Relationships between flares and CMEs H.S. Hudson Space Sciences Lab, UC Berkeley.
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Transcript of Relationships between flares and CMEs H.S. Hudson Space Sciences Lab, UC Berkeley.
Relationships betweenflares and CMEs
H.S. Hudson
Space Sciences Lab, UC Berkeley
SHINE WG 1, 23 January 2008 2/22-
Contents
• Historical stuff• Energy and field• RHESSI coronal hard X-ray sources• Conclusions
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Historical high points• Recognition of CME phenomenon as distinct and
geoeffective• Clear evidence from the January 1997 event (Webb
et al., 1998) that yes, CMEs can happen without “flares” A
• Clear association of CME dynamics with compact, low-lying structures (X-ray dimming; Dere et al. 1997)
• The ill-considered controversy on causality arising from the “myth” debate B
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“…remarkably weak andunimpressive…” - Webb et al. 1998
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CME and flare energiesare well-correlated after all! - Burkepile et al. 2004
A
B
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Density, field, energy
QS
AR 10486
Wheatland et al. method,NLFFF by J. McTiernan
Potential
NLFFF excess
NLFFF excess50% contour
SHINE WG 1, 23 January 2008 6/22-
Density, field, energy
QS
AR 10486
Wheatland et al. method,NLFFF by J. McTiernan
Potential
NLFFF excess
NLFFF excess50% contour
WG 2!
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GONG
SOHO/MDI
B dB
Sudol & Harvey (2005), flare of 2003 Oct. 29,line-of-sight field differences
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Flare of 2001 Aug. 25:GONG + GOES
Other examples withGOES times
The changes are stepwise, of order10% of the line-of-sight field, andprimarily occur at the impulsive phase of the flare
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Timing of acceleration phase and dimming
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Zarro et al. 1999
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Zhang et al. 2001
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Implosive motion
Veronig et al. 2005
Hudson 2000
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TRACE movie: dimming and implosion
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Disk occultation
McKenzie 1975
Hudson 1978
Frost & Dennis 1971
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Splendid RHESSI observations, courtesy Säm Krucker I
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Splendid RHESSI observations, courtesy Säm Krucker II
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Splendid RHESSI observations, courtesy Säm Krucker III
Lin et al. 2002
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Coronal hard X-ray sources
Krucker et al. 2008
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What are the coronal sources?
• Large numbers of fast electrons trapped stably in coronal mirror geometries
• Early-phase sources (cf. Masuda event) are mysterious and probably really important
• Possibility that the tail of the electron distribution is the dominant pressure
• Moving sources may wind up being identified with the filament region of the CME
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Prototype moving source
Hudson et al. 2001
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Background information (flare models)
The “CSHKP” model(Anzer & Pneuman 1982)
The thick-target model(L. Fletcher)
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Fletcher & Hudson 2008
New description of the impulsive phase
http://solarmuri.ssl.berkeley.edu/~hhudson/cartoons/
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Fletcher & Hudson 2008
New description of the impulsive phase
http://solarmuri.ssl.berkeley.edu/~hhudson/cartoons/
Importance of Poynting flux!
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Conclusions
• Flares and CMEs are normally closely related• We need to study the low corona -chromosphere -
transition region to understand powerful CMEs• We have coronal nonthermal signatures in hard X-
rays from the new RHESSI observations