Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977afz....13..587g&link_type=abstract
Astrofizika, vol. 13, Nov. 1977, p. 587-603. In Russian.
Astronomy and Astrophysics
Astronomy
12
Atmospheric Models, Binary Stars, Flare Stars, Stellar Atmospheres, Stellar Radiation, Stellar Spectra, Chromosphere, Continuous Spectra, Energetic Particles, Hydrogen Atoms, Light (Visible Radiation), Photosphere, Solar Flares, Ubv Spectra
Scientific paper
Physical conditions in flares of UV Ceti-type stars are analyzed under the assumption that optical flares occur in a photosphere-chromosphere transition region where the atomic density is of the order of 10 to the (15th to 17th) power per cu cm. A hydrogen gas with such density at temperatures of 5000 to 20,000 K is considered. It is shown that the radiation from this gas at temperatures less than 10,000 K consists of emission from hydrogen atoms and negative hydrogen ions, while at higher temperatures the flare region is partially opaque to continuum emission. The U-B and B-V color indices, Balmer jump, and continuum energy distribution of the gas emission are calculated, and the results are found to be in general agreement with observational data. It is concluded that a UV Ceti-type optical flare is basically a secondary phenomenon caused by some 'explosion' in the upper atmospheric layers and that radiation produced directly by the explosion may appear during the initial flare phase. The problem of flare energetics is discussed along with an analogy between stellar and solar flares.
Grinin V. P.
Sobolev Vladimir
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