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http://dx.doi.org/10.5140/JASS.2011.28.3.163

WZ Cephei: A Dynamically Active W UMa-Type Binary Star  

Jeong, Jang-Hae (Department of Astronomy and Space Science, Chungbuk National University)
Kim, Chun-Hwey (Department of Astronomy and Space Science, Chungbuk National University)
Publication Information
Journal of Astronomy and Space Sciences / v.28, no.3, 2011 , pp. 163-172 More about this Journal
Abstract
An intensive analysis of 185 timings of WZ Cep, including our new three timings, was made to understand the dynamical picture of this active W UMa-type binary. It was found that the orbital period of the system has complexly varied in two cyclical components superposed on a secularly downward parabola over about 80y. The downward parabola, corresponding to a secular period decrease of $-9.{^d}97{\times}10^{-8}y^{-1}$, is most probably produced by the action of both angular momentum loss (AML) due to magnetic braking and mass-transfer from the massive primary component to the secondary. The period decrease rate of $-6.^{d}72{\times}10^{-8}y^{-1}$ due to AML contributes about 67% to the observed period decrease. The mass flow of about $5.16{\times}10^{-8}M_{\odot}y^{-1}$ from the primary to the secondary results the remaining 33% period decrease. Two cyclical components have an $11.^{y}8$ period with amplitude of $0.^{d}0054$ and a $41.^{y}3$ period with amplitude of $0.^{d}0178$. It is very interesting that there seems to be exactly in a commensurable 7:2 relation between their mean motions. As the possible causes, two rival interpretations (i.e., light-time effects (LTE) by additional bodies and the Applegate model) were considered. In the LTE interpretation, the minimum masses of $0.30M_{\odot}$ for the shorter period and $0.49M_{\odot}$ for the longer one were calculated. Their contributions to the total light were at most within 2%, if they were assumed to be main-sequence stars. If the LTE explanation is true for the WZ Cep system, the 7:2 relation found between their mean motions would be interpreted as a stable 7:2 orbit resonance produced by a long-term gravitational interaction between two tertiary bodies. In the Applegate model interpretation, the deduced model parameters indicate that the mechanism could work only in the primary star for both of the two period modulations, but could not in the secondary. However, we couldn't find any meaningful relation between the light variation and the period variability from the historical light curve data. At present, we prefer the interpretation of the mechanical perturbation from the third and fourth stars as the possible cause of two cycling period changes.
Keywords
W UMa-type sta; WZ Cep; period change; light-time effects; magnetic activities;
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1 Demircan O, Dynamical evolution of the RS CVn-type binaries, TJPh, 23, 425-432 (1999).
2 Applegate JH, A mechanism for orbital period modulation in close binaries, ApJ, 385, 621-629 (1992). http://dx.doi.org/10.1086/170967   DOI
3 Balázs J, WZ Cephei, Beob Zirk d A N, 19, 7 (1937).
4 Zhu LY, Qian SB, WZ Cephei: a close binary at the beginning of contact phase, AJ, 138, 2002-2006 (2009). http://dx.doi.org/10.1088/0004-6256/138/6/2002   DOI
5 Samolyk G, Recent minima of 185 eclipsing binary Stars, JAAVSO, 38, 1-10 (2010a).
6 Stepien K, Loss of angular momentum of cool close binaries and formation of contact systems, MNRAS, 274, 1019-1028 (1995).
7 Stepien K, The low-mass limit for total mass of W UMa-type binaries, AcA, 56, 347-364 (2006).
8 van't Veer F, The angular momentum controlled evolution of solar type contact binaries, A&A, 80, 287-295 (1979).
9 Samolyk G, Recent minima of 184 eclipsing binary stars, JAAVSO, 36, 186-206 (2008b).
10 Samolyk G, Recent minima of 154 eclipsing binary stars, JAAVSO, 37, 44-51 (2009).
11 Samolyk G, Recent minima of 161 eclipsing binary stars, JAAVSO, 38, 85-92 (2010b).
12 Schneller H, Sieben neue veranderliche, Astron Nachr, 233, 41-42 (1928).   DOI
13 Nagai K, Visual and CCD minima of eclipsing binaries during 2009, Var Star Bull, 50, 1-10 (2010).
14 Kałużny J, Contact binaries with components in poor thermal contact. II. WZ Cephei, AcA, 36, 105-111 (1986).
15 Lucy LB, W Ursae Majoris systems with marginal contact, ApJ, 205, 208-216 (1976). http://dx.doi.org/10.1086/154265   DOI
16 Maceroni C, van't Veer F, The galactic cluster NGC 188: W Ursae Majoris contact binaries as a clue to two separate bursts of star formation, A&A, 248, 430-434 (1991).
17 Mullan DJ, On the possibility of magnetic starspots on the primary components of W Ursae Majoris type binaries, ApJ, 198, 563-573 (1975). http://dx.doi.org/10.1086/153635   DOI
18 Kholopov PN, General catalogue of variable stars, 4th ed., vol. III, Constellations pavo-vulpecula (Nauka Publishing House, Moscow, 1987).
