Quantitative Analysis of the Spectra of Early B Stars with Ultrasharp Lines

Details Quantitative Analysis of the Spectra of Early B Stars with Ultrasharp Lines Quantitative Analysis of the Spectra of Early B Stars with Ultrasharp Lines

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21460512p&link_type=abstract

American Astronomical Society, AAS Meeting #214, #605.12

Statistics

Computation

Scientific paper

The extent to which contemporary NLTE and LTE models represent the atmospheres of the early B stars with the sharpest lines is discussed. Due to the low rotational broadening in these stars, line blending presents minimal problems and the intrinsic line profiles are revealed. Spectral data from the HST and FUSE spacecraft and the KPNO Coude Feed Telescope are compared with computations from the Hubeny/Lanz codes TLUSTY/SYNSPEC and the Kurucz code SYNTHE. The B stars include ι Her (B3V), HR 1886 (B1V), HR 1887 (B0.5V), and AV 304 (B0.5V) in the SMC, all of which are considered to be abundance standards. Contemporary NLTE model atmospheres represent the photospheres of early B stars remarkably well. Some lines are fit much better in NLTE even for the B3 stars, but widespread discrepancies seem to emerge for stars hotter than B0.5, which also show dynamic atmospheres. Future work need to be done on the following: 1) The determination and meaning of microturbulence and its effect on the atmosphere, 2) Further attention to the strong Si II lines, especially Multiplet 4, 3) Treatment of Ti, V, Cr, Mn, Co, and Ni in NLTE, 4) Wind models for B0-B0.5 stars.
The authors appreciate support from NASA grants NAG5-11802, NAG5-12239, NAG5-13212, and STScI grants GO-09848 & GO-06709.

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