Identification of Prominence Material in Magnetic Cloud
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Identification of Prominence Material in Magnetic Cloud
Shuo Yao China University of Geosciences (Beijing)
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
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Background
1. CME
Bright loop---plasma pile up
Dark cavity---magnetic flux ropes
Bright core---prominence
3-part CME
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2. Magnetic CloudOne 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
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Prominence Filament
NASA SOHO
3. Prominence Material
Cold and dense material from chromosphere
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Temperature: 5000-8000K
Character Ions: He+
Position in CME: Centre of the flux rope Priest 1989, Crooker and Horbury 2005
Zong et al,.2004Gopalswamy, 2006
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?
Forbes et al., 2001
3. The problem
Bothmer and Schwenn, 1998
Identification of 3-Part CME From In Situ MC Observations----Especially the prominence material !!
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Report Flux Rope Np and Tp He+
However, not all the features identified in one event…….
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My workAim: 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:
1.High Np and low Tp
2.Located on centre of magnetic field flux rope
3.Existence of He+
4. Heating before and after revealed by Velocity distribution function (temperature )
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1. SatelliteHelios 2: 1976-1980
electrostatic analyzers
0.3 AU
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Case 1
0.3 AU
High Np and low Tp
Flux rope structure
2. Case Study
Yao et al., 2010, JGR
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Possible existence of He+
H+ : He2+ : He+ m 1 4 4q 1 2 1m/q 1 2 4
E/q E/q~m/q
Yao et al., 2010, JGR
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Thermal velocity distribution functions
Heating perpendicular to B
Solid Line——local B
X——outward solar radial direction
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22 Hours ahead , Solwind observed CME with prominence eruption
Sheeley , 1980
SOLWIND Observation
600km/s×22h
~4.5×107 km ~0.3 AU
1AU~1.5×108 km
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Case 2
0.5 AU
High Np and low Tp
Flux rope structure
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Possible existence of He+
H+ : He2+ : He+ m 1 4 4q 1 2 1m/q 1 2 4
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Thermal velocity distribution functions
Heated Plasma Before and After Prominence Material
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Case 3
0.7 AU
low Tp and High Np
Flux rope structure
Prominence material is 2 hours behind the neutral line of flux rope.
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Possible existence of He+
H+ : He2+ : He+ m 1 4 4q 1 2 1m/q 1 2 4
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Thermal velocity distribution functions
Heated Plasma Before and After Prominence Material
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Report Flux Rope Np and Tp He+
Yao 2010 X X X
Complete evidences from in situ measurements
Summary
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SOHO
Gopalswamy SpaceSciRew, 2006 Yao et al., 2010, JGR
NASA
Remote Observation
Model
In situ measurement
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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 ….
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Thanks !