solar wind induced escape on mars and venus. mutual lessons from different space missions
DESCRIPTION
Solar Wind Induced Escape on Mars and Venus. Mutual Lessons from Different Space Missions. E. Dubinin Max-Planck Institute for Solar System Research, Katlenburg-Lindau, Germany. SOLAR WIND INDUCED ESCAPE. E. B. Plume of PI. BL. lobes. - PowerPoint PPT PresentationTRANSCRIPT
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Solar Wind Induced Escape on Mars and Venus. Mutual Lessons from Different Space Missions
E. Dubinin
Max-Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
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Plume of PI
Plasma sheet
lobesBL
Ionospheric (polar) wind
SOLAR WIND INDUCED ESCAPEE
B
MEX /ASPERA-3
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SOLAR WIND INDUCED ESCAPE
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COLD IONOSPHERIC IONS FAR IN TAIL
Cold ionospheric ions
Cold ionospheric ions
POLAR WIND
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SOLAR WIND INDUCED ESCAPE
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ESCAPE OVER REGIONS WITH STRONG CRUSTAL FIELDS
UV background
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PLASMA SHEET
odswsw BVmn 2/22
22 / OOOon VmnB
P (ASPERA-3)P (MARSIS)dyn
M dayside
nightside
some part of momentum thermal pressure
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2/1))1(
(2 r
kff swO
2/1))1(
(222 r
krff swO
O
O
n
nr 2
sw
O
nn
ESCAPE THROUGH PLASMA SHEET IS CONTROLLED BY SW VARIATIONS
K is momentum transfer factor (~0.1)
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CMEs IMPACT VENUS AND MARS
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MERCURY
VENUS4-5 June hours
hours
CME CME
CME CME
PP
PM~29 nPa
PM~5.3 nPa
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MARS (MARSIS DATA)Sequential plot for local |B|:
9475, 9481, 9482, 9487
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MARS (MARSIS DATA)Sequential plot for ionospheric peak ne:
9475, 9481, 9482, 9487
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VENUS MARS
Different modes of ELS
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- OTHER OPEN QUESTIONS?
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- ION FORESHOCK ? (There are no reflected protons upstream of the nose of the Martian BS. Ion foreshock lies entirely downstrem of the subsolar point)
- HOT OXYGEN CORONA? (There are no ASPERA observations of oxygen ions which could be reliably identified as originated from hot oxygen corona)
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’FILAMENTATION’ OF PLASMA FLOW AROUND MARS
2050 2100 2110 2120 2130
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PLASMA FILAMENTATION IN MULTI-FLUID AND HYBRID SIMULATIONS
Z, Rm
Y, Rm
SW MULTIPLE SHOCKLETS
PROTON NUMBER DENSITY
X, Rm
PROTON NUMBER DENSITYXZ-PLANE YZ-PLANE
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MAGNETIC FIELD IN IONOSPHERE
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IONOPAUSE OR… ?density
altitude
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WHAT IS AN OBSTACLE FOR SW ?
ALFVEN SPEED
PILEUP BOUNDARYPHOTOELECTRON BOUNDARY
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MARS
EARTH
INVERTED V STRUCTURES ON MARS AND AURORA?
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DO WE UNDERSTAND CLEARLY WHAT IS INDUCED MAGNETOSPHERE?
SOLAR WIND WITH ALIGNED IMF
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VENUS EXPRESS OBSERVATIONS
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FIELD CONFIGURATION (POLOIDAL FIELDS)Without flow
With flow
With flow and leakage of dipole field outwards
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REVERSED DRAPING OR WRAPPING EFFECT
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REVERSED DRAPING OR WRAPPING EFFECT
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CURRENT PATTERN
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E+ - hemisphere E- - hemisphere
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CONCLUSIONS
WHILE THE IDEA OF AN INDUCED MAGNETOSPHERE ATFIRST SEEM STRAIGHTFORWARD, IT IS NOT A PARTICULARLYWELL-CONSTRAINED CONCEPT WHEN APPLIED TO VENUS AND MARS
WE NEED A MISSION WITH ADEQUATE PAYLOAD TO ADDRESS THESE QUESTIONS (MAVEN ?)
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BACKUP
Launch, 18 November 20133-axis-stabilized, sun-pointing spacecraft75o inclination, 4.5-hour period orbitFive 5-day “deep dip” campaigns with periapsis altitudes down to the homopause (~125 km). Nominal periapsis: ~150 kmEight science instruments, grouped into three packages
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The MAVEN Science Instruments
Mass Spectrometry Instrument
Remote-Sensing Package
Particles and Fields Package
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BACKUP
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ESCAPE FLUXES AS A FUNCTION OF SW FLUX
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OVER CRUSTAL FIELD REGIONS IONOSPHERIC EROSIONEROSION IS TRIGGERED BY SOME
UNKNOWN FACTORS
5th Alfven Conference, October 5, 2010, Sapporo, Japan
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ELECTRON ACCESS VERSUS TOTAL CRUSTAL FIELD
E= - VxB
SW
By < 0
ALT
, km
By (IMF) > 0 By(IMF) < 0
B (400km),nT B (400km),nT
Ele
ctro
n Fl
ux
- By_IMF < 0 supports electron access to lower altitudes
Dubinin et al., AG, 20085th Alfven Conference, October 5,
2010, Sapporo, Japan
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VnmBj ini
By (IMF) is negative
MAGNETIC FIELD AT LOW ALTITUDES
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VnmBj ini
By (IMF) is positive
MAGNETIC FIELD AT LOW ALTITUDES
FLUX ROPE (Zhang et al. 2012) OR ELECTROJET
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-Thermal escape of hydrogen is the dominant process Mean flux ~ 1.6 x 10 cm s8 -2 -1 ~ 2x 1026
s-1
~ 1026
s-1?