether the observed density and magnetic field fluc-crease in the ACE density starting at that time recompressed tuations are consistent with the proposed type disturbances.the magnetosphere, returning the separatrix to the location of Scudder et al. (2003) developed a test for slow-mode char-Polar at 16:53 UT. acteristics of the observed time domain structures, observed

using Galilean-invariant quantities. Specifically, the disper-sion relation for slow mode waves predicts that Fourier am-.

These two examples provide evidence for the existence of plitudes of the density, Sp and magnetic field variations 3by

shoulders and shoulder depletion layers. In each case the should be linearly anti-correlated:density was low in the vicinity of the IMF-open field lineboundary as predicted by the simulations. bn/nols = -ctsinOBkbyl/Bo. (1)


X 09:30-09:35 Y 09:35-09:39 Z 09:45-09:55

m=-2.58+/-0.42 m=-4.27+/--0.7 =-4.53+/--0.7

3/31/2001 3/31/2001 3/31/2001

0. " 2136 . X2= 1.9500 •-<OOX2=0.3731

0, -0.5 -0.5

0=82.7 0=73.0 0=55.4

lB(nT)l=118.8-19 .7 lB(nT)l=110.4-1 7.1 IH(nT)l=130.0- 90.8

B.(nT)=163.9 B.(nT)=157.7 B.(nT)=177.0

N,(/cc)=141.14 N,(/cc)= 115.87 N,(/cc)=73.96

-10-1.0 j- -1.0-1.0 -0.5 0.0 0.5 1.0 -1.0 -0.5 0.0 0.5 1.0 -1.0 -0.5 0.0 0.5 1.0

Fig. 11. Linear regression fits for three intervals of 31 March 2001, labeled X, Y, and Z in Fig. 1. Normalized changes in density are plottedas functions of normalized changes in the maximum variance component ofrB. Bo and No represent values of B and N at the nominal fitzero of the plane wave and are constrained to be within the interval. The actual zero may lie outside the interval. The function Sig(x), - 1for X<0 and + 1 for X>0, is used to rectify the sign of 3 B so that negative values of the resulting slope represent slow-mode solutions.Sig(0)=0. The reported slope m (related to ca in Eqs. (1) and (2)) is M/sin(G)bk), where M represents actual slopes obtained from the plottedlines. See Scudder et al. (2003) for more details.

Here, a>0, OBK is the propagation angle and Bo is the mag- is positive for all fi and directions of wave propagation. Tonetic field intensity for the interval, n, and P. are plasma test for the slow mode signatures we compare data on thevariables occurring when the mean magnetic field is actually right- and left-hand sides of Eq. (1) to a linear model with-observed. out intercept in a coordinate system determined by minimum

The usual MHD description of the slow mode as- variance analysis on B, as discussed by Scudder et al. (2003).sumes polytropic closure to determine a sound speed, C1 , The ordinate of the fit iswhich is the proportionality constant in the relationship be-tween density and pressure fluctuations: SP=CSn. Also, cSn(t) =- n(t) - n. (3)C2=yPo/no, where P, and n, are the spatially uniform ref-s while the abscissa is determined byerence pressure and density. The dimensionless proportion-ality constant in Eq. (1) is determined from linear theory to 8by(t) = B(t) - By, -. (4)be

v A correct inference of Sby is contingent on having correctlyca = V2 (2) identified k, Bo, 0. We optimize the intercept-free linear re-

(C2 - U2) gression between 8n/no and sin(OBk)Sby/Bo. If after con-where U is the phase velocity of the wave in the plasma rest sideration of the errors, the regression is acceptably ranked,frame. For the slow-mode branch, the denominator of Eq. (2) the best-fit slope <ca>wave is compared with the theoretical


prediction of Eq. (1) evaluated at the optimal (Bo, 0Bk). The measure of the source's generation of pure slow-mode wavesregression slope, together with P, implies a correlative choice in a nondispersive regime. There is no need for a wave packetfor y (<a>). Plasma data can also be analyzed separately to be monochromatic as long as its constituent wave numbersdetermine the underlying value of for Yplasma independent of lie within the same nondispersive branch. The duration thatthe wave fitting described above. Our final consistency check Polar remained within features suggests that a slow-modeis to show that <0t>wave -- <U >plasma. The more extensive wave is standing in front of the magnetopause, as proposedanalysis of Scudder et al. (2003) also allows for wave pack- by Southwood and Kivelson (1995).ets in two orthogonal directions to the principal propagation Figure 12 show data from the three intervals labeled X,defined by the minimum variance analysis. These additional Y, and Z in Fig. 5. While Fig. 11 illustrates a standard de-waves, which may be slow or fast mode waves, are necessary pletion with northward IMF, the case shown in Fig. 12 oc-to fully reconstruct the density variation versus time profile. curred during a relatively high shear event with southwardSince they are not necessary for this study, we have omitted IMF. Panel (X) confirms the presence of the slow mode wavethem here. in the interval before 08:00 UT, previously identified as a

