SEP Properties and Magnetic Field Connection of the Source Region

Details SEP Properties and Magnetic Field Connection of the Source Region SEP Properties and Magnetic Field Connection of the Source Region

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh41b..06n&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH41B-06

Other

7509 Corona, 7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7519 Flares, 7524 Magnetic Fields

Scientific paper

There seems to be no clear explanation as to why some CME/flare events produce major SEP events whereas others do not. Furthermore, we still cannot reliably predict the peak flux and rise time of an SEP event using remote sensing data. Even though CME shocks are the primary accelerator for gradual SEP events and they are likely to have wide angular extensions, we suggest that the magnetic field connection of the source region to the observer may be an important factor for determining their occurrence and basic properties. In order to address this issue, we need to go beyond the common assumption that the longitudes around W60 have the strongest connection to the Earth. For a number of SEP-productive active regions, we compare the properties of intense flares and energetic CMEs that originated from them over their disk passage with the peak fluxes and rise times of the associated >10 MeV and >50 MeV protons. We perform magnetic field extrapolation with the potential field source surface (PFSS) model to locate well-connected field lines with respect to the source region. Once evaluated against multiple criteria, the PFSS extrapolation would be a useful tool to characterize the magnetic field topology in and around the active region responsible for the intense flares and energetic CMEs. This study is expected to partially answer the question of whether flare- accelerated particles contribute to gradual SEP events.

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