19 Wilson RE, Devinney EJ, Realization of accurate close-binary light curves: application to MR Cygni, ApJ, 166, 605-619 (1971). http://dx.doi.org/10.1086/150986   DOI
20 Webbink RF, The evolution of low-mass close binary systems. I. The evolutionary fate of contact binaries, ApJ, 209, 829-845 (1976). http://dx.doi.org/10.1086/154781   DOI
21 Robertson JA, Eggleton PP, The evolution of W Ursae Majoris systems, MNRAS, 179, 359-375 (1977).   DOI
22 Rucinski SM, Contact binaries: angular momentum loss in and out of contact, A&A, 112, 273-276 (1982).
23 Samolyk G, Recent minima of 155 eclipsing binary stars, JAAVSO, 36, 171-185 (2008a).
24 Press WH, Teukolsky SA, Vetterling WT, Flannery BP, Numerical recipes in C, 2nd ed. (Cambridge University Press, Cambridge, 1992), Chap.15.
25 Parimucha S, Dubovsky P, Baluďansky D, Pribulla T, Ham-balekL, et al., Minima times of selected eclipsing binaries, IBVS, 5898, 1 (2009).
26 ParimuchaS, Dubovsky P, Vanko M, Pribulla T, Kudzej I, et al., Minima times of selected eclipsing binaries, IBVS, 5980, 1 (2011).
27 Peale SJ, Orbital resonances in the solar system, ARA&A, 14, 215-246 (1976). http://dx.doi.org/10.1146/annurev.aa.14.090176.001243   DOI
28 Kwee KK, van Woerden H, A method for computing accurately the epoch of minimum of an eclipsing variable, BAN, 12, 327 (1956).
29 Lee W-B, Kang Y-W, Oh K-D, CCD photometry of contact binary WZ Cephei, JASS, 25, 19-24 (2008). http://dx.doi.org/10.5140/JASS.2008.25.1.019   DOI
30 Kim C-H, Lee C-U, Yoon Y-N, Park S-S, Kim D-H, et al., New CCD times of minima of eclipsing binary systems, IBVS, 5694, 1 (2006).
31 Kim C-H, Nha I-S, Kreiner JM, A possible detection of a second light-time orbit for the massive, early-type eclipsing binary star AH Cephei, AJ, 129, 990-1000 (2005). http://dx.doi.org/10.1086/426747   DOI
32 Kley W, Peitz J, Bryden G, Evolution of planetary systems in resonance, A&A, 414, 735-747 (2004). http://dx.doi.org/10.1051/0004-6361:20031589   DOI
33 Kreiner JM, Kim C-H, Nha I-S, An atlas of O-C diagrams of eclipsing binary stars (Wydawnictwo Naukowe Akademii Pedagogicznej, Krakow, 2001).
34 Eaton JA, SW Lacertae, W Urase Majoris, YY Eridani, and the prevalence of starspots in cool contact binaries, AcA, 36, 79-103 (1986).
35 Djurasevic G, An analysis of active close binaries (CB) based on photometric measurements. I. A model of active CB with spots on the components, Ap&SS, 196, 241-265 (1992a). http://dx.doi.org/10.1007/BF00692893   DOI
36 Detre L, Das system WZ Cephei, Budapest Mitt, 10, 3 (1940).
37 Diethelm R, Timings of minima of eclipsing binaries, IBVS, 5920, 1 (2010).
38 Diethelm R, Timings of minima of eclipsing binaries, IBVS, 5960, 1 (2011).
39 Djurasevic G, An analysis of active close binaries (CB) based on photometric measurements. III. The inverse-problem method: an interpretation of CB light curves, Ap&SS, 197, 17-34 (1992b). http://dx.doi.org/10.1007/BF00645069   DOI
40 Djurasevic G, Zakirov M, Hojaev A, Arzumanyants G, Analysis of the activity of the eclipsing binary WZ Cephei, A&AS, 131, 17-23 (1998). http://dx.doi.org/10.1051/aas:1998248   DOI
41 Irwin JB, The determination of a light-time orbit, ApJ, 116, 211-217 (1952). http://dx.doi.org/10.1086/145604   DOI
42 Flannery BP, A cyclic thermal instability in contact binary stars, ApJ, 205, 217-225 (1976).   DOI
43 Harmanec P, Stellar masses and radii based on modern binary data, BAICz, 39, 329-345 (1988).
44 Hoffmann M, Photoelectric observations of contact binary stars, VeBon, 96, 1-9 (1984).
45 Irwin JB, Standard light-time curves, AJ, 64, 149-155 (1959). http://dx.doi.org/10.1086/107913   DOI
46 Bradstreet DH, Guinan EF, Stellar mergers and acquisitions: the formation and evolution of W Ursae Majoris binaries, ASPC, 56, 228-243 (1994).
47 Baldwin ME, Samolyk G, Observed minima timings of eclipsing binaries, number 9 (American Association of Variable Star Observers, Cambridge, 2004).
48 Baldwin ME, Samolyk G, Observed minima timings of eclipsing binaries, number 12 (American Association of Variable Star Observers, Cambridge, 2007).