A Hidden Population of Hot Subdwarf Stars in Close Binaries

Details A Hidden Population of Hot Subdwarf Stars in Close Binaries A Hidden Population of Hot Subdwarf Stars in Close Binaries

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1314...73w&link_type=abstract

INTERNATIONAL CONFERENCE ON BINARIES: In celebration of Ron Webbink's 65th Birthday. AIP Conference Proceedings, Volume 1314, p

Statistics

Methodology

2

Dwarf Stars, Galaxies, Brightness, Spectroscopy, Giant And Subgiant Stars, Spiral Arms And Galactic Disk, Magnitudes And Colors, Luminosities, Spectroscopy And Spectrophotometry

Scientific paper

Observations to date preferentially find Galactic hot subdwarf (sdB/sdO) stars in binaries when the subdwarfs are more luminous than their relatively faint companions (G/K/M dwarfs, white dwarfs). As suggested by Han et al. [1], this selection bias may distort our perspective of the evolutionary channels that form hot subdwarfs in the galactic disk. A predicted and possibly more numerous population of binaries features a lower-mass, lower-luminosity, longer-lived hot subdwarf hiding in the glare from its companion: the subdwarf+A/early F binaries. Such systems may arise when mass transfer is initiated in the Hertzsprung gap; the A/F companion in some cases was ``created'' from a lower-mass star (i.e., it would be a blue straggler if seen in a cluster).
A survey is underway at Penn State to identify hot subdwarfs paired with F stars, determine their properties, and establish their space density. The project makes use of ground and space archival data to identify these systems (from their UV excesses) and new spectroscopic observations to determine their orbital periods and other properties. Successful characterization of this group of close binaries should help to challenge, calibrate, or refine models of binary star evolution that are used in population synthesis studies, including the relative importance of the RLOF and common-envelope channels for the formation of hot subdwarfs. The motivation, methodology, and status of this search for hidden hot subdwarfs are presented in this contribution.

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