HYDROGEN LINE SPECTRA OF A NONTHERMAL PROTON-BEAM DUE TO CHARGE-EXCHANGE IN SOLAR-FLARES

Using more recent values of the atomic parameters and a more refined a tmospheric model, the nonthermal line emission resulting from proton-h ydrogen charge exchange has been recomputed. Confirming the results of Canfield & Chang (1985), the hydrogen H alpha nonthermal line emissio n was found too small to be detectable. On the other hand, the nonther mal emission in the red wings of the Ly alpha and Ly beta lines is sig nificantly 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.