The evolution of short-period binary pulsars: a systematic study

Érgma, É.; Sarna, M. J.; Antipova, J.

doi:10.1046/j.1365-8711.1998.01761.x

Cited by 50 publications

(60 citation statements)

References 17 publications

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“…Near the bifurcation period the nuclear time-scale of the secondary and the angular momentum loss time-scale are very close to each other. Therefore, during the binary evolution orbital period changes are insignificant in comparison with the initial orbital period (Tutukov et al 1985;Ergma et al 1998). In Fig.…”

Section: Results Of Calculationsmentioning

confidence: 99%

Eclipsing binary millisecond pulsar PSR J1740-5340 – evolutionary considerations and observational test

Érgma

Sarna

2003

A&A

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Abstract. We perform evolutionary calculations for a binary system to produce observed binary parameters for the PSR J1740-5340. Our calculations support the model proposed by D' Amico et al. (2001) in which this binary may be the progenitor of a millisecond pulsar + helium white dwarf system. We propose an observational test to verify this hypothesis. We propose that observations of abundances of C, N, O elements in the spectra of the optical companion of PSR J 1740-5340 may give additional information about the nature of the secondary being either i) a perturbed low-mass main-sequence star or ii) an evolved star with helium core and thin hydrogen envelope which has lost its main envelope during semi-detached evolution.

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Section: Results Of Calculationsmentioning

confidence: 99%

Eclipsing binary millisecond pulsar PSR J1740-5340 – evolutionary considerations and observational test

Érgma

Sarna

2003

A&A

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“…It is important to note that systems with an orbital period smaller than about 1-2 days, although in several cases appear to agree with the theoretical P −M relationship, should have had a different evolution because the mass transfer started when their secondaries were still on the main sequence (Ergma et al 1998;Taam et al 2000).…”

Section: The Residual Eccentricitymentioning

confidence: 87%

The residual orbital eccentricity in close binaries

Lanza

Rodonò

2001

A&A

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Abstract. Density fluctuations in convective stars produce small variations of their outer gravitational field that give rise to a very small, though finite, orbital eccentricity in close binaries with convective components. We revisit the theory for such an effect, originally presented by Phinney (1992), and propose a new approach to compute the fluctuations of the outer gravitational field based on Chandrasekhar's virial theorem. It is applied to compute the eccentricities of binaries with a millisecond pulsar component in the framework of a simplified model of their evolution. The comparison with the observations allows us to test the models proposed for the formation of such systems, giving support to the evolutionary scenarios that connect them with low-mass X-ray binaries, and to provide a new test for turbulent convection models of giant stars.

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“…For a more general discussion of MSP formation from LMXBs we refer to e.g. Ergma et al (1998), Tauris & Savonije (1999), Podsiadlowski et al (2002), Deloye (2008).…”

Section: Numerical Methods and Physical Assumptions Of Aicmentioning

confidence: 99%

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Tauris

Sanyal

Yoon

et al. 2013

A&A

147

181

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Context. Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB). In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary. Aims. Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities. Methods. Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre-and post-AIC evolution of close binaries. We investigated the mass transfer onto a massive WD (treated as a point mass) in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars. When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit. Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end. Results. We show that recycled pulsars may form via AIC from all three types of progenitor systems investigated and find that the final properties of the resulting MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel. However, as a consequence of the fine-tuned mass-transfer rate necessary to make the WD grow in mass, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals. In addition, their predicted small space velocities can also be used to identify them observationally. The production time of NSs formed via AIC can exceed 10 Gyr which can therefore explain the existence of relatively young NSs in globular clusters. Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions.

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The evolution of short-period binary pulsars: a systematic study

Cited by 50 publications

References 17 publications

Eclipsing binary millisecond pulsar PSR J1740-5340 – evolutionary considerations and observational test

Eclipsing binary millisecond pulsar PSR J1740-5340 – evolutionary considerations and observational test

The residual orbital eccentricity in close binaries

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

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