Figure 11 illustrates results of the procedure performed depletion. Panels (Y) and (Z) show slow-mode behavior onduring the three intervals of 31 March 2001, indicated by X, both sides of the large change in density imposed from theY, and Z in Fig. 1. The data and optimal linear fits are given, solar wind near 10:23 UT. The actual period of the rapidas well as the slope-fit parameters, uncertainties, normalized change was omitted. In this case the density peaks above ad-

X2, and optimized values of Bo, n, and 0, and their uncer- justed ACE values. The increased parallel and anti-paralleltainties (note that this fit procedure selects for B, a value fluxes suggest that. the spacecraft stayed on the outside ofthat lies within the fit interval). High quality linear fits with the slow-mode enhancement after 10:23 UT. In the subse-negative slopes characteristic of slow mode waves are found quent interval the fits (not shown) varied in slope and X2 in-by this technique, with similar values of B,. The densities creased. It is conceivable that at a given time Polar coulddecrease with time, as do the adjusted ACE data. The pop- simultaneously witness compressive wave power from mul-ulation near the regression lines also provides information tiple sources, thus destroying correlations recorded at succes-about the relative importance during each interval of plasma sive times by Polar. In the 16 April case the second depletioncompression or rarefaction. If both behaviors occur in an in- formed while the IMF rotated from negative to positive By.terval, data points span a range in Sn that straddles zero in The density increased when a strong density enhancement,a significant way. Conversely, in intervals principally char- seen by the ACE, encountered the magnetopause. The in-acterized as compressions (rarefactions) data points cluster creased dynamic pressure caused the magnetopause to movealong the fit line primarily in the second (fourth) quadrant inward, allowing Polar to move from the depleted to the en-of the diagram. Our determinations of 8n(t) really represent hanced density part of the standing wave. Unlike the 31our measure of Sneikz(t) as the wave train is carried past our March event, there was no imposed density decrease allow-viewing position. Data points do not represent simple Fourier ing the magnetopause to push back toward the spacecraft.amplitudes of some mode, but spatially modulated functions, Thus, Polar observed the outer compressive portion of thethat cause our estimates to be distributed along a line rather slow mode wave.than cluster about a point on the line appropriate for the ra- Finally, we note that we found evidence (not shown) fortio of pure Fourier amplitudes. Our diagnostic is immune slow-mode waves in the other illustrated depletion layers.to the vagaries of relative motion, fitting quantities that areGalilean invariant: the relative opposed phase of the densityand magnetic field strength. 8 Discussion

The regression analysis provides strong support for theslow mode playing a significant role in density/field varia- In the previous sections we presented empirical and simu-tions observed in all three regions. To reduce ambiguities in- lation evidence for the existence of two types of depletionherent in the variable densities observed by ACE, our first in- layers forming near the magnetopause when the IMF hasterval for analysis commenced at 09:30 UT. Negative slopes a southward component. In both cases Polar observationscharacteristic of slow-mode structures are evident on both support the predictions of ISM simulation. While these de-sides of the density peak. In interval Z the slow mode slope pletion layers occur under relatively unusual circumstances,was similar to that of interval Y, with a large percentage their presence in ISM simulations provides clues as to whenof the points located below the plot's centerline. Compar- and where they may exist. In the following we further ex-ing Fig. 11 with Fig. lb, we conclude that when the density plore the implications of these findings.peak was reached (probably in the compressive phase of thewave), relative motion between the spacecraft and boundary 8.1 Velocity-separator depletion layersmoved Polar back into the region of stronger depletion. Thisinterpretation is consistent with variations in Polar and ACE Maynard et al. (2003) provided evidence for a depletionB and density data shown in Fig. 1. As the magnetopause layer developing while the IMF clock angle was about 140'.breathed outward Polar moved back into the principal deple- This paper confirms that interpretation by showing a regiontion region. That the data points fit straight lines so well is a of depleted density relative to ACE measurements near the


