On Temporal Variation of the 0.511MeV Line in A Solar Flare

Details On Temporal Variation of the 0.511MeV Line in A Solar Flare On Temporal Variation of the 0.511MeV Line in A Solar Flare

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999soph..186..311g&link_type=abstract

Solar Physics, v. 186, Issue 1/2, p. 311-318 (1999).

Physics

5

Scientific paper

The time profile of the 0.511MeV line flux for the flare of 16December 1988 is studied. Differing from previous conclusions, we found that a fixed spectral index cannot fit the observations. It is shown that a good fit can be realized if the spectral index varies with time. But the same good fit can be also obtained if the conversion factor of positrons to the 0.511MeV photons changes with time. At present it is very difficult to say which situation is more practical.

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