relationships between flares and cmes h.s. hudson space sciences lab, uc berkeley
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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
SHINE WG 1, 23 January 2008 3/22-
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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SHINE WG 1, 23 January 2008 14/22-
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!
SHINE WG 1, 23 January 2008 22/22-
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