Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977ap%26ss..52...51g&link_type=abstract
Astrophysics and Space Science, vol. 52, no. 1, Nov. 1977, p. 51-104.
Astronomy and Astrophysics
Astrophysics
13
Atmospheric Models, Chromosphere, Stellar Models, Variable Stars, Flares, Gas Ionization, High Energy Electrons, Light Curve, Line Spectra, Metal Ions, Star Clusters
Scientific paper
An attempt is made to formulate a theory of flare-star chromospheres on the basis of the fast-electron hypothesis. The two components of flare light (continuum and emission-line) are discussed along with a typical flare light curve, the excitation-energy source for the emission lines, the intensity of ionizing Lyman-continuum radiation, emission-line excitation in stellar flares, and the duration of a flare in emission lines. The electron temperature and density in a flare-star chromosphere are analyzed, the duration of emission-line luminescence is evaluated, and it is suggested that the flare-heated chromosphere maintains emission-line excitation during 'quiescent' periods. Attention is given to the degree of ionization in a stellar flare, the Balmer decrement of the emission lines, variations in emission-line profiles during flares, the dependence of emission-line intensity on flare amplitude, and the two extreme types of flare star established by Haro (1964). The effects of radiation dilution and stellar spectral type on emission-line equivalent width are investigated, and the nature of slow flares is considered. The problem of forbidden lines is examined together with the possibility of observing the forbidden line of O III at 4363 A during a flare, the excitation of helium emission lines in flare-star spectra, Lyman-alpha emission in stellar flares, and the possible presence of the Mg II resonance doublet at 2800 A in flare-star spectra.
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