Absolute Parameters for the Very Young, Hot Eclipsing Binary V684 Mon in NGC 2264

Details Absolute Parameters for the Very Young, Hot Eclipsing Binary V684 Mon in NGC 2264 Absolute Parameters for the Very Young, Hot Eclipsing Binary V684 Mon in NGC 2264

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.0302b&link_type=abstract

American Astronomical Society Meeting 210, #03.02; Bulletin of the American Astronomical Society, Vol. 39, p.98

Astronomy and Astrophysics

Astronomy

2

Scientific paper

V684 Mon (HD 47755, W74, vM37, VSB52) is a young, hot (B5V, B5V; V = +8.57) close eclipsing binary (P = 1.851 d) in the open cluster NGC 2264 (cluster age 3-4 Myr). Walker (1956) noted that this star exhibited double lines, but no published radial velocity curve exists. Koch et al. (1986) discovered that the system eclipsed, but the system was observed over a limited timescale, obtaining only one minimum with enough coverage to generate a reliable timing. Because of the potential for investigating a very young pair of main sequence B-stars in a cluster of known age, this star was put on the observing program at the Bradstreet Observatory at Eastern University and a preliminary light curve analysis was given by Bradstreet et al. (1999). Since 1999 we have been photometrically monitoring V684 Mon in order to obtain times of minimum light as well as to investigate previously observed light curve subtleties which suggested a slightly eccentric orbit and intrinsic variability. 49 spectra of V684 Mon were obtained using the 1.0-m telescope at Mt. Laguna Observatory in 2002 and the system has been confirmed to be double-lined. New precision BVR light curves have been obtained in 2007 using a 40-cm telescope and a SBIG ST10-XME CCD camera. The observations, times of minimum light, period analysis, and light and radial velocity curve analyses using the Wilson-Devinney code yielding absolute parameters for the two stars will be presented. We will discuss the evidence for cluster membership for the system and compare the physical characteristics of the two B-stars with theoretical predictions.

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