Theoretical models of homogeneous chromospheres for main sequence stars

Details Theoretical models of homogeneous chromospheres for main sequence stars Theoretical models of homogeneous chromospheres for main sequence stars

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...105...23m&link_type=abstract

Astronomy and Astrophysics, vol. 105, no. 1, Jan. 1982, p.23-36. Research supported by the Polska Akademia Nauk.

Astronomy and Astrophysics

Astrophysics

5

Atmospheric Models, Chromosphere, Main Sequence Stars, Spectral Line Width, Stellar Radiation, Atmospheric Heating, Energy Spectra, Semiempirical Equations, Stellar Magnetic Fields, Stellar Temperature

Scientific paper

It is shown that the structure of the chromosphere is determined by three parameters: (1) the dissipating wave period; (2) the energy flux spectrum provided to the chromosphere; and (3) the magnetic field; where these parameters are mutually dependent, with the greatest dependency being between the energy flux spectrum value and the magnetic field. The analysis presented demonstrates that it is impossible to reconstruct the semi-empirical models considered when short-period waves are adopted for heating. The range of energy flux spectrum values given is from 10 million erg/sq cm per sec, for the case of stars cooler than the sun, to 100 million erg/sq cm per sec for the case of stars that are hotter. The results contradict theoretical estimates of convective zone-generated mechanical energy flux, especially for cooler stars. It is concluded that the strength of the average magnetic field determines the division of stars into those with weak, and those with strong, chromospheric activity.

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