The 7.5 Magnitude Limit Sample of Bright Short-Period Binary Stars. I. How Many Contact Binaries Are There?

Details The 7.5 Magnitude Limit Sample of Bright Short-Period Binary Stars. I. How Many Contact Binaries Are There? The 7.5 Magnitude Limit Sample of Bright Short-Period Binary Stars. I. How Many Contact Binaries Are There?

2002-07-05

arxiv.org/abs/astro-ph/0207144v1

Astronomy and Astrophysics

Astrophysics

AASTeX5, 11 figures, 3 tables. Table 1 is very wide; in case of problems send e-mail to rucinski@astro.utoronto.ca for a raw t

Scientific paper

10.1086/342677

A sample of bright contact binary stars (W UMa-type or EW, and related: with beta Lyr light curves, EB, and ellipsoidal, ELL - in effect, all but the detached, EA), to the limit of Vmax = 7.5 magnitude is deemed to include all discoverable short-period (P<1 days) binaries with photometric variation larger than about 0.05 magnitude. Of the 32 systems in the final sample, 11 systems have been discovered by the Hipparcos satellite. The combined spatial density is evaluated at (1.02+/-0.24)x10^-5 pc^-3. The Relative Frequency of Occurrence (RFO), defined in relation to the Main Sequence stars, depends on the luminosity. An assumption of RFO~1/500 for MV>+1.5 is consistent with the data, although the number statistics is poor with the resulting uncertainty in the spatial density and the RFO by a factor of about two. The RFO rapidly decreases for brighter binaries to a level of 1/5,000 for MV<+1.5 and to 1/30,000 for MV<+0.5. The high RFO of 1/130, previously determined from the deep OGLE-I sample of Disk Population W UMa-type systems towards Baade's Window, is inconsistent with and unconfirmed by the new results. Possible reasons for the large discrepancy are discussed. They include several observational effects, but also a possibility of a genuine increase in the contact-binary density in the central parts of the Galaxy.

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