Titlebook: Neutron Stars: Theory and Observation; Joseph Ventura,David Pines Book 1991 Kluwer Academic Publishers 1991 Accretion.Supernova.fluid dyna

支形吊灯

镇压

Pairing Interactions in Neutron Stars treated in a semi-empirical way, long-range fluctuations are incorporated consistently by solving coupled two-body equations for the particle-hole interaction and the scattering amplitude at the Fermi surface. The solutions determine the quasiparticle effective mass and the pairing matrix element f

Spangle

ULCER

The Formation of Neutron Stars in The Galaxy accretion-induced collapse of heavy white dwarfs. This article discusses constraints on both scenarios based on observations of supernovae, supernova remnants, binary radio pulsars and radio pulsars in globular clusters.

FOIL

Core Collapse Supernovae and Neutron Star Formationare likely to originate from massive stars, . ≳ 8.., at the end of their quiet hydrostatic nuclear burning and the final outcome is generally believed to be the birth event of most neutron stars. If this picture is correct the energy observed in the explosion must ultimately come from the gain in gr

Offensive

Neutron Star Formation in Close Binary Systemsf accretion-induced collapse of white dwarfs are examined in relation to the origin of low mass X-ray binaries and binary millisecond pulsars. The outcome of the evolution of accreting white dwarfs is summarized as functions of accretion rate and the initial mass of the white dwarf. (2) Secondly dis

sparse

高贵领导

Vaporizing Neutron Stars in Low-Mass X-Ray Binaries and the Statistics of Millisecond Pulsars companion irradiation. Here we discuss the main features of a radiation-driven (RD) evolutionary model that may be applicable to several LMXBs. According to this model, radiation from the accreting compact star in LMXBs ‘vaporizes’ the accretion disk and the companion star by driving a self-sustain

Crohns-disease

Processes