Stellar chromospheres

Abstract

The interpretation of stellar chromospheric line intensities and widths is discussed, and semiempirical chromospheric models of single stars are reviewed. Theoretical chromospheric models based on the short period acoustic wave theory are shown to have promise for explaining the heating of the lower chromospheres of quiet chromosphere stars, but are inadequate to explain the heating of transition regions and coronae of active chromosphere stars and solar plages. Attention is given to the Wilson-Bappu (1957) relation between the widths of the Ca II H and K line emission cores and stellar absolute luminosity, while an examination of the calculations of Basri (1979) reveals that it is essential to solve the transfer equation properly before studying the physical basis of width-luminosity relations. Also considered are theoretical calculations of profiles of optically thick chromospheric lines in the presence of systematic flow patterns.