A Preliminary Study Of The EB-type Interacting Eclipsing Binary, NSV 14514

Details A Preliminary Study Of The EB-type Interacting Eclipsing Binary, NSV 14514 A Preliminary Study Of The EB-type Interacting Eclipsing Binary, NSV 14514

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.0301s&link_type=abstract

American Astronomical Society Meeting 210, #03.01; Bulletin of the American Astronomical Society, Vol. 39, p.97

Astronomy and Astrophysics

Astronomy

Scientific paper

We present preliminary light curve analyses of the EB binary, NSV 14514 from 2006 NURO (Lowell Observatory) and SARA CCD observations using UBVRcIc filters. About 400 observations were taken in each of the B,V,R,I as well as 37 in U.
NSV 14514 [GSC 2764 1417, α(2000)=23h 20m 13.8s, δ(2000)=+37° 08’ 39.84"] was rediscovered by ROTSE (IBVS #5699 2006). The ROTSEI ephemeris is HJD Tmin I = 2451446.889 + 0.406095 d. Its light curves suggest contact, but its difference in amplitudes, 0.98 and 0.35 magnitudes in V, indicate a semidetached configuration. Strong distortions are apparently induced by intense spots.
Six mean epochs of minimum light were computed: HJDMinI = 2454001.7158 (±0.0006) and 2454004.9645 (±0.0005), 2454005.7770 (±0.0008), and HJDMinII = 2454001.9189 (±0.0006), 2454004.7605 (±0.0067), 2454006.7926 (±0.0006). A linear ephemeris was calculated using all available material:
HJD Tmin I = 2454001.7158(± 0.0115) + 0.4060990(± 0.0000047) d*E.
Using our minima only, we obtained,
HJD Tmin I = 24 54001.71563(± 0 .00027) + 0.406118(± 0.000034) d*E.
The period behavior of the system is presently unclear.
A Wilson Code BVRI contact solution was calculated. The mass ratio, M2/M1, is 0.66, and temperature difference T1-T2 is 1300 K. The inclination and fill-out is 78° and 17.5%. The super luminous region was found in the neck of the Roche Lobe of the secondary component with a T-factor, 1.5, indicating a vigorous mass transfer. A cool (magnetic) spot of 10° in radius was modeled on the primary, more massive component. Its colatitude is 70° and its temperature is 0.33 times that of the photosphere. The spots are unusual for a contact binary. In addition, both Algol and V1010 Oph type solutions are being modeled.
Acknowledgements: We wish to thank NASA and the American Astronomical Society for their continued support of our undergraduate research programs through their small research grants.

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