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Interactions of meteoroids with the
Earth's atmosphere
Maria Gritsevich(1) Department of Remote Sensing and Photogrammetry, Finnish Geodetic Institute,
(2) Division of Geophysics and Astronomy, Department of Physics, University of Helsinki,
(3) Institute of Mechanics, Faculty of Mechanics & Mathematics, Lomonosov Moscow State University
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“A space rock a few metres across exploded inEarth’s atmosphere above the city of Chelyabinsk,Russia today at about 03:15 GMT. The numerousinjuries and significant damage remind us that whathappens in space can affect us all…”
Sourse: www.esa.int (News, 15 February 2013)
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Outline
Introduction
A new method implemented for parameters’ identification
Result testing
General statistics and consequences
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Basic definitions
A meteoroid is a solid object moving in interplanetary space, of asize considerably smaller than an asteroid and larger than an atom
A meteor is event produced by a meteoroid entering atmosphere.On Earth most meteors are visible in altitude range 70 to 100 km
A fireball (or bolide) is essentially bright meteor with largerintensity
A meteorite is a part of a meteoroid or asteroid that survives itspassage through the atmosphere and impact the ground
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Past terrestrial impacts
The largest verified impact crater on Earth (Vredefort)
~300 km
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Past terrestrial impacts
Different types of impact events, examples: formation of a massive single crater(Vredefort, Barringer)
~300 km
~1,2 km
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Past terrestrial impacts
Different types of impact events, examples: formation of a massive single crater(Vredefort, Barringer, Lonar Lake)
~300 km
~1,2 km
~1,8 km
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Past terrestrial impacts
Dispersion of craters and meteorites over a large area (Sikhote-Alin)
~1,2 km
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Past terrestrial impacts
Tunguska
~1,2 km
~1,8 km
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Tunguska after 100 years…
Area over 2000 km2
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Impacts as a hazard
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Another reason why we are interested
The three forms of extraterrestrial bodies. Meteorites (right) are remnants of theextraterrestrial bodies (asteroids, comets, and their dusty trails, left) entering Earth’satmosphere and forming an event called a meteor or fireball (middle). The darkfusion crust on the meteorite is a result of ablation during atmospheric entry.
…or:
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What can we do in the lab?Nondestructive physical properties, includingmeasurements of extraterrestrial materials:
BRF measurements
Bulk and grain density (i.e. also porosity)
Magnetic susceptibility
Internal structure (x-ray microtomography)
Development of methods for nondestructive thermal and mechanical properties measurements
Some of the parameters can be determined at wide temperature range (5-1080 K)
Our combined database contains thousands ofindividual meteorites. Results are publishedand/or shared within the scientific community
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Example of recent results (1/2)
The FIGIFIGO measuring BRF of selected sample Gibeon (left). The active optics systemis located horizontally at the top of the measuring arm, and is looking down to the targetthrough a mirror. FIGIFIGO consists of the following main components: casing,measurement arm, rugged computer, and a sunphotometer on a tripod. The casingcontains the main sensor ASD FieldSpec Pro FR optical fiber spectroradiometer (350 –2500 nm), most of the electronics, and batteries.
