Analysis of 2007 UBVRcIc Observations of the Totally Eclipsing, Extreme Mass Ratio Binary, GSC 1283 0053

Details Analysis of 2007 UBVRcIc Observations of the Totally Eclipsing, Extreme Mass Ratio Binary, GSC 1283 0053 Analysis of 2007 UBVRcIc Observations of the Totally Eclipsing, Extreme Mass Ratio Binary, GSC 1283 0053

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.1404s&link_type=abstract

American Astronomical Society, AAS Meeting #212, #14.04; Bulletin of the American Astronomical Society, Vol. 40, p.208

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We present a UBVRcIc analyses of a recently discovered (ROTSE-I, AJ 131, 623, 2006) totally eclipsing, extreme mass ratio eclipsing binary, GSC 1283 0053 from observations taken with the 0.81-m Lowell Reflector with NURO granted time on December 26,29,30 and 31, 2007. Light curves, a period study and a light curve solution is presented.
The light curves were premodeled with Binary 3.0 and then solved with the 2004 version Wilson code. We obtained 269 U, 271 B, 183 V, 269 R and 272 I individual CCD observations with the 2K X 2K NASACAM. Standard star and comp star observations suggest the primary component is spectral type G6.5V (5450 K).
Four mean times of minimum light were determined: HJDMin I= 2454464.8998 (±0.0005)d, 2454465.8577 (±0.0008)d, 2454466.8142 (±0.0005)d, and HJDMin II=2454465.6656 (±0.0002)d. The following linear ephemeris was calculated from these and previous timings:
HJD Min I =2454464.8997 (±0.0006)d + 0. 3830009 (±0.0000007)*E (1)
Not enough data is presently available to determine the nature of the period variation. We suspect that the period is decreasing due to stellar winds and resulting magnetic breaking.
GSC 1283 0053 is an W-type contact binary (the less massive component is the hotter) with a 0.45 mag amplitude in U. The system parameters from the Wilson Code include a mass ratio of only 0.20, a slight temperature difference of 150 K and an inclination of 78.9o. Two magnetic spots were modeled on the primary, more massive component with colatitudes of 120o and 104o, longitudes of 76 o and 283 o, radii of 18 degrees each and with a T-factor of 0.87 and 0.90, respectively.
We wish to thank the American Astronomical Society and its small research grant program for supporting this research.

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