New light curve solution of V568 Peg and first determination of its fundamental parameters

New light curve solution of V568 Peg and first determination of its fundamental parameters

Diana Kjurkchieva and Sunay Ibryamov Department of Physics and Astronomy, Shumen University, 115 Universitetska, 9700 Shumen, Bulgaria
; 11email: s.ibryamov@shu.bg; d.kyurkchieva@shu.bg Department of Physics and Astronomy, Shumen University, 115 Universitetska, 9700 Shumen, Bulgaria
; 11email: s.ibryamov@shu.bg; d.kyurkchieva@shu.bg
Abstract

We present photometric observations of the short-period W UMa star V568 Peg. They allowed us to improve its period. The light curve solution revealed that V568 Peg is an overcontact binary of A subtype with moderate fill-out factor. Its components are K stars which undergo partial eclipses. The mass ratio was estimated by -search analysis. We established existing of big cool spot on the primary component with almost the same parameters during the last 4 years. Based on our light curve solution and the GAIA distance we calculated at the first time the masses, radii and luminosities of the components of V568 Peg.

binaries: close – binaries: eclipsing – methods: data analysis – stars: fundamental parameters – stars: individual (V568 Peg)
\tocauthor

D. Kjurkchieva \papertypeSubmitted on xx.xx.xxxx; Accepted on xx.xx.xxxx

1. Introduction

The temperature difference of the components of W UMa binaries usually are around 100–300 K (only those of B subtype systems are above 1000 K) while their masses and radii may differ considerably (Binnendijk 1965, Lucy Wilson 1979, Csizmadia Klagyivik 2004). The model of Lucy (1968a, 1968b) explained this effect by a common convective photosphere which embedded two stars near or just above the Main Sequence. However, until now there is not a satisfactory explanation of the mechanism of energy transfer, the W phenomenon (the hotter component is the smaller star) and the internal structure of the W UMa binaries. Their future fate is also debatable issue: tight binary or merger (van Hamme 1982a,b; Li et al. 2007). The solutions of these problems requires rich statistics of well-determined global parameters of W UMa stars. The GAIA distances (Bailer-Jones et al. 2018) of a huge number of eclipsing binaries provide invaluable possibility for precise determination of their global parameters on the base of ground-based observations.

This paper presents photometric observations of the short-period W UMa-type system V568 Peg. It was observed 4 years ago in Sloan bands (Kjurkchieva et al. 2015, further on Paper I). The main goal of the new observations was to determine its fundamental parameters by the light curve solution and GAIA distance. This is the first study based on observations by the 10-inch Schmidt-Cassegrain telescope MEADE LX80 SC of the Shumen Astronomical Observatory.

2. Observations

The photometric observations of the target were carried out on Aug 13 2018. We used CCD camera SBIG ST-10XME (2184 1472 pixels, 6.8 m/pixel). Focal reducer TS Optics f/6.3 provides increasing of the field of view from 20 14 arcmin with resolution 0.55 arcsec/pix to 32 22 arcmin with resolution 0.88 arcsec/pix (Kjurkchieva et al. 2018). The exposures in and filter were 90 s and 60 s and the mean photometric precision was 0.029 mag in both filters.

The photometric data were reduced by MaxIm DL 5. An aperture photometry was performed using four standard stars (Table 1) in the observed field whose coordinates were taken from the catalogue 2MASS (Skrutskie et al. 2006) while their magnitudes were from the NOMAD catalog (Zacharias et al. 2004).

The reduced data are accessible in the form of table as online supplemental data and at http://astro.shu.bg/V568Peg/.

Label 2MASS ID RA Dec
V V568 Peg 23 08 13.01 +33 03 03.77 12.960 12.550
C1 23081802+3259237 23 08 18.03 +32 59 23.70 11.361 10.590
C2 23080030+3306284 23 08 00.30 +33 06 28.41 13.770 13.420
C3 23074178+3307567 23 07 41.79 +33 07 56.75 11.534 10.650
C4 23075759+3302504 23 07 57.60 +33 02 50.41 12.130 11.620
Table 1: Coordinates and magnitudes of the target (V) and comparison (C) stars

3. Light curve solution

We carried out the modeling of our data by the package PHOEBE svn (Prsa Zwitter 2005). The observational data (Fig. 1) show that our target is an overcontact system and we modelled them using the corresponding mode ’’Overcontact binary not in thermal contact’’.

