|Statement||Edited by Kjeld Gyldenkerne and Richard M. West with the assistance of Bodil L. Valløe.|
|Contributions||Gyldenkerne, Kjeld, 1919- ed., West, Richard M., 1941- ed., Valløe, Bodil L. ed., International Astronomical Union., International Astronomical Union. Commission 42.|
|LC Classifications||QB821 .M36|
|The Physical Object|
|Number of Pages||238|
|LC Control Number||73580317|
The main difficulty of the theory of non-conservative evolution of close binaries is to estimate the mass loss and to determine the relation between the mass and angular momentum loss. A way to carry out evolutionary computat'ions when these effects are taken into account is to use the parameters which describe the mass and angular momentum : Huang Runqian, Chen Hailin, Xie Xin. Numerical models are presented for the evolution of low-mass binaries. Stars with solar mass are assumed to fill their Roche lobe, and account is taken of the loss of angular momentum. PDF | On Jan 1, , L. R. Yungelson published Evolution of close binaries with mass loss from the system III. Systems containing white dwarfs | Find, read and cite all the research you need on. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A.
Cite this paper as: Wood F.B. () Mass Loss from Close Binaries, In: Hack M. (eds) Mass Loss from Stars. Astrophysics and Space Science Library (A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection with the Journal Space Science Reviews), vol For lower mass stars as well as for massive close binaries, phases of mass exchange can occur during core hydrogen burning, shell hydrogen burning and helium burning. For massive close binaries mass loss by stellar wind already changes the orbital elements (see Chap eq. ). For the components of massive binary systems, rotational and gravitational effects may act together with the radiation force so as to increase the mass loss rate. Our intention here is to discuss the influence of a stellar wind mass loss on the evolution of massive close binaries. Key words. binaries: close – Stars: evolution – binaries: eclipsing – b inaries: spectroscopic – Stars: fundamental parameters – S tars: mass loss – Magellanic Clouds 1. Introduction Evolutionary calculations of massive close binaries have been conducted with various stellar evolution codes since the s, e.g. Paczyn´ski (
Massive star evolution depends critically on mass loss by stellar wind and this stellar wind mass loss may change dramatically when stars evolve from one phase to another. We start the book with a critical discussion of observations of the different types of massive stars, observations that are of fundamental importance in relation to stellar. The formation and evolution of low-mass (M2 M1 or = solar mass) close binaries influenced by angular momentum loss by radiation of gravitational waves and magnetic stellar wind is reviewed. The evolution of close binaries diers from the evolution of single stars, since the presence of a companion sets limits on the stellar expansion during its evolution. We examine the processes that have to be added to the stellar structure equations to compute the structure of the components of binary systems, and to calculate their evolution. The evolution of high-mass systems containing neutron stars is discussed, including double neutron stars, binary pulsars, Thorne-Zytkow objects, and high- and low-mass X-ray binaries. View Show.