Evolution of massive close binaries

Loore, C. De; Greve, J. P. De; Cuyper, J. P. de

doi:10.1007/bf00681952

Cited by 60 publications

(22 citation statements)

References 4 publications

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“…It will be clear that a system like Cyg X-3 is an almost ideal progenitor for close double neutron star systems like the Hulse-Taylor pulsar PSR 1913+16 (P = 7h45 m, e = 0.615) and PSR 1534+12, as was pointed out long ago (Flannery and van den Heuvel 1975;De Loore et al 1975). If the initial system resembles Cygnus X-I, the binary after spiral-in will consist of a helium star and a black hole.…”

Section: Final Evolution Of Hmxbs Cygnus X-3 and The Formation Of Domentioning

confidence: 78%

Massive close binaries: Observational characteristics

Heuvel

1993

Space Sci Rev

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Abstract. Theoretically predicted evolutionary phases of massive close binaries are compared with the observations. For the evolution up to the High-Mass X-ray Binary (HMXB) phase there is fair agreement between theory and observation. Beyond the HMXB phase there is much uncertainty. Notably it is puzzling why we observe so few systems consisting of a helium star and a neutron star (Cygnus X-3 is the only one found so far), and why the incidence of double neutron stars is so low. A better understanding of Common Envelope evolution is required in order to answer these questions. The role of velocity kicks imparted to neutron stars during supernova collapse is discussed. Such kicks might cause many runaway OB stars to be single.

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Section: Final Evolution Of Hmxbs Cygnus X-3 and The Formation Of Domentioning

confidence: 78%

Massive close binaries: Observational characteristics

Heuvel

1993

Space Sci Rev

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“…Systems with low-mass mainsequence companions are also expected to survive, however their progenitor systems may not be Be binaries. The future evolution of these products can either lead to the merger of the two components or to the production of close compact binary systems such as PSR1913+16 and PSR1534+12 (see Flannery & Van den Heuvel 1975;De Loore et al 1975) for a neutron star companion, and to LMXBs for a main-sequence like companion.…”

Section: Discussionmentioning

confidence: 99%

Common-Envelope Evolution, the Formation of CVs, LMXBs, and the Fate of HMXBs

Taam¹

1996

Symp. - Int. Astron. Union

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Abstract. Recent three-dimensional studies of the common-envelope phase of binary evolution have provided important insights into its theoretical description. The role of non-axisymmetric effects associated with gravitational torques is essential for understanding all aspects of the evolution. For successful ejection of the common envelope and survival of the remnant compact binary it is required that the orbital period of the progenitor system is long, so that one of the components of the system is in the red giant or red supergiant stage of evolution. Not only must there be sufficient energy released from the orbit to unbind the common envelope, but it is also necessary that a sufficiently steep density gradient exist above the evolved core of the giant. If these conditions are satisfied, the time scale for orbital decay in the region above the core exceeds the time scale for mass loss from the common envelope and merger is avoided. The implications of these results for the formation of cataclysmic variables (CVs), low-mass X-ray binaries (LMXBs), and the descendants of high-mass X-ray binaries (HMXBs) are discussed.

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“…Observations of white dwarfs in galactic clusters and theoretical stellar models indicate that for single stars the lower mass limit for becoming a supernova is around 6-8 M® (Gunn and Ostriker, 1970;van den Heuvel, 1975;Sugimoto and Nomoto, 1980 ) -On the other hand, a component of a close binary loses before the end of its evolution more than two thirds of its mass by mass transfer to its companion and mass loss out of the system. As a consequence of this mass loss a much larger initial mass of a component of a binary is required for direct collapse of the stellar core to a relativistic star (van den Heuvel, 1981).…”

Section: Evaluation Of the Explosion Parametersmentioning

confidence: 99%

“…An acceleration of the collapsed star due to an asymmetry in the explosion process was taken into account numerically by De Cuyper (197*0; de Loore, De Greve, van den Heuvel and De Cuyper (1975) for a time dependent explosion in a circular orbit. The analytic treatment of an instantaneous asymmetric explosion neglecting the effects of impact was given by Sutantyo (1978).…”

Section: Introductionmentioning

confidence: 99%

Supernovae in Binary Systems : Production of Run-Away Stars and Pulsars

Cuyper

1982

International Astronomical Union Colloquium

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The effects of an instantaneous asymmetric supernova explosion in an eccentric binary system are analyzed, taking into account the mass loss out of the system, the influence of the impact of the supernova shell on the companion star and the extra “kick” velocity which a collapsed star might receive in an asymmetric supernova explosion. For a random orientat-ion in space of this asymmetric kick velocity, the survival probability and the runaway velocities are derived and their properties discussed for an explosion occurring at a given position in the initial keplerian orbit and the mean and extreme values of these quantities over one orbit are derived. As an example, the outcome of a possible supernova explosion in the ten best known WR+OB binaries is studied and a comparison is made with the observed run-away OB stars, radio pulsars and binary X-ray pulsars.

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Evolution of massive close binaries

Cited by 60 publications

References 4 publications

Massive close binaries: Observational characteristics

Massive close binaries: Observational characteristics

Common-Envelope Evolution, the Formation of CVs, LMXBs, and the Fate of HMXBs

Supernovae in Binary Systems : Production of Run-Away Stars and Pulsars

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