The values of target (weighting) temperature = determined by different ways are slightly different: = 5100 K is the value from the dereddened index and relation of Sekiguchi Fukugita (2000); = 5000 K is the value from the dereddened index and relation of Covey et al. (2007); = 4850 K is the value from the 2MASS dereddened index and relation of Cox (2000); = 4800 K is the value determined by GAIA DR2 (Gaia Collaboration 2018). The different values of target temperature may due at least partially to the different phases of measurement of the color indices ( should be determined by measurements at quadratures).

The interstellar reddening was estimated based on the following considerations. The extinction in the V568 Peg direction is 0.221 mag according to the NED database (Schlafly Finkbeiner 2011) and 0.134 mag according to the 3D model of Arenou et al. (1992) for distance 253 pc (see Section 4). The extinction values of NED refer to distance above 500–600 pc while the distance to V568 Peg is considerably smaller. It was reasonable to reduce the extinction in all colors of the NED database by the same factor 0.61(=0.134/0.221) as in . This rule was used for estimation of all dereddened indices.

Unfortunately, there were not spectra of V568 Peg for confident temperature determination. This problem may be overcame by low-dispersion spectral observations (for instance by future low-dispersion spectrograph of the 2-m telescope at NAO Rozhen). In our case = 4900 K was adopted as some average value of the values determined by different ways.

We fixed the primary temperature = and searched for best fit varying initial epoch , secondary temperature , mass ratio , inclination and potential . Coefficients of gravity brightening 0.32 and reflection effect 0.5 appropriate for late stars were assumed. We used linear limb-darkening law whose coefficients were interpolated (depending on stellar temperatures and filters) according to the tables of Van Hamme (1993). In order to reproduce the O’Connell effect of around 0.065 mag (Fig. 1) we put a cool spot on the primary and varied its parameters (longitude , latitude , angular size and temperature factor ).

The mass ratio determination of the partially-eclipsed binary V568 Peg required -search analysis. For this aim we varied the mass ratio in a wide interval, from 0.1 to 10.0. The -search curve (Fig. 2) exhibits two minima. The first one at = 0.4 is deeper and narrower while the second one at = 4 is shallower and wider. The value for = 4 is around 3 times bigger than that for = 0.4. We carried out detailed investigation of the solution around = 4 by varying of all parameters but reached inconsiderable decreasing of (by several ). That is why we chose as input value = 0.4. Radial velocity measurements could provide confirmation of our choice although the spectral lines of the W UMa stars are broadened and blended that leads to low-precise determination of the spectral mass ratio (Frasca 2000, Bilir et al. 2005, Dall & Schmidtobreick 2005). Unfortunately, V568 Peg is too faint for radial velocity measurements based on spectral observations by the 2-m telescope at NAO Rozhen.

After reaching the best light curve solution we adjusted the stellar temperatures and around the value by the formulae (Kjurkchieva Vasileva 2015)

(1)

where the quantities (the ratio of the relative luminosities of the stellar components) and are determined from the PHOEBE solution. In fact, formulae (1) are consequence of the definition given earlier.

Last fitting procedure was carried out for fixed and to obtain the final and self-consistent solution.

Figure 1: Top: the folded light curves of V568 Peg and their fits; Bottom: the corresponding residuals (shifted vertically to save space)
Figure 2: -search curve

PHOEBE gives as output parameters the relative (volume) radius of each component ( is linear radius and a is orbital separation). One can determine the luminosity ratio from the PHOEBE output parameter . The output potentials and allowed to calculate the target fill-out factor .

We estimated the precision of the fitted parameters by the procedure described in Dimitrov et al. (2017).

Table 2 contains the final values of the fitted stellar and spot parameters and their uncertainties. Table 3 exhibits the calculated parameters: , and . Their errors are determined from the uncertainties of fitted parameters. The synthetic curves corresponding to the parameters of our light curve solution are shown in Fig. 1 as continuous lines while Fig. 3 exhibits the 3D configuration of V568 Peg.