Example of measured albedo: Bruderheim L6 meteorite
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Example of recent results (2/2)
1003 1006
1004
1009
603
607
1005
1011
1007
1008
1010
1012
1001
99
33
S12
9
87
82
S127
S195
A
S16
4
S19
5
S138
41 S194
14
16
25
3.5
4
4.5
5
5.5
6
Log
(10-9
m3 /k
g)
Ure
ilites
LL
L
H
E
Increasing meteorite mass Increasing meteorite mass
300 m
Porosity
Metal rich rim
Magnetic susceptibility was used as atool to identify of non-ureilitic meteorites withinAlmahata Sitta (2008 TC3) meteorite collection
Porosity mappingusing XMT
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Classical double-station programallow us to calculate:
meteor height length along trajectorymeteor intensityspectrum
first attempts:Harvard Meteor ProjectOndrejov Observatory in Czechoslovakia
first success:bright fireball photographed on April 7, 1959: four meteorites were found near P íbram in Czechoslovakia in the area predicted from the double-station photographic data (Ceplecha, 1961)
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g g gg
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The largest piece (Luhy, 4.5 kg)
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The largest programs
European Fireball Network
Prairie (Meteorite)
Network
Meteorite Observation &
Recovery Project
Operational time Since 1963 1963-1975 1971-1985
Number of Stations ~ 50 16 12
Station Spacing, km ~ 90 250 193
Cameras per Station 1 4 5
Availability of obtained data partly published published published
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Immediate objectivesmore reliable and rapid meteorite recovery from the Earth’s surface
understanding of meteorite origins, physical properties and chemical composition
meteor orbital characteristics and their association with parent objects
possible identification of when and where a meteor can enter the Earth’s atmosphere and potentially become a meteorite
understanding of how to predict the consequences based on event observational data
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Registered meteorite fallsMeteorite name country year mass found type
íbram Czechoslovakia 1959 5.8 H5 Lost City USA 1970 17.2 H5 Innisfree Canada 1977 4.58 L5 Peekskill USA 1992 12.57 H6
Tagish Lake Canada 2000 ~ 10 CI Morávka Czech Republic 2000 1.4 H5
Neuschwanstein Germany/Austria 2002 6.2 EL6 Park Forest USA 2003 18 L5
Villalbeto de la Peña Spain 2004 5 L6 Bunburra Rockhole Australia 2007 0.34 eucrite
Buzzard Coulee Canada 2008 ~ 41 H4 Almahata Sitta Sudan 2008 ~ 4 ureilite
Grimsby Canada 2009 0.22 H5 Jesenice Slovenia 2009 3.67 L6 Košice Slovakia 2010 3.92 H5
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Introduction
A new method implemented for parameters’ identification
Result testing
General statistics and consequences
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Groundbased observations
The information on meteor body entry into the atmosphere contains detaileddynamic and photometric observational data. The important input parametersare: the fireball brightness I (t), its height h (t) and its velocity V (t)
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’Reentry’ concept
íbram meteorite
Entry starts with a rarefied hypersonic flow (usually defined as those with aKnudsen number above 0.1), do not follow the Navier-Stokes equations
The introduction of non-equilibrium real gas effects becomes important
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Interpretation of Earth observations
21 ,2 d a
dVM c V Sdt
sin ,dh Vdt
31*2 h a
dMH c V Sdt
DynamicalPhotometric
dtdEI
0dVdt
0
1
2
t
t
IM dtV
Usually simplified case used is:
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A dynamical methods: special case
2/3
2/3bSA
M
33 2
2
( )2
d ad
b
c VV
21 ,2 d a
dVM c V Sdt
The main drawback is approximation of constant meteoroid shape, whichadopted in the majority of publications in Meteor Physics
The values of deceleration are obtained with the numerical differentiation
32
2306,0
VVa
d
32
2101,0
VVa
d
Halliday et al.
Wetherill, ReVelle
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More general approach
sin*21 22
00 svHV
MSh
cdydm e
e
eh
0 01 ;2 sin
ed
e
h Sdv vsm cdy M
m = M/Me; Me – pre-atmospheric mass
v = V/Ve; Ve – velocity at the entry into the atmosphere
y = h/h0; h0 – height of homogeneous atmosphere
s = S/Se; Se – middle section area at the entry into the atmosphere
0; 0 – gas density at sea level
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Two additional equations
variations in the meteoroid shape can be described as (Levin, 1956)
assumption of the isothermal atmosphere
=exp(-y)
)(ee M
MSS
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Analytical solutions of dynamical eqs.
