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A subalfvenic plasma flow past the magnetized obstacle: Ganymede
magnetosphereScobeltsyn Institute of Nuclear Physics, Lomonosov
Moscow State University, Leninskie Gory, 119992, Moscow, Russia
[email protected] I. Alexeev and Elena S. Belenkaya
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Content Jupiter magnetosphere global structure and magnetic
field at Ganymedes orbit
Ganymede aurora spot at Jupiter and aurora at Ganymede
Ganymede orbit placed near to (1) Jupiter magnetosphere Alfenic
radius, (2) inner edge of the Jovian current disk, (3) equatorial
projection of the main oval
Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*
Space Research Institute, 7 March 2013, 12:00 12:20
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*2013 February 15Astronomy Picture of the
DayShadows Across Jupiter Image Credit &Copyright:Damian
Peach
Space Research Institute, 7 March 2013, 12:00 12:20
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Paraboloid model full sizeNear Ganymede
magnetosphere Alexeev, Belenkaya, AG, [2005]
Space Research Institute, 7 March 2013, 12:00 12:20
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Paraboloid model of the Jovian
magnetosphereModel components In a Jovian solar-magnetospheric
coordinate system: Bm(t) = Bd() - planetary field vector+
BMD(,BDc,RD1,RD2) - field from equatorial current disc + Bsd (,R1)
- from currents shielding planetary field+ BMD(,BDc, R1,RD1,RD2) -
field from currents shielding current disc field+ BTS(,,R2,Bt) -
from cross-tail + closure magnetopause currents + b(kJ,BIMF) -
fraction of the IMF penetrating the magnetosphere
Time-dependent model parameters
magnetic dipole tilt angleR1 subsolar MP distanceRD2 and RD1
radial distances of the inner and outer edges of the current discR2
radial distance of the inner edge of the tail current sheetBt/(1+2
R2/ R1)1/2 tail field strength at the inner edge of the tail
current sheetBDC current disc field strength at the outer edge of
the current discBIMF IMF vectorkJ coefficient of the IMF
penetrationAlexeev, Belenkaya, AG[2005]
Space Research Institute, 7 March 2013, 12:00 12:20
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*The transition from dipole like to
stretched tail-like field lines in Jupiter magnetosphere.
R1RD1RD2RD1R2 =0 Bt=3 nT BDC=3 nT
R1 =92.8 RJR2 =85.4 RJRD1 =84.4 RJRD2 =16.4 RJ
Space Research Institute, 7 March 2013, 12:00 12:20
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*The transition from dipole like to
stretched tail-like field lines. Nearest Earth tail edge (e.g. Lui
et al., 1992). The carton is based on data by AMPTE CCE Magnetic
Field Experiment
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Ulysses the jovian magnetospheric magnetic
fieldMeasured by Ulysses the magnetic field dependent on the radial
distance r (Cowley et al., 1996) is marked by solid curve. For
comparison there are also shown magnetic field strength calculated
by present model (heavy curve).
Alexeev and Belenkaya, AG, [2005] Equatorial current disk
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Relative intensity versus pitch angle
versus time and position for 15- to 29-keV electron data as
generated and reported by Tomas et al. [2004a, 2004b] using data
from the Galileo EPD instrument
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Energetic ion spectra and plasma beta=1 at Ganymede
orbitGanymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Mauk et al. [2002]
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Satellite Footprints Seen in Jupiter
AuroraThis ultraviolet image of Jupiter was taken with the Hubble
Space Telescope Imaging Spectrograph (STIS) on November 26, 1998.
John Clarke, BU, USA. Ganymede's auroral footprint. near the
center,
Space Research Institute, 7 March 2013, 12:00 12:20
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Unipolar jovian generator Schematic of the
relationship between observed equatorial electron field-aligned
enhancements reported by Tomas et al. [2004a, 2004b] and the
circuit of electric currents that connects Jupiters middle
magnetosphere to the auroral ionosphere. The auroral circuit figure
is based on concepts of Hill [1979] and Vasyliunas [1983] as
replotted by Mauk et al. [2002]. It is understood that the shape of
the field lines in the actual Jovian system are substantially
stretched away from the dipolar configuration. Landay and Lifshitz,
1959Mauk et al. [2002].
