منابع مشابه
Discovery of a 3.6-hr Eclipsing Luminous X-ray Binary in the Galaxy Ngc 4214
We report the discovery of an eclipsing X-ray binary with a 3.62-hr period within 24 of the center of the dwarf starburst galaxy NGC 4214. The orbital period places interesting constraints on the nature of the binary, and allows for a few very different interpretations. The most likely possibility is that the source lies within NGC 4214 and has an X-ray luminosity, Lx, of up to 7 × 10 ergs s. I...
متن کاملEclipsing Binary Pulsars
The first eclipsing binary pulsar, PSR B1957+20, was discovered in 1987. Since then, 13 other eclipsing low-mass binary pulsars have been found; 12 of these are in globular clusters. In this paper we list the known eclipsing binary pulsars and their properties, with special attention to the eclipsing systems in 47 Tuc. We find that there are two fundamentally different groups of eclipsing binar...
متن کاملAutomated analysis of eclipsing binary lightcurves. I. EBAS — a new Eclipsing Binary Automated Solver with EBOP
We present a new algorithm— Eclipsing Binary Automated Solver (EBAS), to analyse lightcurves of eclipsing binaries. The algorithm is designed to analyse large numbers of lightcurves, and is therefore based on the relatively fast EBOP code. To facilitate the search for the best solution, EBAS uses two parameter transformations. Instead of the radii of the two stellar components, EBAS uses the su...
متن کاملEclipsing Binary Stars from Space
We have begun a programme to obtain high-precision photometry of bright detached eclipsing binary (dEB) stars with the Wide field InfraRed Explorer (wire) satellite (Bruntt & Buzasi 2006). Due to the small aperture of wire only stars brighter than V = 6 can be observed. We are collecting data for about a dozen dEB targets and here we present preliminary results for three of them. We have chosen...
متن کاملGravitational lensing in eclipsing binary stars
I consider the effect of the gravitational deflection of light upon the light curves of eclipsing binary stars, focussing mainly upon systems containing at least one white dwarf component. In absolute terms the effects are small, however they are strongest at the time of secondary eclipse when the white dwarf transits its companion, and act to reduce the depth of this feature. If not accounted ...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Publications of the Astronomical Society of the Pacific
سال: 1971
ISSN: 0004-6280,1538-3873
DOI: 10.1086/129217