Theoretical studies of the RS Canum Venaticorum stars

Details Theoretical studies of the RS Canum Venaticorum stars Theoretical studies of the RS Canum Venaticorum stars

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982udnw.rept.....m&link_type=abstract

Final Report, 1 Jan. 1980 - 31 Dec. 1981 Delaware Univ., Newark.

Mathematics

Chromosphere, Giant Stars, Photosphere, Stellar Magnetic Fields, T Tauri Stars, Balmer Series, Dwarf Stars, Hydrogen Atoms, Mathematical Models, Radiative Heat Transfer

Scientific paper

The activity in RS Canum Venaticorum (CVn) is investigated. Models for chromospheric structure are developed and the role of magnetic fields both in the photosphere as well as in the chromosphere and upper atmosphere are examined. T Tau stars are also studied from the same points of view. The properties of magnetic field loops are used to help understand the atmospheric structure in RS CVn stars. The concepts developed in the case of these stars appear to be applicable over a much broader region of the HR diagram. The absence of stable magnetic loops in the atmospheres of late type giant stars suggests that the atmospheres of RS CVn active components are qualitatively distinct from the solar atmosphere.

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