Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...380..660g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 380, Oct. 20, 1991, p. 660-676.
Astronomy and Astrophysics
Astrophysics
13
Chromosphere, H Lines, Plasma Heating, Radiative Transfer, Solar Flares, Absorption Spectra, Balmer Series, Lyman Alpha Radiation, Solar Spectra, Stellar Models
Scientific paper
Strong flare heating that penetrates deeply into the solar chromosphere is examined, and a simple model that is supported by a numerical radiative transfer simulation is applied to study how elevated free electron densities produce markedly increased Stark emission in the wings of hydrogen Lyman and Balmer lines. The proportionality that exists between the observed Stark wing intensity and the total energy deposition in the partially ionized layer is calculated for various Lyman and Balmer lines. It is concluded that when the effects of background opacity sources on the wing enhancements are not important, the magnitude of the nonthermal heating that penetrates the chromosphere may be inferred from the observed line wings. It is predicted that Ly-alpha extended wings will exhibit enhancement of Stark shape, even when inherent damping wing opacity exceeds Stark wing opacity over the entire absorption profile.
Canfield Richard C.
Gayley Ken G.
No associations
LandOfFree
Inferring chromospheric flare heating from hydrogen-line wings does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Inferring chromospheric flare heating from hydrogen-line wings, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Inferring chromospheric flare heating from hydrogen-line wings will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1875404