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.
1. History
V530 And [2MASS J01274106 + 3351552, NSVS 6447718, TYC 2300-116-1, (2000) = 01 h 27 m 41.050 s, (2000) = +33° 51′ 55.47′′ ICRS, , , ] was discovered by Khruslov (2008) [1]. It was designated as EB with a 12.6–13.3 R-magnitude range () with the ephemeris: Their light curve is given as Figure 1.
V530 And was observed by the Robotic Optical Transient Search Experiment [2] and found to have a period = 0.57721 d and a mean unfiltered magnitude of 12.769. A light curve amplitude of 0.633 mag was determined. It was stated that the light curve was calculated to be in the Fourier region where Lyrae (EB) types are expected. Finally, V530 And appeared in the 80th namelist of variable stars (IBVS #5969, 2011). It was also designated as an EB type. 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.
2. Observations
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). Our light curves were taken with the Lowell 0.81 m reflector in Flagstaff with a CRYOTIGER cooled (<−100°C) NASACAM and a CCD chip with standard UBVRcIc filters. Observations were taken on 27 and 29 September, 2011, by Samec, Kring, and Faulkner. The time was awarded by the Lowell TAC as a part of the time allocated from NURO. Analyses were done by Flaaten and Samec. The individual observations included 92 in the -filter, 93 in , 92 in , and 91 in and . The standard error of a single observation was 3 mmag in and , 2 mmag in and , and 4 mmag in . Our observations are given in Table 1, in delta magnitudes, , , , and in the sense of variable minus comparison star.
3. Finding Chart
Our comparison star () was GSC 2300 0035, [(2000) = 01 h 27 m 41.0660 s, (2000) = +33° 51′ 55.298′′ , Guide 9]. The check star () was GSC 2300 0053, [ = , (2000) = +38° 57′′ 24.156′′ , , Guide 9]. We include a finding chart of these stars and the variable () in Figure 2.
4. Period Determination
Two mean times of minimum light were determined from our observations. These include HJD and HJD . We determined 9 more times of low light from the NSVS catalog data set for object number 6447718. We combined this data with Khruslov’s ephemeris to calculate the following new ephemeris (see Table 2 for the calculation): The following is from our Wilson-Devinney program light curve solution:
Each time of minimum light and low light used in the calculation and depicted in Figure 3 is given in Table 2 along with their residuals. Equation (3) is from the programs iterative fit to the light curve data while (2) is a least squares fit to the minima. The NSVS minima are times of low light and carry large uncertainties. We include both ephemerides since they are the best we have at this time.
What we have here is an initial period study. The Wilson programs determination (3) may be better than the one determined from the minima. Further observations, over the course of 10 years or more, are needed to better determine a precision ephemeris and the nature of the period behavior of the system.
5. Light Curves
The light curves were folded , , , , , (), (), and () color curves using (2). They are given in Figures 4(a), 4(b), and 4(c).
(a)
(b)
(c)
Light curve characteristics are given in Table 3. The primary light curve amplitudes of this EB system average 0.8−0.6 mags from to , respectively, and 0.4 mags in the secondary amplitudes. A small O’Connell effect (MAX II-MAX I) [3] of about 1% exists with MAX II being slightly depressed. Thus, we expect some spot activity. The secondary eclipse showed a time of constant light of 41.5 minutes. This means that the eclipses are total and that the more massive, larger star is the hotter component. This is to be expected in normal stellar evolution. We also note that this binary is not one of the common W-type shallow contact types.
6. Synthetic Light Curve Solution
2MASS Photometry yielded a value of ≈0.19. From this, we assumed that the primary component was ~F2 type, with a surface temperature of ≈7000 K [4] so this value was used for the primary components temperature in modeling. The light curves were premodeled with Binary Maker 3.0 [5]. From this work, it was determined that the synthetic light curve fits would be done in Mode 4, semidetached with component one filling its Roche lobe. The parameters resulting from this premodeling were used as starting values for the Wilson-Devinney program [6–9]. The secondary component remained under-filling its Roche lobe throughout the iterations. Adjusted parameters were those with parentheses in Table 4. A simultaneous 5-color synthetic light curve solution was undertaken with the Wilson-Devinney program. No q-search was needed since the curves display total eclipses. A mode 3 solution (contact binary) was also run with much poorer goodness of fit parameters.
7. Discussion
We find that V530 And is a V1010 Oph type near contact binary. The primary, more massive component is filling its Roche lobe and the secondary is under-filling. This means that the binary is likely achieving contact for the first time. The temperature difference () in components is ~500 K. The mass ratio was found to be somewhat extreme, . The potentials are given as s, and the -values are the relative flux from each stars. The values of are the gravity darkening’s, s are the two dimensional limb darkening, and the s are the dimensions of the Roche lobes. The more massive star is filling its Roche lobe with a fillout, , of 100% while the smaller star is just under-filling with a fillout of 99% calculated by potentials. Thus, the state of the star is near contact or has just come into contact. We reason this is true because of the temperature disparity. It is of interest that both surface spots stayed remarkably stable throughout the iterations and are near the points of both stars. There may be some thermodynamic reason why the hemispheres of dark spots are facing each other. The solution is seen overlaying the normalized flux curves shown in Figures 5(a), 5(b), and 5(c). The complete numeric values for the solution are given in Table 4. Four phases, at orbital quadrature’s, of the Roche-lobe model of the binary and for the dark spots, are shown as in Figures 6(a), 6(b), 6(c) and 6(d). Phase zero shows the total eclipse.
(a)
(b)
(c)
(a)
(b)
(c)
(d)
8. Conclusion
Thus, the components are apparently F2V and F5V spectral types. Despite the fairly early spectral types, with the primary star nearly A-type, the presence of the large cool magnetic spots on both stars reveal that they have convective atmospheres and thus would be classified as solar type. It is a near contact, totally eclipsing, binary. Thus, the binary will likely soon come into contact through the process of magnetic braking due to solar type winds leaving the stars along the stiff magnetic field lines [10].
Acknowledgments
The authors thank USC, Lancaster, for their support of thier membership in NURO for the past 8 years, the American Astronomical Society for its support through its former small research program, and the Arizona Space Grant for the partial support for thier student’s travel.