X 07:45-07:53 Y 10:10-10:15 Z 10:23-10:281.1.0 I I I I 1.0 i I I I I��.0

m=-2.93+/-0.44 M=-0.91 +/-0.18 m=-1.02+/-0.07

4/18/2000 4/16/2000 4/16/2000

0.5. 0.5 0.5

"0.0• X2 =1.0727 O'. - X2 =1.6334 X2=8.71

-0.5 -0.5- -0.5

0=69.9 0=96.1 0=100.9

1B(nT)l=44.3-74. JB(nT)J=48.9-72.9 JD(nT)l=38.2-74.3

Bo(nT)=59.0 B.(nT)=63.3 B(nT)=56.8

N°(/cc)=33.31 N.(/cc)=52.84 N.(/cc)=105.97

-1.0 -0.5 0.0 0.5 1.0 -1.0 -0.5 0.0 0.5 1.0 -1.0 -0.5 0.0 0.5 1.06B Sig(B). ) B Y Sig(B,.)/B. 6 B Sig(Bl)/Bi

Fig. 12. Linear regression fits for three intervals of 16 April 2000, labeled X, Y, and Z in Fig. 5. See caption for Fig. 11.

location of velocity separator. ISM reveals that the deple- 8.2 Shoulder depletion layerstion develops best in the presence of a significant BX and/ordipole tilt. Crooker et al. (1992) showed that the effects of We have developed evidence for the existence of shoulder de-

Bx and dipole tilt are similar and may either add or subtract, pletion layers in the Polar data and ISM simulations. Two ef-

depending on polarity. Figure 19 of Maynard et al. (2003) fects occur: the dayside cusp at the magnetopause is pinched

showed that as the dipole tilt increases, the merging site toward the equator and a shoulder develops above the cusp.

moves to higher latitudes away from the tilt. This length- Both effects can be explained as fringe-field effects from Re-

ens the time for draping of the IMF field lines around the gion 1 currents closing through the high-latitude ionosphere

magnetopause to the high-latitude site. We suggest that pro- over the polar cap. Siscoe et al. (1991, 2002c) show that as-

longed draping times allow magnetic flux to pile up and con- sociated current loops pass through the magnetopause above

sequent depletion layers to form. Component merging at low the cusp, which augment/modify the Chapman-Ferraro cur-

latitudes is inconsistent with this flux pileup. The presence rents in that region. These currents form a loop where the

of the depletion layer supports our interpretation of'observa- field internal to the loop has strong +X and -Z compo-

tions presented in Maynard et al. (2003), that magnetic merg- nents, which adds to the magnetic field above the cusp and

ing was proceeding at high latitudes poleward of the space- subtracts below the cusp. This perturbation magnetic field

craft. In any situation in which the merging site is remote contributes to shoulder development. Similarly, it depresses

and additional draping time is involved to reach that merging the magnetic field in the sub-solar region. The magnetic field

site, we may expect depletion to occur. at the nose drops below the dipole field for IEF values of4mVm- 1.

a


Sunward dipole tilts push the shoulder region forward. We have furnished observational evidence in support of theThis increases the time required for the IMF to drape to the Southwood and Kivelson (1995) hypothesis that density de-merging site and allows density depletions to deepen. Even pletions (Zwan and Wolf, 1976) and enhancements (Song etat equinox the dipole tilt varies +120 every day, and the tilt is al., 1990; 1992) are parts of a slow mode wave standing instrongest at solstice. IMF Bx causes complementary varia- front of the magnetopause. The existence of depletion layerstions (Crooker et al., 1992). The IEF phase plane is generally in front of a dayside, high-shear magnetopause with south-tilted, with large Bx increasing the tilt in the XZ plane, so ward IMF components requires that any merging must be re-that the phase plane tilt may add or subtract from the dipole mote from the observation. Their presence in the sub-solartilt to provide an effective tilt that in some cases is much region favors high latitude merging and rules out sub-solargreater. The IEF phase plane orientation varies on time scales component merging, if merging occurs on that field line.of 10 s of min (Weimer et al., 2002). Thus, the depths of de-pletions may be dynamic quantities, depending on the values Acknowledgements. We thank F. S. Mozer, C. T. Russell, and W.of all three IMF components and the dipole tilt. K. Peterson for Polar electric field, magnetic field, and ion com-