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Ganymede/plasma parametersBo, jovian magnetic field, 64 nTne, 5
elns cm3< Z >, eq. av. (lobe) ion charge 1.3 < A >, eq.
av. (lobe) ion mass in mp 14 ni, ion no. density 4 ions/cm3m, ion
mass density 54 amu/cm3kTi, equator ion temperature 60 eVkTe,
electron temperature 300 eV pi,th, pressure thermal 0.04 nPapi,en
(20 keV 100 MeV ions) 3.6 nPa pe (both cold and hot electrons) 0.2
nPap(nPa), eq. (max) total pressure 3.8 nPa
vcr, local corotation velocity 187 km/s vs, satellite orbit
velocity 11 km/s v, plasma azimuthal vel. 150 km/su, relative
velocity (range), 139 km/s vA, eq. Alfven speed 190 km/s cs, eq.
sound speed 280 km/s B2o/2o, eq. (lobe) magnetic pressure 1.6
nPau2, eq. av. ram pressure 1.7 nPau2, lobe ram pressure 0.08
nPa
Bs, maximum Ganymede surface field 1500 nTA= (ovA)1, Alfven
cond. eq. 4.2 S P, av. ionosph. Pedersen cond 2 S H, av. ionosph.
Hall cond 0.1 SM/mi, ions per s added locally to flow 6x1026 s1
fpe, av. electron plasma freq. 20 kHzfpi, av. plasma freq. mass
mi ion 140 Hzfce, eq. (lobe) electron cyclotron freq. 1.8 kHzfci,
eq. (lobe) cyclotron freq. mass mi ion 0.09 Hzg,th thermal ions
gyroradii eq. (lobe) 36 kmg,pu pickup ions gyroradii eq. (lobe) 200
km
MA = u/vA equator (range) 0.73Ms = u/cs(range) Mf = u/( v2A +
c2s)1/2 (range) 0.5v /vcr 0.8 A (degrees) =tan1(u/vA) 36 = p /
(B2/2o) (lobe) 2.4P (av)g/A (eq) 0.5M /iur2s(range) 5-500Bsurf /
Bbg(range) 13-23,pgu/rs(range) 0.01-0.08Ganymede Lander, GLCW_6_06,
Moscow Space Research Institute, 7 March 2013, 12:00
12:20*Kivelson, et al. (2004), Magnetospheric interactions with
satellites, in Jupiter: The Planet, Satellites and Magnetosphere,
Cambridge Univ. Press, Cambridge, U. K.
Space Research Institute, 7 March 2013, 12:00 12:20
- Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Inductive interaction of conducting bodies
with amagnetized plasma, A. V. Gurevich, A. L. Krylov, and E. N.
Fedorov, Zh. Eksp. Teor. Fi., 75, 2132-2140 (1978) VA
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Jia et al., JGR, 2009
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Imp=2 RssBmp/0=1 MAI=A 6RGV flow BJ
I = DVB/0VA, Belcher [1987]
I= MA 6RG BJ/0=1.14 MAJia et al., JGR, 2008
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Ganymede Lander, GLCW_6_06, Moscow Space Research Institute, 7
March 2013, 12:00 12:20*Figure 1. Raw HST image (zoom) of Jupiters
northern auroral region displaying the ultravioletfootprint of
Ganymede in the anomaly region. The image was obtained with
HST/ACS/SBC with the F125LP filter on 2 March 2007 during the
GO-10862 HST campaign. The central meridian longitude is 145 (S3),
and the exposure time is 100 s.
