A Search for Optical Proxies for High Energy Emissions from Solar Flares

Details A Search for Optical Proxies for High Energy Emissions from Solar Flares A Search for Optical Proxies for High Energy Emissions from Solar Flares

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997phdt........18b&link_type=abstract

Thesis (PHD). UNIVERSITY OF HAWAII , Source DAI-B 58/05, p. 2468, Nov 1997, 164 pages.

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X Rays

Scientific paper

Solar flares have high energy emission in soft and hard X-rays, either of which may be associated with the initial energy release, and optical emission from secondary heating of the chromosphere. Stellar astronomers typically are limited to the optical and soft X-ray thus limiting their investigation of the dynamics of stellar flares. Stellar astronomers assert they have found optical proxies for high energy emission from stellar flares. This dissertation tests that assertion by searching for optical proxies for high energy emissions from solar flares. This dissertation also examines the partitioning of the initial energy release. The search was performed on thirty-one flares observed in Ca II K, soft X-rays and hard X-rays. Twenty-seven of these flares had Hα. The optical data were reduced to photometry by applying a time-invariant aperture. I discovered that the Hα and Ca II K lines are adequate flux proxies for one another with Hα emitting twice the Ca II K flux. The optical lines rise like the hard X-rays and decay like the soft X-rays. The optical lines can be used as temporal proxies on time scaled longer than the lag between the soft X-ray and optical maxima. The optical lines are also good flux proxies for the soft X-rays. There is no evidence that Hα is a flux proxy for injected electron beam. I have found that the initial energy release is not partitioned, but is primarily transferred into non-thermal energization of particles. Since these flares are X-ray weak, and the radiated energy from the coronal emission is far less than the energy contained in the beam, I conclude that the deposition of the beam in the chromosphere is not strong enough to evaporate lots of plasma to coronal temperatures and an atypically large amount of material must be evaporated to transition region temperatures. I predict that these flares should be EUV-bright.

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