Photometric Investigation of the Critical Contact Systems, GSC 3355 0394 and NSV 1719

Details Photometric Investigation of the Critical Contact Systems, GSC 3355 0394 and NSV 1719 Photometric Investigation of the Critical Contact Systems, GSC 3355 0394 and NSV 1719

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541927s&link_type=abstract

American Astronomical Society, AAS Meeting #215, #419.27; Bulletin of the American Astronomical Society, Vol. 42, p.280

Astronomy and Astrophysics

Astronomy

Scientific paper

Here we present the first BVRI precision light curves and analyses of the critical contact binaries, GSC 3355 0395 and NSV1719.
GSC 3355 0394 has an EB type light curve which is dominated by hot and cool spot activity. It displays night to night variations in light curve shapes.
The period study yields 6 new times of minimum light, HJD I = 2454408.9555 (±0.0012)d, 2454427.9001 (±0.0005)d, 2454829.9867 (±0.0023)d, 2454849.85215 (±0.00056)d, HJD II= 2454829.7566 (±0.0004)d, 2454849.6213 (±0.0035)d, and the first precision ephemeris, HJD Tmin I = 2454408.9547 ± 0.0017 + 0. 4621603 ± 0. 0000008 d*E.
Standard magnitudes indicate that both variables are of K2±2V type. BVRI Wilson synthetic light curve solutions are calculated. The critical contact is the best solution. Four major spot regions were determined, including a stream spot.
We also present the first precision observations of the recently discovered, high amplitude W UMa system, NSV 1719. The curves are of EW type, and they display night to night variations in light curve shapes.
Eight times of minimum light were determined: HJD I = 2458422.8085 (±0.0001)d, 2458423.6797 (±0.0005)d, 2458425.7114 (±0.0003)d, and 2458428.9056 (±0.0005)d. HJD II= 2458422.6634 (±0.0001)d, 2458423.8241 (±0.0003)d , 2458425.8563 (±0.0003)d, and 2458428.7591 (±0.0021)d, and the first precision ephemeris was determined:
HJD Tmin I = 2458425.7115 ± 0.0008 + 0.29030944 ± 0.00000012 d*E
Our best solution reveals NSV 1719 to be a spotted, solar type binary with similar masses (m1/m2 0.7) and a very shallow contact solution, f = 3±1%. So, we find NSV 1719 is near critical contact. Surprisingly, it has already achieved a W-type configuration.
We wish to thank NURO and SARA for their telescope time and the American Astronomical Society for their support through Small Research Grants. We also thank the Arizona Space Grant for travel support for our students.

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