y = , v = 1, m = 1
Initial conditions
where by definition:
11exp)(
2vvm
))()(ln(2ln)( 2viEiEvy
x z
zdzex)i(E
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The key dimensionless parameters used
characterizes the aerobraking efficiency, since it is proportional to the ratio of the mass of the atmospheric column along the trajectory, which has the cross section S , to the body’s mass
is proportional to the ratio of the fraction of the kinetic energy of the unit body’s mass to the effective destruction enthalpy
sHc
VcM
Shc m
d
eh
e
ed log,
21,
sin21 2
00
characterizes the possible role of the meteoroid rotation in the course of the flight
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Next step: determination of and t, sec h, km V, km/sec0,0 58,8 14,540,2 56,1 14,490,4 53,5 14,470,6 50,8 14,440,8 48,2 14,401,0 45,5 14,341,2 42,8 14,231,4 40,2 14,051,6 37,5 13,791,8 35,0 13,422,0 32,5 12,962,2 30,2 12,352,4 27,9 11,542,6 25,9 10,432,8 24,2 8,893,0 22,6 7,243,2 21,5 5,543,3 21,0 4,70
On the right:Data of observations of Innisfree fireball (Halliday et al., 1981)
Ei( )x ze dzx
z
The problem is solved by the least squares method
2ln)(vy
))()(ln( 2viEiE
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The desired parameters are determined by the following formulas:
the necessary condition for extremum:
2
1 1
2 ;i i
n ny y
ii i
e e
1 1 1
exp( 2 ) exp( ) exp( ) ( ( ) ) 0n n n
i i i i i i ii i i
y y y
2 2
1 12
1
((( ) ) ( 2 exp( ) (( ) 2( ) )1
exp( )( ( ) )
i
n n
i i i i i i ii i
n
i i ii
y
y
the sufficient condition:
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Final step: determination of From the current dynamical model the intensity of fireball luminosity can be rewritten as:
This can be compared with values I(v) calculated from the observed magnitude
dtdVMV
dtdMV
dtMVdI
2)2/( 22
dtdVvvVMvVM eeee 1
1exp1
23
1)1exp1
1))i(E-iE(
2sin 22
23
0
3 vvvvh
VM ee
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The dependence between light curve and shape change coefficient
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Introduction
A new method for parameters’ identification
Result testing
General statistics and consequences
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Result of calculations for well registered meteorite falls
fireball Ve, km/s sin 102 , s2/km2
íbram 20,887 0,68 8,34 13,64 6,25
Lost City 14,1485 0,61 11,11 1,16 1,16
Innisfree 14,54 0,93 8,25 1,70 1,61
Neuschwanstein 20,95 0,76 3,92 2,57 1,17
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Graphical comparison
5 10 15 2020
40
60
h
V
Innisfree
íbram
Lost City
Analytical solution with parameters found by the method (solid lines) is compared to observation results (dots)
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Meteoroid’s Deceleration
sine
o
dy V vdt h
))()(ln(2ln)( 2viEiEvy
)exp()i(E-iE
2sin
2
2
0
22
vv
hvV
dtdydvV
dtdV e
e
We can compare data in the planes (t, V) and (t, h)
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Coupling of parameters used in meteoroid entry modelling
Lost City: velocity of the main body
3
5
7
9
11
13
15
0 1 2 3 4 5 6 7 8 9 10
t, s
V, k
m/s
Comparison with paperCeplecha, ReVelle 2005
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This image cannot currently be displayed.
Lost City: height of the main body
0
10
20
30
40
50
60
70
80
90
100
0 1 2 3 4 5 6 7 8 9 10
t, s
h, k
m
Comparison with paperCeplecha, ReVelle 2005
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Lost City: deceleration of the main body
-5
-4
-3
-2
-1
0
0 1 2 3 4 5 6 7 8 9 10
t, s
dV/d
t, km
/s2
Comparison with paperCeplecha, ReVelle 2005
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Terminal mass prediction: comparison with found meteorites’ mass
fireball , g/cm3 Vt, km/s M(Vt ), kg Mt, kg
Lost City 3,73 3,4 43 17,2
Innisfree 3,5 4,7 27 4,58
Neuschwanstein3,49 2,3 28 6,2
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Neuschwanstein
Initial mass, kg
520 - 670 *
300 – 600 1
400 – 530 2
1Spurny et al.
