منابع مشابه
Eclipsing 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 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 کاملThe LMC eclipsing binary HV 2274 revisited
We reanalyse the UV/optical spectrum and optical broad-band data of the eclipsing binary HV 2274 in the LMC, and derive its distance following the method given by Guinan et al. (1998a,b) of fitting theoretical spectra to the stars' UV/optical spectrum plus optical pho-tometry. We describe the method in detail, pointing out the various assumptions that have to be made; moreover, we discuss the s...
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 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 ...
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ژورنال
عنوان ژورنال: The Astronomical Journal
سال: 1959
ISSN: 0004-6256
DOI: 10.1086/107863