The nature of stellar active regions

Details The nature of stellar active regions The nature of stellar active regions

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983pasp...95.1025w&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 95, Dec. 1983, p. 1025-1032.

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4

Dwarf Stars, Main Sequence Stars, Radiative Transfer, Stellar Activity, Stellar Atmospheres, Calcium, Chromosphere, Emission Spectra, Faculae, G Stars, Hydrogen, K Stars, Line Spectra, Potassium, Radiant Flux Density, Stellar Models, Stellar Spectrophotometry

Scientific paper

Observational estimates of chromospheric radiative loss rates in Ca II H and K in main-sequence F, G, and K dwarfs are used to compare stars that span a range of activity levels with each other and with the sun. For stars with spectral types similar to that of the sun, it is found that chromospheric radiative losses in stars with active chromospheres exceed the flux emitted by plages on the sun at solar maximum by about a factor of 6. If this difference is due primarily to a difference in the fraction of the stellar surface covered by plage-like material, and not to a change in the character of the emission-line regions, then more than half of the stellar surface in stars with large chromospheric radiative loss rates must be covered by active regions. It is also possible to show that active regions in young solar-type stars extend at least to latitudes + or - 25 deg from the rotational equator and that a typical individual region contributes no more than 2 percent - 3 percent of the total H and K emission. In Kappa Cet, observations show that the rotational modulation persisted in both phase and amplitude for at least 100 days (12 rotation cycles).

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