Expanding chromospheres of late G and K supergiants

Details Expanding chromospheres of late G and K supergiants Expanding chromospheres of late G and K supergiants

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.222..307m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 222, Sept. 15, 1986, p. 307-322.

Statistics

Computation

6

Chromosphere, G Stars, H Alpha Line, K Stars, Late Stars, Radiative Transfer, Stellar Mass Ejection, Supergiant Stars, Computational Astrophysics, Line Shape, Stellar Models, Temperature Dependence, Thermodynamic Equilibrium

Scientific paper

The radiative transfer problem in non-LTE moving atmospheres has been explicitly solved for Hα line profiles. These computations have been done for a schematic model of the line-forming region over a wide range of optical depths and velocity gradients in order to cover the observed characteristics in 23 G and K supergiants. The best theoretical fits yield optical depths in the range 10 - 500 and velocity fields in the range 0.5 - 3 Doppler widths. The computed mass-flow rates lie in the range 10-5 - 10-7M_sun;yr-1; the higher the extent of the line-forming region, the lower the mass-loss rates. The effect of the extent on the Hα emission components has also been investigated in some detail. The temperature sensitivity of the mass-loss rates has been considered in an approximate manner.

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