Hydrogen line spectra of a nonthermal proton beam. due to charge exchange in solar flares

Details Hydrogen line spectra of a nonthermal proton beam. due to charge exchange in solar flares Hydrogen line spectra of a nonthermal proton beam. due to charge exchange in solar flares

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297..854f&link_type=abstract

Astronomy and Astrophysics, v.297, p.854

Astronomy and Astrophysics

Astrophysics

23

Line: Profiles, Radiative Transfer, Sun: Flares

Scientific paper

Using more recent values of the atomic parameters and a more refined atmospheric model, the nonthermal line emission resulting from proton-hydrogen charge exchange has been recomputed. Confirming the results of Canfield & Chang (1985), the hydrogen Hα nonthermal line emission was found too small to be detectable. On the other hand, the nonthermal emission in the red wings of the Lyα and Lyβ lines is significantly high and can be used as a diagnostic of low energy protons. However, this emission is at least one order of magnitude lower than the value derived by Canfield and Chang.

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