Particle Acceleration, Flares, and CMEs Hugh S. Hudson SSL, UC Berkeley 13 May 20111.
An Overall Framework for Solar Flares? H. S. Hudson Space Sciences Laboratory University of...
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Transcript of An Overall Framework for Solar Flares? H. S. Hudson Space Sciences Laboratory University of...
An Overall Frameworkfor Solar Flares?
H. S. HudsonSpace Sciences Laboratory
University of California, Berkeley
CS-16 29/08/10
CS-16 29/08/10
Dimming, implosion, oscillations
A broad framework
• How does the flare instability work?• Formation of signatures• Plasma physics• Consequences
- Coronal structure
- Astrobiology?
CS-16 29/08/10
What is the basic physics of a flare/CME, and how do we relate observations of many diverse types to understanding it?
One natural approach is to make a cartoon, understood to be a kind of giant interpolation formula
CS-16 29/08/10
Contributions welcome!
Contributions welcome!
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Google “Flare Cartoons”
Cartoons
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Tan & Huang 2006
Anzer & Pneuman 1982
Fletcher & Hudson 2008
http://solarmuri.ssl.berkeley.edu/~hhudson/cartoons
Ergun et al. 2002
Formation of signatures:spectroscopy
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• Problem of solar UV spectroscopy (lack of!)• The impulsive phase: transition between thermal and
nonthermal plasma states• Particle acceleration
Plasma physics I: particle acceleration
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• The impulsive phase: electrons at 104 kT dominate
• The coronal phase: LCR ~ 0.1 Lbol
Mewaldt et al. 2007
Plasma physics II
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• How does the flare instability proceed?
• How do we understand the coupling of scales?
• Physics of waves• Ion-neutral physics in the
chromosphere
Consequences
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• The nanoflare hypothesis• Luminosity: Is the diverted energy important?• Hard radiation and astrobiology?
A broad framework
• How does the flare instability work?• Formation of signatures• Plasma physics• Consequences
- Coronal structure
- Astrobiology?
CS-16 29/08/10
What is the basic physics of a flare/CME, and how do we relate observations of many diverse types to understanding it?
One natural approach is to make a cartoon, understood to be a kind of giant interpolation formula
Conclusions
• Solar flares, for all their complexity, have simple organizing principles
• The basic question – “How does the impulsive phase work?” – remains unanswered
CS-16 29/08/10
See also Hudson & Micela, CS-14
Thanks
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CS-16 29/08/10
Magnetic changes during flares
“Confusogram” legend: 10x10 2.5” pixels 240 minutes time base 500 G magnetic range
(Sudol & Harvey 2005)
CS-16 29/08/10
Flare energy
Woods et al 2004
Hudson et al 2006
In time In space