Abstract
We present the first precision UBVRcIc light curves, an initial period study, and a simultaneous light curve solution for the near-contact solar type eclipsing binary V530 And. Our observations were taken with the 0.81 m Lowell reflector on 27 and 29 September, 2011, with time being granted from the National Undergraduate Research Observatory (NURO). Our Wilson Devinney Program solution yields a semidetached, V1010 Oph configuration: the more massive component is filling its Roche lobe. The system is apparently approaching contact for the first time. It is not a classic Algol.
Highlights
HistoryV530 And [2MASS J01274106 + 3351552, NSVS 6447718, TYC 2300-116-1, α(2000) = 01 h 27 m 41.050 s, δ(2000) = +33∘ 51 55.47 ICRS, J = 11.679, H = 11.485, K = 11.421] was discovered by Khruslov (2008) [1]
Their light curve is given as Figure 1
EB binaries are very close together producing distorted curves from tidal and Coriolis forces, but the stars are not in contact, so their light curves still maintain dissimilar eclipse depths. This system was observed as a part of our student/professional collaborative studies of interacting binaries from data taken from NURO observations (National Undergraduate Research Observatory)
Summary
V530 And [2MASS J01274106 + 3351552, NSVS 6447718, TYC 2300-116-1, α(2000) = 01 h 27 m 41.050 s, δ(2000) = +33∘ 51 55.47 ICRS, J = 11.679, H = 11.485, K = 11.421] was discovered by Khruslov (2008) [1]. It was designated as EB with a 12.6–13.3 R-magnitude range (Min II = 13.0) with the ephemeris: J.D. Hel Min I = 2451479.632 d + 0.57723 ⋅ E. V530 And appeared in the 80th namelist of variable stars (IBVS #5969, 2011) EB binaries are very close together producing distorted curves from tidal and Coriolis forces, but the stars are not in contact, so their light curves still maintain dissimilar eclipse depths
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