1. INTRODUCTION

CW Cep is a well-known apsidal motion binary system observed by many investigators (Abrami & Cester 1960; Nha 1975; Han et al. 2002; Wolf et al. 2006) since its discovery by Petrie (1947) as a double lined spectroscopic eclipsing binary. The spectral types of two components of CW Cep were determined as B0.5 + B0.5, and masses were calculated as 11.7 M⊙ and 11.0 M⊙ by Popper (1974). The light curves were analyzed by many authors using well observed full-light curves with different models for the parameters of the binary system, related with its apsidal motion (Cester et al. 1978) with the WINK model, Clausen & Giménez (1991) by the EBOP model, and Terrell (1991), and Han et al. (2002) by the WD model. While Popper & Hill (1991) discussed the radial velocity curve based on the spectroscopic observations by Popper (1974), high resolution IUE observations for the radial velocity curve were made by Stickland et al. (1992). Most of these studies suggested that CW Cep is a detached main sequence binary system, composed of two stars of slightly different mass and radius.

With regard to the apsidal motion study of the close eclipsing binary systems, CW Cep showed one of the shortest apsidal period, among similar binary systems, which leads particular interests for this binary system. Based on intensive photoelectric observations with UBV filters, Nha (1975) calculated the apsidal motion period of CW Cep as 39 years, while Han (1984) derived the apsidal motion period as 43.1 years with more times of minimum lights based on the UBV photoelectric observations. After their studies, more times of minimum lights were available by many investigators recently, according to the new observations. Therefore, the apsidal motion period of CW Cep was improved in time order as 45.5 years by Gimenez et al. (1987), 45.6 years by Clausen & Giménez (1991), and 45.7 years by Han et al. (2002). The last authors, for the first time, noticed a new type of complication confusing the apsidal motion behavior, which shows about 34 years periodic variation with an amplitude of 0.003 days. Erdem et al. (2004) calculated the apsidal motion period of CW Cep as 46.1 years through the variation of the longitude of periastron (ω) of the system's orbit, with new observations using BVR filters. More recently, with new observations by Wolf et al. (2006), they suggested the apsidal motion period of CW Cep as 46 years, which is similar to those of other previous authors (Clausen & Giménez 1991; Han et al. 2002). They confirmed an extra periodic change suggested by Han et al. (2002) and proposed a Light Time Effect (LTE) with the period of 38.5 years and the small semi-amplitude of 0.002 days caused by an unseen third body.

It is nearly 10 years since the observations by Wolf et al. (2006), and this indicates the necessity of new observations for this binary system to examine more accurate apsidal motion period. In line with this, we made new observations for CW Cep in the 2015 season and obtained three new times of minimum lights to confirm the apsidal motion period of this system, together with available minimum times from the published literatures.

2. NEW OBSERVATIONS

New CCD photometric observations presented in this work were made in the 2015 observational season at the Jincheon station of Chungbuk National University Observatory (CBNUOJ), Korea. The altitude of the Jincheon station is 87 m sea level and the 60-cm reflecting telescope is installed by Korea Astronomy and Space Science Institute (KASI), and operated by CBNUOJ. An electronically cooled SBIG STX- 16803 4K CCD camera is equipped with a Johnson standard BVRI filter set, and is attached at the reflector f/2.9 prime focus of the 60 cm wide field telescope. Since our observations are focused on the acquisition of accurate eclipse timings, only B filter is used for fast time-resolved photometry for the first two nights. The observations of the last night were made with BVR filters to derive the weighted average of each filters for higher accuracy. The field of view of the CCD camera is 72’ × 72’ with a pixel scale of 1.05 arcsec/pixel, which is wide enough to cover the many field stars around CW Cep including the comparison star GSC 04282-00330, and differential photometry was applied for this observation. All of the observed CCD frames were exposed 15 ~ 80 seconds depending on the observational circumstances, and corrected with bias, dark and flat-field images for the differential photometry. The IRAF/DIPHO software package was applied to process the observed CCD frames. The details of the data reduction were extensively described by Kim et al. (2014) based on the same observational circumstances. We obtained three times of minimum lights, two for primary and one secondary minima, and determined the times of minimum lights by conventional Kwee & van Woerden (1956) method as listed in Table 1 together with other times of minima determined by previous investigators.

Table 1.1) PE: Photoelectric photometry, CCD photometry 2) CBNUOJ : Chungbuk National University Observatory at Jincheon

3. MINIMUM LIGHTS AND O-C DIAGRAM

With our new times of minimum lights of CW Cep, we collected all published times of minimum lights from the literature to analyze the apsidal motion of this binary system. Among the available times of minimum lights, the visual and photographic data observed at the early stage of apsidal motion were excluded in this study because those data could increase uncertainty of period variations. Only photoelectric and CCD times of minimum lights were used in our analysis and listed in Table 1, including our timings.

These times of minima were simultaneously analyzed with the apsidal motion plus the light-time effect ephemeris represented by:

where Ps is the sidereal period, τap and τ3 denote the apsidal motion and the LTE terms, respectively. τap is a function of four parameters (anomalous period Pa, eccentricity e, longitude of the periastron ω0, angular velocity of the line of apsides ) The formalism for τ3 was given up to sixth power of the eccentricity Giménez & Bastero (1995). Irwin (1952) gave an exact form for τ3 with five unknown parameters which are the semi-amplitude K, the eccentricity e3, the period P3, the periastron passage time T3, the longitude of periastron ω3 for the light orbit of mass center of the eclipsing pair around the mass center of the triple system.

