Titlebook: Structure and Evolution of Single and Binary Stars; C. W. H. Loore,C. Doom Book 1992 Springer Science+Business Media New York 1992 star.st

oxidant

The Evolution of Low-Mass Stars,core is smaller than 0.31 M.. The upper boundary for this group of low-mass stars is not exactly determined; in fact it depends on the initial chemical composition of the stars and on the details of the theoretical computation of stellar models, especially on the modeling of convection. For Schwarzs

mitral-valve

The Evolution of Intermediate Mass Stars,xygen core, formed at helium exhaustion, is degenerate. Intermediate mass stars may thus be defined by means of two critical core masses. At the lower boundary the mass of the helium core for non-degenerate helium ignition, 0.31 M. is adopted, and at the upper boundary the mass of the carbon-oxygen

绝食

Canyon

坦白

The Evolution of Binary Stars General Considerations,naries: the total mass of the system M (=M.+M.), the mass ratio q (=M./M.) and the orbital period P. Evolutionary computations for close binaries can start with the two components at the ZAMS; the system is then defined by these three parameters. Owing to the interaction among the components where m

objection

The Evolution of Low and Intermediate Mass Binary Systems, of the companion. If a well determined critical value of the radius is exceeded mass transfer can occur from one component to the other, or mass can even leave the system, or may be stored in rings or disks. The computation of these mass transfer stages is only possible when certain approximations

变态

Generator

TAG

Conquest

0067-0057 ars with a variety ofmasses. The last chapter gives several models of stars with specificmasses. .The book is intended as an introduction for students, as well as areference for researchers.978-0-7923-1844-6978-94-011-2502-4Series ISSN 0067-0057 Series E-ISSN 2214-7985