2ReVelle et al., 2004
Our result corresponds to the estimates done based on the analysis of recorded acoustic, infrasound and seismic waves caused by the meteorite fall
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Initial masses for earlier meteorite falls
íbram Lost City Innisfree
M, kg 317 169 179
M1, kg 1300 52 18
Mph, kg 215002 4903 3184
M, kg 3205 655 ?
M6, kg – 165 42
M, kg 2507 2107 –
M5, kg 1700 38 25
1 (ReVelle, Rajan, 1979), 2 (Ceplecha, 1977; Oberst et al., 1998), 3 ( et al., 1978),4 (ReVelle, 1980), 5 (Wetherill, ReVelle, 1981), 6 (Ceplecha, ReVelle, 2005), 7 (Bagolia et al., 1980)
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Characteristic heights for the fireball trajectories
1 13 3 330,
30 4 3e
m
M LL R
hsw – the height below which the flow around the equivalent sphere of radius Rtakes place in the thin viscous shock layer regime (i.e. a thin shock is formed)
40 0 0 ln / , 0.19 10 lh h L l l
hl – the height at which the size L is equal to the mean free path of air molecules
hbl – the height corresponding to the formation of a thin boundary layer on theequivalent sphere
40.7 15 lgblh R
53 17.05lgswh R
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Calculated characteristic heightshb, km
hmI,km
ht, km
Me, kg
L, cm
hl, km
R, cm
hsw, km
hbl, km
18 75,5 44,9 27,5 11,5 4,8 89,0 9,2 69,4 55,2
169 78,9 44,2 34,0 6,1 3,9 87,5 7,5 67,9 53,8
195 77,4 40,6 30,4 3,3 3,2 86,1 6,1 66,4 52,5
204 61,9 40,6 29,5 187,9 12,1 95,7 23,4 76,3 61,2
205 72,5 38,0 28,9 0,6 1,8 81,9 3,4 62,1 48,7
219 67,7 33,5 26,1 33,5 6,8 91,6 13,2 72,1 57,5
223 78,5 49,0 27,1 141,7 11,1 95,0 21,3 75,6 60,6
276 81,8 32,4 24,4 8,2 4,3 88,2 8,3 68,6 54,4
285 58,8 35,0 19,8 104,1 10,0 94,3 19,2 74,9 60,0
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Introduction
A new method implemented for parameters’ identification
Result testing
General statistics and consequences
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Distribution of parameters and for MORP fireballs
Innisfree
-3
-2
-1
0
1
2
3
-1 0 1 2 3 4 5 6 7
ln
ln
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Looking for Meteorite ‘region’
-3
-2
-1
0
1
2
3
-1 0 1 2 3 4 5 6 7
ln
ln
min3ln ln m
1,min tt vMM
sin = 0.7 and 1; Mmin = 8 kgInnisfree
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Meteorite falls prediction (down to 50 g)
-3
-2
-1
0
1
2
3
-1 0 1 2 3 4 5 6 7
ln
ln
Halliday et al., 1996
sin = 0.7 and 1; Mmin = 8 kg and 0.05 kgInnisfree
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Some historical events
Event Original mass, t
Collected meteorites, kg
1 Canyon Diablo meteorite (Barringer Crater) > 106 > 30 103 0.1 0.1
2 Tunguska 0.2 106 - 0.3 30
3 Sikhote Alin 200 > 28 103 1.2 0.15
4 Neuschwanstein 0.5 6.2 3.9 2.5
5 Benešov 0.2 - 7.3 1.8
6 Innisfree 0.18 4.58 8.3 1.7
7 Lost City 0.17 17.2 11.1 1.2
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Same events on the plane (ln , ln )
(1)
( 2)
( 3 )
( 4)(5 )
(6)(7)
-3
-2
-1
0
1
2
3
-3 -2 -1 0 1 2
ln
ln
(1) Crater Barringer
(2) Tunguska
(3) Sikhote Alin
(4) Neuschwanstein
