The Eclipsing X-Ray Binary System Centaurus X-3

Al-Banawi Al-Banawi

doi:10.3844/pisp.2010.65.68

Abstract

Problem statement: We present new physical and geometrical elements for the eclipsing X-ray binary system Krzemenski's star (Centaurus X-3). Approach: In this study, the procedure depended on getting the best fit between the observational photometric light curves and synthetic ones built up in accordance to the Roche model. Results: The estimated elements showed a good agreement with the early estimated ones. Conclusion: In building the synthetic light curves, we assumed that the optical component of the system is filling to Roche lobe, the system is rotationally synchronized and we neglecting the effect of the magnetic fields of both components.

Highlights

A binary stellar system is one in which two stars orbit around a common center of mass, that is they are gravitationally bound to each other
A sub-class of binary systems are X-ray binaries, the systems in which a compact object and a stellar companion, orbit each other at a distance small enough to enable mass transfer from the companion star to the compact object
The present study focuses on the analysis of one such binary, Centaurus X-3, in a step to derive more reliable physical and geometrical elements

Summary

Introduction

A binary stellar system is one in which two stars orbit around a common center of mass, that is they are gravitationally bound to each other. A sub-class of binary systems are X-ray binaries, the systems in which a compact object (a white dwarf, neutron star or a black hole formed after collapse of an ordinary star) and a stellar companion, orbit each other at a distance small enough to enable mass transfer from the companion star to the compact object. The transferred matter spirals towards the compact object and forms an “accretion disk” around it. In case of a neutron star or a white dwarf the emission originates from both the accretion disk and the surface of the compact star while in black hole binaries the only source of X-rays is the accretion disk.

Methods

Results

Conclusion