position data, and C. W. Smith and D. J. McComas for ACE mag-

8.3 Slow mode structure of depletion layers netic field and plasma data. We especially thank M. Kivelson forhelpful discussions. This work was supported in part by AFOSR

sfor evidence of slow Task 2311SDA3, NASA grants NAG5-8135 (Sun-Earth Connec-Wode haves exam ding ie P rontofthnlar mtions Theory Program grant) and NASW-99014, and by the NASAmode waves standing in front of the depletion layer as postu- Polar mission through subcontracts with the University of Califor-lated by Southwood and Kivelson (1995). In fact, evidence nia at Berkeley. The work at Iowa is supported by NASW5-7883for a density enhancement and low B appears near 12:30 UT by the Polar Project office at NASA. The ISM was developed underin Fig. 2. However, it was shown in Maynard et al. (2003) sponsorship of the Defense Threat Reduction Agency, 45045 Avia-that this slow-mode-like feature reflected similar variations tion Drive, Dulles, VA 20166-7517.in the solar wind and was not unique to the formation of a de- Topical Editor T. Pulkkinen thanks a referee for his help in eval-pletion layer. Figure 2c shows that magnetic fields observed uating this paper.

at Polar track shocked values of ACE measurements quitewell, confirming that the structure was imposed by the so-lar wind. Because of the skimming nature of its orbit, Polar Referencesdid not fully penetrate to magnetosheath features standing infront of the magnetopause, unless there were variations in Anderson, B. J. and Fusilier, S. A.: Magnetic pulsations from 0.1 tofrontofthe drier.ariations unldyamipessutere c ge vathponsin 4.0 Hz and associated plasma properties in the Earth's subsolarthe drivers. Variations in dynamic pressure change the posi- magnetosheath and plasma depletion layer, J. Geophys. Res., 98,tion of the magnetopause and the relative position of Polar 1461,1993.

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Just as the nose of the magnetopause presents an obsta- Crooker, N. U., Eastman, T. E., and Stiles, G. S.: Observations

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4L


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R O D U T O P EForm ApprovedREPORT DOCUMENTATION PAGE OMB No. 0704-0188

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5c. PROGRAM ELEMENT NUMBER61102F

6. AUTHOR(S) 5d. PROJECT NUMBERN.C. Maynard*, W.J. Burke, J.D. Scudder**, D.M. Ober*, 2311G.L. Siscoe***, W.W. White*, K.D. Siebert*, D.R. Weimer*, Se. TASKNUMBERG.M. Erickson***, J.Schoendorf* and M.A. Heinemann SD

5f. WORK UNIT NUMBERA3

7. PERFORMING ORGANIZATION NAME(S) AND ADDRESS(ES) 8. PERFORMING ORGANIZATION REPORTAir Force Research Laboratory/VSBXP NUMBER29 Randolph RoadHanscom AFB MA 01731-3010

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*ATK Mission Res, Nashua, NH; **Dept of Phys & Astronomy, Univ of Iowa, Iowa City, Iowa;***Center for Space Physics, Boston Univ, Boston, MA

13. SUPPLEMENTARY NOTESREPRINTED FROM: ANNALES GEOPHYSICAE, Vol 22, pp 2151-2169, 2004.

14. ABSTRACTAbstract. We present observations from the Polar satel-lite that confirm the existence of two types of depletion lay-ers predicted under southward interplanetary magnetic field(IMF) conditions in magnetohydrodynamic simulations. Thefirst depletion type occurs along the stagnation line whenIMF Bx and/or dipole tilt are/is present. Magnetic merg-ing occurred away from the equator (Maynard et al., 2003)and flux pile-ups developed While the field lines drape to thehigh-latitude merging sites. This high-shear type of deple-tion is consistent with the depletion layer model suggestedby Zwan and Wolf (1976) for low-shear northward IMF con-ditions

15. SUBJECT TERMSMagnetospheric physics Magnetopause Cusp and boundary layersMagnetosheath Magnetospheric configuration and dynamics16. SECURITY CLASSIFICATION OF: 17. LIMITATION 18. NUMBER 19a. NAME OF RESPONSIBLE PERSON

OF ABSTRACT OF PAGES W. Burkea. REPORT c. THIS PAGE SAR 19b. TELEPHONE NUMBER (include areaUNCLAS UNCLAS UNCLAS code)

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observed and simulated depletion layers with southward imf · and boundary layers; magnetosheath;...

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