UBVRI Observations And Analysis Of The Solar Type, Total Eclipsing Binary, TYC 3034-299-1

Details UBVRI Observations And Analysis Of The Solar Type, Total Eclipsing Binary, TYC 3034-299-1 UBVRI Observations And Analysis Of The Solar Type, Total Eclipsing Binary, TYC 3034-299-1

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21915327f&link_type=abstract

American Astronomical Society, AAS Meeting #219, #153.27

Astronomy and Astrophysics

Astronomy

Scientific paper

TYC 3034-299-1 (CVn) is a magnetically active, solar type contact binary and a ROTSE variable. This system was observed as a part of our continuing student/professional collaborative study of interacting binaries. The current UBVRI light curves were taken with the Lowell 0.81-m reflector in Flagstaff on May 10 and May 11, 2010. Four times of minimum light were determined from our observations. They include (with standard errors):
HJD I = 2455326.72754±0.00024, 2455327.713303±0.00025,
HJD II = 2455326.92427±0.00068, 2455327.91256±0.00060.
We also obtained the following timings of minimum light from parabolic fits to the data of Blattler (IBVS number 5699, 2006):
HJD I = 2453382.6915, 2453445.4980, 2453502.3800, 2453515.4154, 2453517.3907,
HJD II = 2453463.4719, 2453515.607.
From these and Nelson's (IBVS numbers 5875 and 5929, 2009) observations, an improved ephemeris was calculated from all the available eclipse timings:
J.D. Hel Min I = 2455326.9244±0.0005 + 0.39500870 ± 0.00000016 d*E.
Our light curve amplitudes are deep for a contact binary, ranging from 0.85 magnitude in U to 0.66 in I. Time of totality of 7 minutes was detected in the secondary eclipse indicating that this system is a W-type W UMa system (less massive star is hotter). The O'Connell effect ranges from 67 mmag to 36 mmag in U to I, respectively, revealing substantial magnetic activity.
A 5-color simultaneous light curve solution was calculated using the Wilson Code. Our model reveals a dark spot region at longitude 58°. The 18% fill-out and the virtually identical temperatures of the two stars show that the system has nearly reached thermal contact. We performed a q-search over the interval from q = 0.3 to 0.8. The mass ratio is 0.46.
We wish to thank Lowell Observatory for their allocation of observing time and the American Astronomical Society and the Arizona Space Grant for travel support for this observing run.

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