(5) Benešov
(6) Innisfree
(7) Lost City
~1,2 km
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Same events on the plane (ln , ln )
(1)
( 2)
( 3 )
( 4)(5 )
(6)(7)
-3
-2
-1
0
1
2
3
-3 -2 -1 0 1 2
ln
ln
(1) Crater Barringer
(2) Tunguska
(3) Sikhote Alin
(4) Neuschwanstein
(5) Benešov
(6) Innisfree
(7) Lost City
~1,2 km
0 < < 1, 0 < < 1
>1, > 10 < < 1, > 1
> 1, 0 < < 1
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Meteorites /craters prediction
(1)
( 2)
( 3 )
( 4)(5 )
(6)(7)
-3
-2
-1
0
1
2
3
-3 -2 -1 0 1 2
ln
ln
(1) Crater Barringer
(2) Tunguska
(3) Sikhote Alin
(4) Neuschwanstein
(5) Benešov
(6) Innisfree
(7) Lost City
~1,2 km
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ConclusionsConsideration of non-dimensional parameters andallow us to predict consequences of the meteor impact.These parameters effectively characterize the ability ofentering body to survive an atmospheric entry and reachthe ground. The set of these parameters can be also used tosolve inverse problems, when we have to evaluateproperties of the entering body based on observations.
The results are applicable to study the properties of near-Earth space and can be used to predict and quantify fallenmeteorites, and thus to speed up recovery of theirfragments.
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Some relevant papersGritsevich, M.I., Stulov, V.P., and Turchak, L.I. (2012): Consequences for Collisions of Natural Cosmic Bodies with the Earth Atmosphere and Surface // Cosmic Research, 50(1), 56–64
Gritsevich, M., and Koschny, D. (2011): Constraining the luminous efficiency of meteors // Icarus, 212(2), 877-884.
Gritsevich, M.I. (2009): Determination of Parameters of Meteor Bodies Based on Flight Observational Data // Advances in Space Research, 44(3), 323-334.
Gritsevich, M.I. (2008): The Pribram, Lost City, Innisfree, and Neuschwanstein Falls: An analysis of the Atmospheric Trajectories // Solar System Research, 42(5), 372-390.
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Thank you very much!
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Why do we pass from y to exp(-y) ?
x z
zdzexve )i(E,)i(E-iE,
22
0 0.2 0.4 0.6 0.8 1
4
6
8
y
v 0 0.2 0.4 0.6 0.8 1
0.01
0.02
0.03
0.04
e y
v
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Newton's Second Law of Motion
21 sin2 d a
dVM c V S Mgdt
212 d a
dVM c V Sdt
limt o
dMV MVdt t
( )( ) ( )MV M M V V M V U MV
lim limt o t o
dMV MV M V MU dVMdt t t dt
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Mass computation3
3/200
sin21
m
ede
AhcM
Initial Mass depends on ballistic coefficient
320 0
2/3
1( ) exp (1 )2 sin 1
ed
m
h AM v c v
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Forms of some recovered meteorites
íbram Innisfree
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3
0 02 3
1 12 sine d
m
h AM c
Ae=Se/We2/3
0,
h0,
Ae
cd, m,
sin21 00
e
ed M
Shc
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1. :
22 exp exp( ) 0, Ei - Ei( )y v
2. 2.
( , , , ) 2 exp exp( )i i i iF y v y
3.
24
1( , ) ( ( , , , )) min
n
i ii
Q F y v