|Statement||edited by E.P.J. van den Heuvel and S.A. Rappaport.|
|Series||NATO ASI series. Series C, Mathematical and physical sciences ;, vol. 377, NATO ASI series., no. 377.|
|Contributions||Heuvel, Edward Peter Jacobus van den, 1940-, Rappaport, S. A., 1942-|
|LC Classifications||QB821 .N363 1992|
|The Physical Object|
|Pagination||xvii, 566 p. :|
|Number of Pages||566|
|LC Control Number||92026378|
Get this from a library! X-Ray Binaries and Recycled Pulsars. [E P J Heuvel; S A Rappaport] -- The motivation for the Workshop on which this book is based was the discovery in recent years of a large number of binary and millisecond radio pulsars, in the galactic disk as well as in globular. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86AAuthor: E. P. J. van den Heuvel, A. King. Binary and millisecond pulsars (BMSPs) with He white dwarf companions are generally thought to be recycled in low-mass X-ray binaries (LMXBs). Here we investigate the formation of three recently discovered binary pulsars: PSRs J, J, and J+Cited by: (ebook) X-Ray Binaries and Recycled Pulsars () from Dymocks online store. Proceedings of the NATO Advanced Research Workshop on X-Ray.
ond X-ray pulsars in LMXBs. There are only 5 accretion-powered mil-lisecond X-ray pulsars known among more than 80 LMXBs containing neutron stars, but there are another 11 “nuclear-powered” millisecond pulsars which reveal their spin only during brief, thermonuclear X-ray bursts. In addition, 2 of the accretion-powered pulsars also exhibit. X-ray binaries are some of the most varied and perplexing systems known to astronomers. The compact object which accretes mass from its companion star may be a white dwarf, neutron star, or black hole, whereas the donor star can be a 'normal' star or a white dwarf. The various combinations differ widely in their behaviour, and this timely volume provides a unique reference of our knowledge to Reviews: 1. Binary and millisecond pulsars (BMSPs) with He white dwarf companions are generally thought to be recycled in low-mass X-ray binaries (LMXBs). Here we investigate the formation of three recently discovered binary pulsars: PSRs J, J, and J+ These pulsars are in circular orbits with low-mass white dwarf companions, but their spin periods and period derivatives are. Introduction and Abstract. Within this article the very wide field of accretion phenomena observed in X-rays is restricted to bright low-mass X-ray binaries (LMXB), where recent observational evidence leads to a global picture that for the first time sheds light on the innermost regions of an accretion disk LMXB are actually very similar to cataclysmic variables, one just has to replace the.
In X-ray binaries, neutron stars (the very dense stellar remnants of heavy stars) accrete matter from a close-by companion star. This matter eventually falls on the neutron star, significantly affecting it. I.e., the star is spun up to very high spin rates. In the end, it might rotate times a second which causes very fast oscillations in. 3. Binary X-ray pulsars 4. Theoretical prediction. Unavoidable formation of binary recycled radio pulsars 5. Magnetic field decay during accretion 6. Evolutionary formation schemes 7. Binary radio pulsars in globular clusters. The formation of single recycled pulsars 8. Relativistic effects in compact neutron star binaries. Millisecond pulsars (MSPs) are thought to originate from low-mass X-ray binaries (LMXBs). The discovery of eclipsing radio MSPs, including redbacks and black widows, indicates that evaporation of the donor star by the MSP’s irradiation takes place during the LMXB evolution. In this work, we investigate the effect of donor. X-ray binaries are a class of binary stars that are luminous in X-rays are produced by matter falling from one component, called the donor (usually a relatively normal star), to the other component, called the accretor, which is very compact: a neutron star or black infalling matter releases gravitational potential energy, up to several tenths of its rest mass, as X-rays.