Controversy Grodent, D., B. Bonfond, A. Radioti, J.-C. Gerard,
X. Jia, J. D. Nichols, and J. T. Clarke (2009), Auroral footprint
of Ganymede, J. Geophys. Res., 114, A07212,
doi:10.1029/2009JA014289
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Hubble Space Telescope images shown auroral emission from
electron excited atomic oxygen. Ganymede Lander, GLCW_6_06, Moscow
Space Research Institute, 7 March 2013, 12:00 12:20*Controversy
Mellisa A McGrat et al, JGR, in press 2013 doi: 10.1002/jgra.50122
Line at 1356 Open-closed field line boundaryThe thermal Jovian
plasma at Ganymede can produce a maximum of only ~10-40 R, Max
brightness are 200 R 400 R 300 R intensity can produce by 75-300
eV
Space Research Institute, 7 March 2013, 12:00 12:20
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The emitted power of Ganymedes auroral foot-print as a function
of Ganymedes orbital longi-tude and, consistently, as a function of
Ganymedes latitude in Jupiters plasma sheet.Ganymede Lander,
GLCW_6_06, Moscow Space Research Institute, 7 March 2013, 12:00
12:20*Controversy Grodent et al, JGR, 2009Ganymedes auroral
footprint 400 kV2 A = 800 GW Emitted power 2 GW ~0.25%
Space Research Institute, 7 March 2013, 12:00 12:20
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ConclusionsGanymedes orbit is mostly interesting region of the
Jupiters magnetosphere.Magnetometer and energetic particle detector
with energy 1 keV 1 Mev data will bring a high scientific
output.Steady magnetic reconnection and particle acceleration can
be studiedAurora phenomena can be studied by UV imagerGanymede
Lander, GLCW_6_06, Moscow Space Research Institute, 7 March 2013,
12:00 12:20*
Space Research Institute, 7 March 2013, 12:00 12:20
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Thank you!!!Ganymede Lander, GLCW_6_06, Moscow Space Research
Institute, 7 March 2013, 12:00 12:20*
Space Research Institute, 7 March 2013, 12:00 12:20
Explanation:Two dark shadows loom across the banded and
mottledcloud tops of Jupiterin this sharp telescopic view. In fact,
captured on January 3rd, about a month after the ruling gas giant
appeared at opposition inplanet Earth's sky, the scene includes the
shadow casters. Visible inremarkabledetail at the left are the
largeGalilean moonsGanymede (top) and Io. With the two moon shadows
still in transit, Jupiter'srapid rotationhas almost carried its
famousGreat Red Spot(GRS) around the planet's limb from the right.
The pale GRS was preceded by the smaller but similar huedOval BA,
dubbed Red Spot Jr., near top center. North is down in
theinvertedimage.
*Kivelson, M. G., F. Bagenal, W. S. Kurth, F. M. Neubauger, C.
Paranicas, and J. Saur (2004), Magnetospheric interactions with
satellites, in Jupiter: The Planet, Satellites and Magnetosphere,
edited by F. Bagenal, T. E. Dowling, and W.B. McKinnon,pp.513 536,
Cambridge Univ. Press, Cambridge, U. K.
* Figure 4. (a) Flows and the projection of field lines (white
solid lines) in the XZ plane at Y = 0. Colorrepresents the Vx
contours, and unit flow vectors in yellow show the flow direction.
A theoreticalprediction of the Alfven characteristics (orange
dashed lines) is shown for reference. The projection of
theionospheric flow is also shown as color contours on a circular
disk of r = 1.08 RG in the center. (b) Azoomed-in view of the light
area in Figure 4a. Flow streamlines are superimposed on color
contours ofVx. Note that the color bar differs from that in Figures
4a and 4b in order to illustrate the relatively weakflow within the
magnetosphere. (c) Same as Figure 4a but in the YZ plane at X = 0.
(d) Field-alignedcurrent density along with unit flow vectors shown
on a sphere of radius r = 1.08 RG.*Figure 7. (a) Color contours of
the current density (Jy) in the ^Y direction plotted in the XZ
plane at Y =0. The projection of magnetic field lines in this plane
is superposed as green lines with arrowheadsrepresenting the field
orientation. (b) Same as Figure 7a but for the field-aligned
current density (Jpar) inthe YZ plane. Flow is into the plane. (c)
A global view of the current flowlines in the magnetospherefrom the
upstream flank side. The axes are labeled in units of Ganymedes
radii RG.
*Figure 2. Ganymede auroral emission from atomic oxygen
illustrating the different morphologies on the different
hemispheres of the satellite. The magnetospheric plasma flow is
into the page for the trailing hemisphere, out of the page for the
leading hemisphere, and approximately from right to left for the
Jupiter-facing hemisphere. The black and white dashed line in each
image represents the 0 (2003 and 2007), 90 (2000), or 270 (1998)
deg W longitude meridian.
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