International Observational Campaigns of the Last Two Eclipses in EE Cephei: 2003 and 2008/9
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Astronomy & Astrophysics manuscript no. EECep˙AaA˙120417 c ESO 2018 September 19, 2018 International observational campaigns of the last two eclipses in EE Cep: 2003 and 2008/9 ⋆ C. Gałan1,2, M. Mikołajewski1, T. Tomov1, D. Graczyk3, G. Apostolovska4, I. Barzova5, I. Bellas-Velidis6, B. Bilkina5, R.M. Blake7, C.T. Bolton8, A. Bondar9, L. Br´at10,11, T. Bro˙zek1, B. Budzisz1, M. Cikała1,12, B. Cs´ak13, A. Dapergolas6, D. Dimitrov5, P.Dobierski1, M. Drahus14, M. Dr´o˙zd˙z15, S. Dvorak16, L. Elder17, S. Fra¸ckowiak1, G. Galazutdinov18, K. Gazeas19, L. Georgiev20, B. Gere21, K. Go´zdziewski1, V.P.Grinin22, M. Gromadzki1,23, M. Hajduk1,24, T.A. Heras25, J. Hopkins26, I. Iliev5, J. Janowski1, R. Koci´an27, Z. Kołaczkowski3,28, D. Kolev5, G. Kopacki28, J. Krzesi´nski15, H. Kuˇc´akov´a27, E. Kuligowska29, T. Kundera29, M. Kurpi´nska-Winiarska29 , A. Ku´zmicz29, A. Liakos19, T.A. Lister30, G. Maciejewski1, A. Majcher1,31, A. Majewska28, P.M. Marrese32, G. Michalska3,28, C. Migaszewski1, I. Miller33,34, U. Munari35, F. Musaev36, G. Myers37, A. Narwid28, P.N´emeth38, P.Niarchos19, E. Niemczura28, W. Ogłoza15, Y. Oˇgmen¨ 39, A. Oksanen40, J. Osiwała1, S. Peneva5, A. Pigulski28, V.Popov5, W. Pych41, J. Pye17, E. Ragan1, B.F. Roukema1, P.T. R´o˙za´nski1, E. Semkov5, M. Siwak15,29, B. Staels42, I. Stateva5, H.C. Stempels43, M. Ste¸´slicki28, E. Swierczy´nski´ 1, T. Szyma´nski29, N. Tomov5, W. Waniak29, M. Wie¸cek1,44, M. Winiarski15,29, P.Wychudzki1,2, A. Zajczyk1,24, S. Zoła15,29, and T. Zwitter45 (Affiliations can be found after the references) Received xxxxx xx, xxxx; accepted xxxxx xx, xxxx ABSTRACT Context. EE Cep is an unusual long-period (5.6 yr) eclipsing binary discovered during the mid-twentieth century. It undergoes almost-grey eclipses that vary in terms of both depth and duration at different epochs. The system consists of a Be type star and a dark dusty disk around an invisible companion. EE Cep together with the widely studied ε Aur are the only two known cases of long-period eclipsing binaries with a dark, dusty disk component responsible for periodic obscurations. Aims. Two observational campaigns were carried out during the eclipses of EE Cep in 2003 and 2008/9 to verify whether the eclipsing body in the system is indeed a dark disk and to understand the observed changes in the depths and durations of the eclipses. Methods. Multicolour photometric data and spectroscopic observations performed at both low and high resolutions were collected with several dozen instruments located in Europe and North America. We numerically modelled the variations in brightness and colour during the eclipses. We tested models with different disk structure, taking into consideration the inhomogeneous surface brightness of the Be star. We considered the possibility of disk precession. Results. The complete set of observational data collected during the last three eclipses are made available to the astronomical community. The 2003 and 2008/9 eclipses of EE Cep were very shallow. The latter is the shallowest among all observed. The very high quality photometric data illustrate in detail the colour evolution during the eclipses for the first time. Two blue maxima in the colour indices were detected during these two eclipses, one before and one after the photometric minimum. The first (stronger) blue maximum is simultaneous with a “bump” that is very clear in all the UBV(RI)C light curves. A temporary increase in the I-band brightness at the orbital phase ∼ 0.2 was observed after each of the last three eclipses. Variations in the spectral line profiles seem to be recurrent during each cycle. The Na i lines always show at least three absorption components during the eclipse minimum and strong absorption is superimposed on the Hα emission. Conclusions. These observations confirm that the eclipsing object in EE Cep system is indeed a dark, dusty disk around a low luminosity object. The primary appears to be a rapidly rotating Be star that is strongly darkened at the equator and brightened at the poles. Some of the conclusions of this work require verification in future studies: (i) a complex, possibly multi-ring structure of the disk in EE Cep; (ii) our explanation of the “bump” observed during the last two eclipses in terms of the different times of obscuration of the hot polar regions of the Be star by the disk; and m (iii) our suggested period of the disk precession (∼ 11–12 Porb) and predicted depth of about 2. for the forthcoming eclipse in 2014. arXiv:1205.0028v3 [astro-ph.SR] 26 Sep 2012 Key words. Stars: binaries, eclipsing – Stars: circumstellar matter – Stars: emission-line, Be 1. Introduction (epoch E = 0) by Romano (1956) and soon confirmed by Weber (1956), who reported observations obtained during a previous The 11th magnitude star EECep is a unique object among the eclipse in 1947 (E = -1). Since then, ten consecutive primary about 40 well-known eclipsing systems with orbital periods eclipses have been observed, while a secondary eclipse has never longer than one year. The primary B5 III star is obscured by been detected. The depths of the eclipses vary across a wide an invisible, dark secondary component of very low luminosity range of magnitudes from about 0m. 5to2m. 0 (see Graczyk et al. every 5.6 yr. The variability of the star was discovered in 1952 2003). However, all of them seem to have the same features: they are almost grey and have a similar asymmetric shape (the ⋆ Tables B.1 – B.36 are available at the CDS via descending branch of every eclipse has a longer duration than the anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via ascending one). In the light curves of all the eclipses, it is pos- http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/544/A53 2 C. Gałan et al.: International observational campaigns of the last two eclipses in EE Cep 0 1a 0.2 0.4 1 1a 4a 2 4 0.6 0.8 1 1 3 1.2 1.4 4 3 Var - comp [mag] 1.6 4a 2 1.8 2 Fig. 1. Schematic representation of the eclipse geometry in the 2.2 EECep system. The inner opaque and outer semi-transparent re- 720 740 760 780 800 820 gions of the disk are separated. The characteristic positions of JD - 2450000 the disk and the star configuration during the eclipses (left) cor- respond to the contact times (1a, 1, 2, 3, 4, 4a) distinguished in Fig. 2. U (dots) and i (crosses) light curves obtained during the the light curve (right). The figure shows a highly simplified case 1997 eclipse of EECep. that ignores a number of issues such as e.g. possible inhomo- geneities in the distribution of brightness on the star’s surface or of the actual size of the disk. results of the second campaign were systematically presented during the eclipse at a web page1. sible to distinguish five characteristic phases (shown in Fig.1): ingress (1-2) and egress (3-4) are preceded and followed, respec- 2. Observations tively, by extended atmospheric eclipse parts (1a-1 and 4-4a), 2.1. The 1997 eclipse and in the middle of the eclipses a bottom phase of variableslope (2-3) occurs. During the 1997 eclipse (epoch E = 8), the first multicolour The most plausible hypothesis to explain the observed shape UBVRCi (λ¯ i ≈ 7420 Å) photometric observations were made of the light curve, as well as the changes in the eclipse depth using a 60 cm Cassegrain telescope at the Piwnice Observatory during successive conjunctions and their weak dependence on near Toru´n(Poland) equipped with a one-channel photometer the photometric band was proposed by Mikołajewski & Graczyk (Mikołajewski & Graczyk 1999). This eclipse was one of the (1999). Their model considers the eclipses of a hot B5-type pri- deepest eclipses of all those observed in EECep. However, the mary by an invisible, dark companion, which is most proba- amplitude of the minimum changes quite weakly with wave- bly a dusty disk around a low-luminosity central object. The length from about 1m. 75 in the U passband to about 1m. 45 in i disk is slightly inclined to the orbital plane. The obscurations (Fig.2). These observations thus provided the first evidence that of the star by the opaque interior of the disk can explain the the eclipsing body cannot be an ordinary evolved cool star, mo- deep central parts of the eclipses, while the semi-transparent tivating us to organize a special international observational cam- exterior areas are responsible for the observed external wings, paign for the next two minima. A complete set of UBVRCi pho- which are similar to wings caused by atmospheric eclipses in tometry obtained in 1997 is shown in our Appendix (available ζ Aur type variable stars. The projection of the inclined disk online) in Table B.1. onto the sky plane produces oblong shape of an obscuring body, which is tilted with respect to the direction of motion during most of the occultations. Since the eclipses are not central (the 2.2. International photometric campaigns in 2003 and 2008/9 impact parameter is non-zero), the light curves observed during Observers from four European countries responded to the ap- the eclipses have an asymmetric shape (Fig. 1). A possible pre- peal of Mikołajewski et al. (2003) to perform a precise moni- cession of the disk can change both the inclination of the disk toring of the subsequent eclipse of EECep anticipated in 2003 to the line of sight and the tilt of its cross-section to the transit (epoch E = 9).