On the interpretation of chromospheric emission lines

Details On the interpretation of chromospheric emission lines On the interpretation of chromospheric emission lines

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...348..279j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 348, Jan. 1, 1990, p. 279-296.

Astronomy and Astrophysics

Astrophysics

48

Chromosphere, Emission Spectra, Stellar Spectra, Ultraviolet Spectra, Atomic Energy Levels, Forbidden Transitions, Radiative Transfer, Stellar Activity, Stellar Coronas

Scientific paper

This paper reexamines the formation of ultraviolet emission lines in stellar chromospheres, using detailed radiative transfer calculations and relatively simple methods based on approximate line cooling rates, including escape probabilities. Approximations for the cooling integrals are demonstrated to work well for 'effectively thin' chromospheric lines. Two cases are identified, whose behavior can be understood using Ayres's (1979) chromospheric scaling laws relating the chromospheric structure to stellar properties: those of inactive stars, like cool giants, and more active stars like the sun.

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