The calculation of flux constant lineblanketed model atmospheres for solar type stars.
Abstract
Two computer programs have been used to compute flux constant model atmospheres, which include the effects of convection as well as line blanketing, for solar type stars. One program computes a model atmosphere and then calculates the integrated radiative flux and convective flux as a function of optical depth. After applying a lineblanketing correction to the fluxes, temperature corrections are calculated and a new model atmosphere computed. A second program computes the line blocking of a model atmosphere as a function of optical depth. The lineblocking data, expressed as a function of the radiative flux computed without allowance for line absorption, is used by the model atmosphere program to allow for line absorption effects. This method of computing lineblanketed model atmospheres, the flux fraction method, does not make the opacity correlation assumption that is inherent in the giantline method. Model atmospheres have been computed for the Sun, a metal deficient star ([A/H] =  ) and Groombridge 1830 and the colours of these models are discussed. The models do predict the observed variation of ultraviolet excess, 8( UB), with metal abundance.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 1973
 DOI:
 10.1093/mnras/164.3.197
 Bibcode:
 1973MNRAS.164..197B