A method to estimate the effect of line blanketing in NLTE radiative transfer calculations

Details A method to estimate the effect of line blanketing in NLTE radiative transfer calculations A method to estimate the effect of line blanketing in NLTE radiative transfer calculations

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...373..993b&link_type=abstract

Astronomy and Astrophysics, v.373, p.993-997 (2001)

Astronomy and Astrophysics

Astrophysics

13

Stars: Atmospheres, Radiative Transfer, Line: Formation, Ultraviolet: Stars

Scientific paper

We present a method to estimate the contribution of line opacity to the total opacity as a function of wavelength. The estimated line-opacity function can then be used to simulate line-blanketing in NLTE radiative transfer calculations. Given a reference flux distribution (either observed or theoretical), our method allows to obtain a good estimate of the spectrum without the need for considering in detail all the millions of lines contributing to line blanketing. We applied the method to the spectra computed from a sample of photospheric models with effective temperatures Teff = 4200, 5200 and 6200 K, log g = 4.0, 4.5, 5.0 and [A/H] = 0.0, -1.0, -2.0, taken from the NextGen database (Allard & Hauschildt \cite{allardhauschildt:95}). The computed flux distributions agree quite well with the corresponding LTE line-blanketed NextGen fluxes when we introduce the estimated line-opacity contribution as a multiplicative factor of the continuum opacity in the radiative transfer calculations. In particular we discuss the importance of a correct estimate of the continuum flux, mainly in the UV, in the NLTE formation of the Ca Ii H & K, the Ca Ii InfraRed Triplet (IRT: lambda = 8498, 8542, 8662), Na I D, Li I and K I resonance lines.

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