All the timings were fitted to Eq. (1) by using the code (available at http://sirrah.troja.mff.cuni.cz/~zasche/Programs.html) given by Zasche et al. (2009) and Zasche & Wolf (2013). We made small corrections of the code by considering the inclination of the eclipsing pair in it involving up to sixth power of the eccentricity. With the initial values of the apsidal motion and LTE parameter given by Wolf et al. (2006), we improved iteratively the apsidal motion and LTE parameters. the calculation we fixed the inclination of the eclipsing pair as 82.5° derived by Clausen & Giménez (1991) and Han et al. (2002). The final solution was listed in the sixth column of Table 2, together with those et al. (2002), Wolf et al. (2006) and Bulut et al. (2011) for comparison. The resultant O-C diagram was drawn with the linear term of our result in the top of Fig. 1 where the solid continuous curves denote the combination of τap and τ3 and the dashed curve represents only τ3 term. In the middle the residuals from the linear plus the apsidal motion ephemeris were plotted with the theoretical LTE τ3 term. The residuals from the full contribution of Eq. (1) were plotted in the bottom panel. The standard deviation of the residuals with a relatively large scatter was calculated to be ±0.0025 days which is slightly larger than the small semi-amplitude of 0.0021 days for the LTE orbit as listed in Table 2.

Fig. 1.Eclipse timing variation diagram with theoretical lines calculated with the parameters in Table 2. Open and cross symbols refer to primary and secondary minimum timings, respectively, where circle and square represent Photoelectric (PE) and CCD timings, respectively. The black and grey solid lines on the top panel represent the theoretical apsidal motion plus LTE terms for primary and secondary eclipses, respectively. The dash lines on the top and middle panels also represent the theoretical LTE (τ3). The bottom panel indicates the residual from Eq (1).

Table 2.Parameters of the apsidal motion and LTE for CW Cep

Because the Zasche code we used was based on a differential least-square method Zasche et al. (2009), our solution of Eq. (1) may be a solution with a local minimum rather than a global solution. It would be very necessary to check whether our solution is globally valid for all parameter space. In line with this validity, we subsequently attempted a Monte Carlo simulation to obtain optimized values of the parameters both of the apsidal motion and the LTE orbit as performed by Lee et al. (2015). After 800 simulations all the apsidal motion parameters showed a quick convergence to nearly the same values listed in Table 2, while the LTE parameters show relatively wide variation as shown in the histograms of Fig. 2. Particularly, the distribution of e3 showed remarkably wide variation, indicating that the proposed LTE orbit is not well defined with reliable accuracy by present observational data.

Fig. 2.Histograms for distributions of the third body orbit parameters. The black lines represent the calculated elements of the third body orbit.

4. DISCUSSION OF APSIDAL MOTION PERIOD

In this study, the new times of minimum lights were presented by the observations of CBNUOJ, together with the collected times of minimum lights as shown in Table 1. The O-C diagram of a differential least-square fit to the minimum lights were shown in Fig. 1. We calculated the new apsidal motion period as 46.27 ± 0.04 years. The apsidal parameters are listed in Table 2, which shows similar apsidal motion period with those of earlier investigators (Han at al 2002; Wolf et al. 2006), however with much improved accuracy. The existence of a third body in the CW Cep system was also suggested by many previous investigators (Han et al. 2000; Wolf et al. 2006; Bulut et al. 2011). Based on the analysis of currently available minimum lights in Table 1, we calculated the period of the LTE caused by the third body as 39.3 ± 4.4 years as shown dash line in Fig. 1. However, the LTE caused by the third body may not be convinced due to a wide variation of orbital eccentricity (e3) in Fig. 2 and a small semi-amplitude compatible to a large scatter band of the residuals in Fig. 1.

The masses and radii of CW Cep by the photometric and spectroscopic parameters suggested by Clausen & Giménez (1991) are M1=11.82 ± 0.14M⊙, M2=11.09 ± 0.14M⊙, R1=5.48 ± 0.12R⊙, and R2=4.99 ± 0.12R⊙. With these parameters, we calculated the internal structure constant of the system, as logk2,obs=-2.106 that is slightly small value rather than the theoretical internal structure constant -2.08 suggested by Wolf et al. (2006). If the third body component exists around CW Cep, the minimum mass of the third can be calculated by the mass function ( f(M3)) of 4×10-5. The results show that the third body component should be 0.279 M⊙ when i3 is 90°, and in the case of i3 is 30°, the mass is 0.562 M⊙. These are approximately 2% range of mass of CW Cep binary system, which is too small compared to CW Cep and the masses are close to red dwarfs range. Therefore detecting the third body by photometry and spectroscopy would be very difficult. Apsidal motion period is very important because it can provide the important constant for the stellar internal structure. In this regards, many investigators have paid attention to the apsidal motion of CW Cep, and more accurate observations will be necessary to analyze the apsidal motion of the binary system and periodic variations by the third body.