The formation of submillisecond pulsars and the possibility of detection

Du, Y. J.; Xu, R. X.; Qiao, G. J.; Han, J. L.

doi:10.1111/j.1365-2966.2009.15373.x

Cited by 31 publications

(23 citation statements)

References 61 publications

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“…As an alternative for the formation of MSPs, this evolutionary channel has been widely explored by some authors (Wickramasinghe et al 2009; Hurley et al 2010; Chen et al 2011a). In particular, Du et al (2009) argued that the AIC of massive white dwarfs can produce submillisecond pulsars (quark stars) with a spin period less than 1 ms (or less than 0.5 ms).…”

Section: Introductionmentioning

confidence: 99%

On the progenitors of millisecond pulsars by the recycling evolutionary channel

Liu

Chen

2011

Monthly Notices of the Royal Astronomical Society

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The recycling model suggested that low‐mass X‐ray binaries (LMXBs) could evolve into binary millisecond pulsars (BMSPs). In this work, we attempt to investigate the progenitor properties of BMSPs formed by the recycling evolutionary channel, and if submillisecond pulsars can be produced by this channel. Using Eggleton’s stellar evolution code, considering that the dead pulsars can be spun up to a short spin period by the accreting material and angular momentum from the donor star, we have calculated the evolution of close binaries consisting of a neutron star (NS) and a low‐mass main‐sequence donor star, and the spin evolution of NSs. In the calculation, some physical processes, such as the thermal and viscous instability of an accretion disc, propeller effect and magnetic braking, are included. Our calculated results indicate that all LMXBs with a low‐mass donor star of 1.0–2.0 M⊙ and a short orbital period (≲ 3–4 d) can form millisecond pulsars with a spin period less than 10 ms. However, it is difficult to produce submillisecond pulsars by this evolutionary channel. In addition, our evolutionary scenario cannot account for the existence of BMSPs with a long orbital period (Porb≳ 70–80 d).

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Section: Introductionmentioning

confidence: 99%

On the progenitors of millisecond pulsars by the recycling evolutionary channel

Liu

Chen

2011

Monthly Notices of the Royal Astronomical Society

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“…However, the accretion-induced collapse (AIC) of a white dwarf (Du et al 2009;Xu 2003Xu , 2005 could produce an extremely low mass self-bound star (strange quark or quark-cluster star), even as low as a planet-mass (Horvath 2012;Xu 2014;Xu & Wu 2003). A massive main sequence star will collapse into a NS with a lower limit of about 1 M .…”

Section: Discussionmentioning

confidence: 99%

4U 1746–37: An ultra‐low‐mass compact star candidate

2015

Astron Nachr

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Key words dense matter -equation of state -stars: neutron -X-rays: bursts -X-rays: binaries the Rossi X-ray Timing Explorer observed three photospheric radius expansion bursts in 4U 1746-37, all with low touchdown fluxes. We discuss the possibility of a low-mass neutron star in 4U 1746-37 if the touchdown flux corresponds to its Eddington limit. 4U 1746-37 is a dipping binary system which has a high inclination angle. Two geometric effects, the reflection of the far side accretion disc and the obscuration of the near side accretion disc have also been included. We apply a Monte-Carlo simulation, with typical values of hydrogen mass fraction and color correction factor, to constrain the mass and radius of the neutron star in 4U 1746-37. We found that the mass of 4U 1746-37 is 0.41 +0.70 −0.30 M at 99.7 % confidence which is an ultra-low-mass compact star candidate. It could be reproduced by a self-bound compact star, i.e., quark star or quark-cluster star, from an ccretion-induced collapse process.

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“…A lowmass NS may be difficult to form from the collapse of a massive star. However, an extremely low-mass, self-bound star (strange quark or quark-cluster star), even as low as planet mass (Xu & Wu 2003;Horvath 2012), could exist through the accretioninduced collapse of a white dwarf (Xu 2005;Du et al 2009). …”

Section: Discussionmentioning

confidence: 99%

An Ultra-Low-Mass and Small-Radius Compact Object in 4u 1746-37?

Chen

et al. 2014

ApJ

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Photospheric radius expansion (PRE) bursts have already been used to constrain the masses and radii of neutron stars. RXTE observed three PRE bursts in 4U 1746-37, all with low touchdown fluxes. We discuss here the possibility of a low-mass neutron star in 4U 1746-37 because the Eddington luminosity depends on stellar mass. With typical values of hydrogen mass fraction and color correction factor, a Monte Carlo simulation was applied to constrain the mass and radius of a neutron star in 4U 1746-37. 4U 1746-37 has a high inclination angle. Two geometric effects, the reflection of the far-side accretion disk and the obscuration of the near-side accretion disk, have also been included in the mass and radius constraints of 4U 1746-37. If the reflection of the far-side accretion disk is accounted for, a low-mass compact object (mass of 0.41 ± 0.14M and radius of 8.73 ± 1.54 km at 68% confidence) exists in 4U 1746-37. If another effect operated, 4U 1746-37 may contain an ultra-low-mass and small-radius object (M = 0.21 ± 0.06M , R = 6.26 ± 0.99 km at 68% confidence). Combining all possibilities, the mass of 4U 1746-37 is 0.41 +0.70 −0.30 M at 99.7% confidence. For such low-mass neutron stars, it could be reproduced by a self-bound compact star, i.e., a quark star or quark-cluster star.

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The formation of submillisecond pulsars and the possibility of detection

Cited by 31 publications

References 61 publications

On the progenitors of millisecond pulsars by the recycling evolutionary channel

On the progenitors of millisecond pulsars by the recycling evolutionary channel

4U 1746–37: An ultra‐low‐mass compact star candidate

An Ultra-Low-Mass and Small-Radius Compact Object in 4u 1746-37?

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