Chromospheric Line Blanketing and the Hydrogen Spectrum of dM Stars

Details Chromospheric Line Blanketing and the Hydrogen Spectrum of dM Stars Chromospheric Line Blanketing and the Hydrogen Spectrum of dM Stars

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.8109s&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #81.09; Bulletin of the American Astronomical Society, Vol. 28, p.1383

Astronomy and Astrophysics

Astronomy

Scientific paper

We present non-LTE calculations of the Hi spectrum in a grid of chromospheric models that represents a dM0 star in which the activity level ranges from quiescent to very active. We investigate three different treatments of the background opacity: 1) continuous opacity only, 2) blanketing due to lines that form in the photosphere below Tmin, and 3) blanketing by lines that form throughout the entire outer atmosphere. We show that the predicted W_lambda of Lyalpha in all models, and of Hα in very active (dMe) stars, is reduced by as much as a factor of ~ 4 by the inclusion of background line opacity. A consistent treatment of line blanketing that includes the effect of the chromospheric and transition region temperature structure in the calculation of background line opacity is necessary for the accurate calculation of Lyalpha , and in some cases Hα , in thes e stars. The Hα line in less active models, and the Pabeta line in all models, is negligibly affected by the treatment of background opacity. We also show that the broad-band continuum flux in regions where lambda < 2000 A is increased by as much as a factor of ~ 3 in some models by the inclusion of chromospheric line blanketing.

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