- 2450000 source
[d] [] [K] [K] [] [] []
6925.380188(24) 0.247095(1) 76.3(1) 0.494(1) 5734(48) 5409(17) 2.786(2) 70(1) 75(1) 22.0(2) 0.85(1) Paper I
6925.533810(14) 0.247095(2) 75.6(1) 0.403(3) 4963(30) 4713(23) 2.6343(1) 70(1) 75(1) 20.5(2) 0.88(1) this paper
Table 2: Fitted parameters of the best light curve solution
source
0.462(6) 0.340(4) 0.265 0.35 Paper I
0.475(6) 0.317(9) 0.204 0.36 this paper
Table 3: Calculated parameters
Figure 3: 3D configuration of V568 Peg made using Binary Maker 3 by Bradstreet and Steelman (2002).
Figure 4: O-C diagram of V568 Peg: the three clusters of points correspond to WASP data while the last two points to our two solutions

4. Global parameters of V568 Peg

The GAIA distance of V568 Peg is 253 pc (Bailer-Jones et al. 2018). It allowed us to calculate the target global parameters by the following procedure.

(a) We obtained the target absolute magnitude = 5.884 mag by the formula of distance modulus using its visual magnitude = 12.81 mag at quadrature (the extinction =0.134 was estimated according to Arenou et al. (1992)).

(b) The bolometric magnitude = 5.794 mag was calculated from and the bolometric correction BC = -0.36 mag (Masana et al. 2006) corresponding to temperature 4900 K.

(c) The total luminosity = 0.537 L was obtained from .

(d) The individual luminosities = 0.394 L and = 0.143 L were calculated by and ratio = 0.36 from the PHOEBE solution.

(e) The component radii = 0.851 R and = 0.569 R were determined from the individual luminosities and temperatures (Table 2).

(f) The orbital axis = 1.796 R was calculated from the absolute radii and relative stellar radii (Table 3).

(g) The total mass = 1.272 M was determined by the third Kepler law based on the orbital axis and target period .

(k) The individual mases = 0.907 M and = 0.365 M were obtained from and the mass ratio (Table 2).

5. Analysis of the results

The comparison of the parameter values of the new solution (Tables 2–3) with the previous one (Paper I) led to the following results.

(1) The difference in inclination is negligible.

(2) There is small difference in relative component radii (1.5 for the primary radius and 7 for the secondary radius).

(3) The temperature differences of the components are close while the component temperatures themselves differ by around 700 K (Table 2). This is an illustration of the known fact that the light curve solution is strongly sensitive to but not to the individual temperatures. Thus, the two solutions could be considered as similar in temperature parameters. This is supported by almost the same luminosity ratios of the two solutions (Table 3). We assume that the new solution is more confident due to the determination of its value by several dereddened color indices.

(4) The values of the mass ratio differ by 18 . We attributed the difference to using of third light (of around 0.065) in the previous solution (Paper I) because the new data can be well-reproduced by the parameters of old solution including the the same third light value. But we assume that the new solution is more reasonable because it does not require an art third light (invisible around the target). Moreover, the new value is more confident because it is obtained by detailed -search analysis.

(5) The biggest difference of the two solutions is the value of the initial epoch (Table 2). It implies shorter period than the known value. To check this supposition we determined times of light minima of SWASP data (Butters et al. 2010). From the O–C diagram (Fig. 4) we derived the period value of 0.24708000.0000003 d.

(6) The closeness of the spot positions and spot parameters of the two solutions (Table 2) means existing of stable large cool spot on the primary component during the last 4 years, i.e. during around 5740 cycles.

6. Conclusion

Our observations of V568 Peg revealed that the target is an overcontact binary of A subtype with moderate fill-out factor. Its components are K stars which undergo partial eclipses. The new data allowed us to improve the target period while the GAIA distance provided a possibility to calculate the masses, radii and luminosities of its components.

Acknowledgments

The research was supported partly by projects DN08/20 and DM08/02 of Scientific Foundation of the Bulgarian Ministry of Education and Science, project D01-157/28.08.2018 of the Bulgarian Ministry of Education and science, as well as by projects RD-08-142 and RD-08-112/2018 of Shumen University.

The authors are very grateful to the anonymous Referee for the valuable notes and recommendations.

This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

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