Measuring Proton Energies and Fluxes Using EIT (SOHO) CCDs Areas Outside the Solar Disk Images. L. Didkovsky 1 , D. Judge 1 , A. Jones 1 , and J. Gurman 2 1 USC Space Sciences Center 2 Goddard Space Flight Center. We Propose.
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L. Didkovsky1, D. Judge1, A. Jones1, and J. Gurman2
1USC Space Sciences Center
2 Goddard Space Flight Center
“Why haven’t we made more progress in understanding SEP events?”, - T. von Rosenvinge (Chapman Conference on Solar Energetic Plasmas and Particles, 2004, Finland)
Original SW area
Of 128 x 128 pix
One-pixel Events and CCD Deposited Energy Areas Outside the Solar Disk Images
Angles of incidence (spatial areas) to create one-pixel events into 21x21x12 m EIT CCD
The largest low-energy flux and the largest trend: 10/28
The largest high-energy flux, the smallest trend, and the smallest time delay from the X-ray peak: 01/20
An example of extracted from EIT (thick lines) proton fluxes in four energy ranges of 47, 150, 316, and 415 MeV compared to the GOES (thin lines) database. Dotted line shows GOES X-ray flare profile for reference in arbitrary units. Some dropouts are due to a low statistics of the SEP events.
10:48:10 (415 MeV)
Concentration in space/time
11:00:10 (415 MeV)
Proton Flux Anisotropy Areas Outside the Solar Disk Images
Wind Satellite data (http://lepmfi.gsfc.nasa.gov/mfi/)
Concentration in space
Concentration in time