Solar sources of impulsive SEPs

Special one-day seminar at SSL, Berkeley

Nov. 3, 2006 (09:00-15:00)

http://sprg.ssl.berkeley.edu:80/RHESSI/iseps/

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X-ray jet (EUV, WL?) Flare Coronal hole

Skinny coronal hole Helmet streamer Spike burst / IIIs

Candidate Counterparts I

Candidate Counterparts II

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High coronal flare

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Post-CME turbulence

CME-driven shockFlare shock Previously owned particles

Type III burst

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What are the problems?

• What thing accelerates the SEPs?

• How is the chemical signature imposed (elemental, isotopic, ionization)?

• What is the physics of the acceleration?

• What causes the observed delays?

• Does the problem of magnetic connectivity require an extended source region?

• Are there multiple types of counterpart for the impulsive SEPs?