UBV Photometry of the Massive Eclipsing Binary TT Aur

Abstract

UBV observations of the massive binary system TT Aur were carried out mainly at theTurkish National Observatory (TUG). These observations, together with IUE spectra and times of eclipse minima collected from the literature, were used to study the system parameters.Simultaneous solution of the light curves by the Wilson-Devinney code allows a semi-detached configuration with a slightly larger Roche-lobe filling secondary. This picture is supported by other evidence. The shoulders of the primary minimum suggest some excess absorption, in keeping with circumstellar material in the form of a disk-like structure around the primary component. The deeper primary minimum in the U filter may indicate a hotter region on the secondary-facing hemisphere of the primary.The period variation of the system can also be related to the possible existence of a third component in a circular orbit around the system.An alternative detached representation is also considered using optimal curve-fitting techniques. We appeal for further observations to help resolve some outstanding issues in this interesting massive binary.

The early-type semidetached binary system V716 Centaurus

“…7, the zero‐age main‐sequence (ZAMS) and terminal‐age main‐sequence (TAMS) of Girardi et al (2000) are plotted. A literature search reveals that the OB‐type binaries such as TT Aur (Özdemir et al 2001), SX Aur (Chambliss & Leung 1979), XZ Cep, V448 Cyg (Harries, Hilditch & Hill 1997), U Her (Hilditch 1984), VY Lac (Semeniuk & Kaluzny 1984), β Lyr (Harmanec 1990), DM Per (Hilditch, Hill & Khalesseh 1992), IZ Per (Srivastava & Padalia 1970), V356 Sgr, Z Vul (Hilditch & Bell 1987), V Pup (Andersen et al 1983), μ 1 Sco (Schneider, Darland & Leung 1979), V337 Aql (Giuricin & Mardirossian 1981), IU Aur (Giuricin et al 1979) and LY Aur (Cester et al 1978) are all similar to V716 Cen. All of these systems are semidetached and mass transfer occurs from the less massive, Roche lobe filling secondary component to the more massive primary in core hydrogen‐burning phase, namely Case A (Paczyński 1971).…”

Analysis of δ Librae including Hipparcos astrometry

“…e.g. Özdemir et al 2001). For δ Lib, we can examine residuals from the main parabolic trend for further effects in view of the possible additional components in the system (Worek 1998; Lazaro, Arevalo & Claret 2002; Budding et al 2005a).…”

The most plausible explanation of the cyclic period changes in close binaries: the case of the RS CVn-type binary WW Dra

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