SEPs and Solar Radio Bursts S. Krucker and H. Hudson Time-of-flight analysis of SEP propagation Connectivity of the SEP field lines SIRA relevance

Event of Dec. 6, 2000: a “classic” type III burst with X-rays, radio waves, plasma waves, and particles leading to a “good” timing result (Krucker and Lin, ApJ 542, L61, 2000)

A “delayed” event (an extreme example!); the inverse-beta analysis leads to an injection time substantially following ihe impulsive-phase type III bursts.

Injection time and EIT wave location: hypothesis of shock acceleration at a site remote from the flare itself.

Modeling the origins of the heliospheric fields Particle cross-field transport is weak, so that the field lines guiding the particles are open Several groups are actively working on modeling the connectivity The modelers have confirmed the result from type III bursts, namely that active- region fields may be open

Schrijver & Derosa, Solar Phys. 212, 165, 2003 Open field lines within an active region found by PFSS modeling Open lines Closed lines

Nitta et al., SPD (June 2003) Open field lines in a flaring AR (see movie). Black lines connect to source surface via the Schrijver- Derosa PFSS model

3D reconstruction of type III electron trajectories (Paesold et al., A&A 371, 331, 2001)

What can we learn from SIRA? The April 7 SEP event was in the east, and in principle therefore poorly connected. What is the connectivity? SIRA can help us locate the acceleration/injection for such events by event tracking. The “top of the corona” is poorly modeled by PFSS (or MHD) techniques and not observed almost at all. SIRA is our best bet for understanding the structure of this region by direct imaging.