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Solar Wind Induced Escape on Mars and Venus. Mutual Lessons from Different Space Missions

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.

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Solar Wind Induced Escape on Mars and Venus. Mutual Lessons from Different Space Missions

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  1. 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

  2. SOLAR WIND INDUCED ESCAPE E B Plume of PI BL lobes Plasma sheet Ionospheric (polar) wind MEX /ASPERA-3

  3. SOLAR WIND INDUCED ESCAPE

  4. COLD IONOSPHERIC IONS FAR IN TAIL POLAR WIND Cold ionospheric ions Cold ionospheric ions

  5. SOLAR WIND INDUCED ESCAPE

  6. ESCAPE OVER REGIONS WITH STRONG CRUSTAL FIELDS UV background

  7. PLASMA SHEET dayside P (ASPERA-3) dyn P (MARSIS) M nightside some part of momentum thermal pressure

  8. ESCAPE THROUGH PLASMA SHEET IS CONTROLLED BY SW VARIATIONS K is momentum transfer factor (~0.1)

  9. CMEs IMPACT VENUS AND MARS

  10. MERCURY CME CME PP PM~29 nPa 4-5 June hours VENUS CME CME hours PM~5.3 nPa

  11. MARS (MARSIS DATA) Sequential plot for local |B|:9475, 9481, 9482, 9487

  12. MARS (MARSIS DATA) Sequential plot for ionospheric peak ne:9475, 9481, 9482, 9487

  13. MARS VENUS Different modes of ELS

  14. - OTHER OPEN QUESTIONS?

  15. - 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)

  16. ’FILAMENTATION’ OF PLASMA FLOW AROUND MARS 2050 2100 2110 2120 2130

  17. PLASMA FILAMENTATION IN MULTI-FLUID AND HYBRID SIMULATIONS YZ-PLANE XZ-PLANE PROTON NUMBER DENSITY PROTON NUMBER DENSITY MULTIPLE SHOCKLETS SW Z, Rm x=0 X, Rm Y, Rm

  18. MAGNETIC FIELD IN IONOSPHERE

  19. IONOPAUSE OR… ? density altitude

  20. WHAT IS AN OBSTACLE FOR SW ? PHOTOELECTRON BOUNDARY PILEUP BOUNDARY ALFVEN SPEED

  21. INVERTED V STRUCTURES ON MARS AND AURORA? M A R S E A R T H

  22. DO WE UNDERSTAND CLEARLY WHAT IS INDUCED MAGNETOSPHERE? SOLAR WIND WITH ALIGNED IMF

  23. VENUS EXPRESS OBSERVATIONS

  24. FIELD CONFIGURATION (POLOIDAL FIELDS) Without flow With flow With flow and leakage of dipole field outwards

  25. REVERSED DRAPING OR WRAPPING EFFECT

  26. REVERSED DRAPING OR WRAPPING EFFECT

  27. CURRENT PATTERN

  28. E+ - hemisphere E- - hemisphere

  29. CONCLUSIONS WHILE THE IDEA OF AN INDUCED MAGNETOSPHERE ATFIRST SEEM STRAIGHTFORWARD, IT IS NOT A PARTICULARLY WELL-CONSTRAINED CONCEPT WHEN APPLIED TO VENUS AND MARS WE NEED A MISSION WITH ADEQUATE PAYLOAD TO ADDRESS THESE QUESTIONS (MAVEN ?)

  30. BACKUP Launch, 18 November 2013 3-axis-stabilized, sun-pointing spacecraft 75o inclination, 4.5-hour period orbit Five 5-day “deep dip” campaigns with periapsis altitudes down to the homopause (~125 km). Nominal periapsis: ~150 km Eight science instruments, grouped into three packages

  31. The MAVEN Science Instruments Mass Spectrometry Instrument Particles and Fields Package Remote-Sensing Package

  32. BACKUP

  33. ESCAPE FLUXES AS A FUNCTION OF SW FLUX

  34. IONOSPHERIC EROSION EROSION IS TRIGGERED BY SOME UNKNOWN FACTORS OVER CRUSTAL FIELD REGIONS 5th Alfven Conference, October 5, 2010, Sapporo, Japan

  35. ELECTRON ACCESS VERSUS TOTAL CRUSTAL FIELD By (IMF) > 0 By(IMF) < 0 By < 0 SW Electron Flux ALT, km E= - VxB B (400km),nT B (400km),nT - By_IMF < 0 supports electron access to lower altitudes 5th Alfven Conference, October 5, 2010, Sapporo, Japan Dubinin et al., AG, 2008

  36. MAGNETIC FIELD AT LOW ALTITUDES By (IMF) is negative

  37. MAGNETIC FIELD AT LOW ALTITUDES By (IMF) is positive FLUX ROPE (Zhang et al. 2012) OR ELECTROJET

  38. -Thermal escape of hydrogen is the dominant process Mean flux ~ 1.6 x 10 cm s 26 -1 8 -2 -1 ~ 2x 10 s -1 ? 26 ~ 10 s

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