Stellar model atmospheres with magnetic line blanketing

Details Stellar model atmospheres with magnetic line blanketing Stellar model atmospheres with magnetic line blanketing

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..224...29k&link_type=abstract

The A-Star Puzzle, held in Poprad, Slovakia, July 8-13, 2004. Edited by J. Zverko, J. Ziznovsky, S.J. Adelman, and W.W. Weiss,

Computer Science

4

Stars: Chemically Peculiar, Stars: Magnetic Fields, Stars: Atmospheres.

Scientific paper

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 λ5200 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.

Affiliated with

Also associated with

No associations

Rating

Stellar model atmospheres with magnetic line blanketing does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Stellar model atmospheres with magnetic line blanketing, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Stellar model atmospheres with magnetic line blanketing will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1083035