Hostname: page-component-78c5997874-lj6df Total loading time: 0 Render date: 2024-11-05T14:45:11.806Z Has data issue: false hasContentIssue false

Stellar model atmospheres with magnetic line blanketing

Published online by Cambridge University Press:  02 March 2005

S. Khan
Affiliation:
Tavrian National University, Yaltinskaya 4, 95007 Simferopol, Crimea, Ukraine email: [email protected], [email protected] Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, 1180 Wien, Austria email: [email protected]
O. Kochukhov
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, 1180 Wien, Austria email: [email protected]
D. Shulyak
Affiliation:
Tavrian National University, Yaltinskaya 4, 95007 Simferopol, Crimea, Ukraine email: [email protected], [email protected] Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, 1180 Wien, Austria email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Model atmospheres of A and B stars are computed taking into account magnetic line blanketing. These calculations are based on the new stellar model atmosphere code LLMODELS which implements a direct treatment of the line opacities and ensures an accurate and detailed description of the line absorption. The anomalous Zeeman effect was calculated for field strengths between 1 and 40kG and a field vector perpendicular to the line of sight. The magnetically enhanced line blanketing changes the atmospheric structure and leads to a redistribution of energy in the stellar spectrum. The most noticeable feature in the optical region is the appearance of the $\lambda$5200 broad, continuum feature. However, this effect is prominent only in cool A stars and disappears for higher effective temperatures. The presence of a magnetic field produces an opposite variation of the flux distribution in the optical and the UV regions. A deficiency of the UV flux is found for the whole range of considered effective temperatures, whereas the “null wavelength region” where the flux remains unchanged shifts towards the bluer wavelengths for higher temperatures.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Copyright
© 2004 International Astronomical Union