Evolution of a (1+0.75) solar mass close binary system with mass exchange and gravitational radiation losses.

Chau, W. Y.; Lauterborn, D.

doi:10.1086/155279

Cited by 7 publications

(2 citation statements)

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“…(1) If the companion is a low mass white dwarf [64] or an RL-filled star (e.g., [65]), mass transfer from the companion to the NS may occur. (2) When the companion star has not filled in its RL, gravitational radiation only removes energy and angular momentum [63].…”

Section: Gravitational Radiationmentioning

confidence: 99%

Can SGRs/AXPs Originate from Neutron Star Binaries?

Wang

Chang

2014

Physics Research International

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Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are two groups of enigmatic objects, which have been extensively investigated in past few decades. Based on the ample information about their timing behaviors, spectra, and variability properties, it was proposed that SGRs/AXPs are isolated neutron stars (NSs) with extremely strong magnetic fields, the so-called magnetars. Nonetheless, some alternative models are probably equally convincing such as those proposing that they are accreting NSs with a fall-back disk or rotation-powered magnetized and massive white dwarfs. The nature and nurture of SGRs/AXPs remain controversial. In this paper, we propose that SGRs/AXPs can, alternatively, originate from normal NSs in binary systems, which resorts to the reexplosion of normal NS induced by instant contraction of the massive star envelope in a Thorne-Żytkow object (TZO). The spin-period clustering is due to either the brake of a slowly rotating envelope or the frictional drag during the common-envelope phase.

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Section: Gravitational Radiationmentioning

confidence: 99%

Can SGRs/AXPs Originate from Neutron Star Binaries?

Wang

Chang

2014

Physics Research International

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“…Faulkner (1971) and Taam, Flannery, & Faulkner (1980) showed that gravitational radiation, by removing orbital angular momentum, could stimulate mass transfer from the main sequence red component at a rate which causes the binary to evolve more rapidly than nuclear evolution would dictate. Faulkner (1976) and Chau & Lauterborn (1977) have both found very significant effects of J [via gravitational radiation (GR) in their computations] on the evolution of low-mass close binary systems. Chau (1978) has considered the effects of loss of orbital angular momentum via gravitational radiation on the period changes and the implications for mass-transfer rate determinations.…”

Section: Gravitational Radiation and Magnetic Braking Via Mswmentioning

confidence: 99%

Structure and evolution of low-mass W Ursae Majoris type systems - II. With angular momentum loss

Li¹,

Han²,

Zhang³

2004

Monthly Notices of the Royal Astronomical Society

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In a previous paper, using Eggleton's stellar evolution code we have discussed the structure and evolution of low‐mass W Ursae Majoris (W UMa) type contact binaries without angular momentum loss (AML). The models exhibit cyclic behaviour about a state of marginal contact on a thermal time‐scale. Part of the time of each cycle is spent in contact and part in a semidetached state. According to observations, W UMa systems suffer AML. We present the models of low‐mass contact binaries with AML due to gravitational wave radiation or magnetic stellar wind (MSW). We find that gravitational radiation cannot prevent the cyclic evolution of W UMa systems, and the effect of gravitational radiation on the cyclic behaviour of contact binary evolution is almost negligible. We also find that the most likely AML mechanism for W UMa systems is magnetic braking, and that magnetic braking effects can increase the period of the cyclic evolution and shorten the fraction of the time spent in the poor thermal contact state exhibiting EB light curve. If W UMa stars do not undergo cyclic evolution, and their AML is caused simultaneously by MSW of both components, we find that the value of the parameter, λ, should be taken as about 3.8 for W UMa systems, which is larger than the largest value of similar single stars derived from observations. This indicates that the AML efficiency in W UMa systems may be lowered in comparison with non‐contact stars because of less mass contained in the convective envelopes of the components in W UMa systems or some feedback mechanism which may have an effect on W UMa systems. If W UMa systems lose their angular momentum at a constant rate, an angular momentum rate of d ln J/dt≈ 1.6 × 10−9 yr−1 can prevent the cyclic behaviour of the model, and the model can keep in good contact with an essentially constant depth of contact.

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The Evolution of Low Mass Binary Systems

Taam¹

1986

The Evolution of Galactic X-Ray Binaries

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Evolution of a (1+0.75) solar mass close binary system with mass exchange and gravitational radiation losses.

Cited by 7 publications

References 0 publications

Can SGRs/AXPs Originate from Neutron Star Binaries?

Can SGRs/AXPs Originate from Neutron Star Binaries?

Structure and evolution of low-mass W Ursae Majoris type systems - II. With angular momentum loss

The Evolution of Low Mass Binary Systems

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