The Balmer Decrement in Be Stars

Details The Balmer Decrement in Be Stars The Balmer Decrement in Be Stars

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21934420a&link_type=abstract

American Astronomical Society, AAS Meeting #219, #344.20

Astronomy and Astrophysics

Astronomy

Scientific paper

Classical Be stars are non-supergiant B stars that have exhibited emission in their photospheric lines generated by a circumstellar disk formed by material ejected from the stellar surface. In order to investigate the relationship between observed emission in the H Balmer lines and the physical properties of the disks, we present optical spectra of Be/XRBs, cluster, and field Be stars covering Hα through Hδ. We use Hα emission to determine disk presence and strength. We then search for correlations in the profiles of Hβ through Hδ with Hα strength and the star's environment (binary vs. cluster member vs. field). To compliment these observations, we are developing models to examine the effects of disk temperature, density, radius, and inclination angle on the shape of the line profile. We assume a steady state, geometrically thin disk rotating with Keplerian motion. Our goal is to combine these disk models with available TLUSTY NLTE models of B star atmospheres to accurately reproduce our observations.
We are grateful for support from NSF grant AST-1109247, NOAO student support, and Lehigh University.

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