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Identification of Prominence Material in Magnetic Cloud

Identification of Prominence Material in Magnetic Cloud. Shuo Yao China University of Geosciences (Beijing) yaoshuo@cugb.edu.cn Co-authers: E. Marsch 2 , C.-Y. Tu 1 and R. Schwenn 2 1: Department of Geophysics, Peking University, China

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Identification of Prominence Material in Magnetic Cloud

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  1. Identification of Prominence Material in Magnetic Cloud Shuo Yao China University of Geosciences (Beijing) yaoshuo@cugb.edu.cn Co-authers: E. Marsch2, C.-Y. Tu1 and R. Schwenn2 1: Department of Geophysics, Peking University, China 2: Max-Planck-Institut for Solar System Research, Germany ILWS Workshop 2011, Friendship Hotel, Beijing, China

  2. Background 1. CME Bright loop---plasma pile up Dark cavity---magnetic flux ropes Bright core---prominence 3-part CME

  3. 2. Magnetic Cloud One type of Interplanetary Coronal Mass Ejection (ICME) Enhanced magnetic field strength Smooth rotation of magnetic field vector in day’s time Low proton temperature 171 172 173 Helios 1 1981 DOY171-173

  4. 3. Prominence Material NASA SOHO Prominence Filament Cold and dense material from chromosphere

  5. Temperature: 5000-8000K Character Ions:He+ Position in CME: Centre of the flux rope Priest 1989, Crooker and Horbury 2005 Zong et al,.2004 Gopalswamy, 2006

  6. 3. The problem Identification of 3-Part CME From In Situ MC Observations----Especially the prominence material !! Forbes et al., 2001 Bothmer and Schwenn, 1998 ？

  7. Report Flux Rope Np and Tp He+ However, not all the features identified in one event…….

  8. My work • Aim: identify prominence material from the in-situ observation of magnetic cloud. • Cases: • 1979DOY129, at 0.3 AU • 1976 DOY 90, at 0.5 AU • 1978DOY358, at 0.7 AU • Evidences: • High Np and low Tp • Located on centre of magnetic field flux rope • 3.Existence of He+ • 4. Heating before and after revealed by Velocity distribution function (temperature ) 8

  9. 0.3 AU 1. Satellite Helios 2: 1976-1980 electrostatic analyzers 9

  10. 2. Case Study Case 1 0.3 AU Flux rope structure High Np and low Tp Yao et al., 2010, JGR 10

  11. Possible existence of He+ E/q E/q~m/q H+ : He2+ : He+ m 1 4 4 q 1 2 1 m/q 1 2 4 Yao et al., 2010, JGR

  12. Thermal velocity distribution functions Solid Line——local B X——outward solar radial direction Heating perpendicular to B 12

  13. SOLWIND Observation 22 Hours ahead，Solwind observed CME with prominence eruption 600km/s×22h ~4.5×107 km ~0.3 AU 1AU~1.5×108 km Sheeley，1980

  14. Case 2 0.5 AU Flux rope structure High Np and low Tp 14

  15. Possible existence of He+ H+ : He2+ : He+ m 1 4 4 q 1 2 1 m/q 1 2 4 15

  16. Thermal velocity distribution functions Heated Plasma Before and After Prominence Material

  17. Case 3 0.7 AU Prominence material is 2 hours behind the neutral line of flux rope. Flux rope structure low Tp and High Np

  18. Possible existence of He+ H+ : He2+ : He+ m 1 4 4 q 1 2 1 m/q 1 2 4 18

  19. Thermal velocity distribution functions Heated Plasma Before and After Prominence Material 19

  20. Summary Complete evidences from in situ measurements Report Flux Rope Np and Tp He+ Yao 2010 X X X

  21. Model In situ measurement SOHO NASA Remote Observation Gopalswamy SpaceSciRew, 2006 Yao et al., 2010, JGR

  22. It seems….Closer to the Sun, the more info about CME So…we do expect more on Solar Orbiter & Solar Probe+ in the Next Cycle ….

  23. Thanks ! 23

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