Millisecond X-Ray Pulsars in Low-mass X-Ray Binaries

White, N. E.; Zhang, William

doi:10.1086/311018

Cited by 108 publications

(106 citation statements)

References 21 publications

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“…However, in this case the higher the accretion rate is, the stronger is the pull of crustal material into the core resulting in an earlier freezing of the decay. In a subsequent paper [55], it was claimed that such a positive correlation betweenṀ and the final value of µ is supported by some observational evidence [56] [57].…”

mentioning

confidence: 91%

“…Moreover the period distribution for the stiff EoS is much flatter than that for the soft-EoS, displaying a broad maximum at P ∼ 3 ms. It has been recently claimed that X-ray sources in LMBs show rotational periods clustering in the interval 2 → 4 ms [89] [90]. This effect could be explained introducing a fine tuned relation between µ andṀ (µ ∝Ṁ 1/2 [89]).…”

mentioning

confidence: 99%

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Spin and Magnetism in Old Neutron Stars

Colpi

Possenti

Popov

et al. 2001

Lecture Notes in Physics

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Abstract. The thermal, spin and magnetic evolution of neutron stars in the old low mass binaries is first explored. Recycled to very short periods via accretion torques, the neutron stars lose their magnetism progressively. If accretion proceeds undisturbed for 100 Myrs these stars can rotate close to break up with periods far below the minimum observed of 1.558 ms. We investigate their histories using population synthesis models to show that a tail should exist in the period distribution below 1.558 ms. The search of these ultrafastly spinning neutron stars as pulsars can help discriminating among the various equations of state for nuclear matter, and can shed light into the physics of binary evolution.The evolution of isolated neutron stars in the Galaxy is explored beyond the pulsar phase. Moving through the tenuous interstellar medium, these old solitary neutron stars lose their rotational energy. Whether also their magnetism fades is still a mystery. A population synthesis model has revealed that only a tiny fraction of them is able to accrete from the interstellar medium, shining in the X-rays. There is the hope that these solitary stars will eventually appear as faint sources in the Chandra sky survey. This might give insight on the long term evolution of the magnetic field in isolated objects.

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confidence: 91%

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confidence: 99%

Spin and Magnetism in Old Neutron Stars

Colpi

Possenti

Popov

et al. 2001

Lecture Notes in Physics

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“…X-ray burst oscillation sources form two distinct classes: '' fast oscillators,'' with frequencies close to twice the frequency difference of the kHz quasiperiodic oscillations (QPOs) seen in the persistent emission, and '' slow oscillators,'' with frequencies near the difference of the kHz QPO frequencies (White & Zhang 1997). If the kHz QPO frequency difference is close to the spin frequency of the neutron star, then the slow oscillators have a burst oscillation frequency close to the spin frequency, while the fast oscillators produce signals at twice the spin frequency.…”

Section: Introductionmentioning

confidence: 99%

Discovery of X‐Ray Burst Oscillations from a Neutron Star X‐Ray Transient in the Globular Cluster NGC 6440

Kaaret

Zand

Heise

et al. 2003

ApJ

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We report the discovery of millisecond oscillations in an X-ray burst from the X-ray transient SAX J1748.9À2021 in the globular cluster NGC 6440. Oscillations at a frequency of 409:7 AE 0:3 Hz were present in one of 15 X-ray bursts observed with the Proportional Counter Array on the Rossi X-Ray Timing Explorer during the outburst that occurred in 2001. The burst was relatively dim and had the second longest duration and decay time. The average peak luminosity of two bursts showing radius expansion is ð3:6 AE 0:4Þ Â 10 38 ergs s À1 , consistent with the Eddington luminosity for a 1:4 M and 10 km radius neutron star burning hydrogen-poor matter. We speculate that the dichotomy observed between sources with burst oscillations at once versus twice the frequency difference of kHz quasiperiodic oscillations in the persistent emission may be related to the magnetic field geometry of the neutron stars.

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“…These objects underscore the statistically significant absence of pulsars with spins faster than 650 Hz that has been noted previously Chakrabarty 2005). It remains unclear whether this cutoff in the spin distribution reflects the distribution of neutron star magnetic field strengths (e.g., White & Zhang 1997) or angular momentum losses from gravitational radiation (e.g., Wagoner 1984;Bildsten 1998).…”

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confidence: 99%

Discovery of the Accretion-powered Millisecond X-Ray Pulsar IGR J00291+5934

Markwardt

Morgan

Chakrabarty

et al. 2005

ApJ

108

151

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We report on observations of the sixth accretion-powered millisecond pulsar, IGR J00291ϩ5934, with the Rossi X-Ray Timing Explorer. The source is a faint recurrent X-ray transient initially identified by the International Gamma-Ray Astrophysics Laboratory. The 599 Hz (1.67 ms) pulsation had a fractional rms amplitude of 8% in the 2-20 keV range, and its shape was approximately sinusoidal. The pulses show an energy-dependent phase delay, with the 6-9 keV pulses arriving up to 85 ms earlier than those at lower energies. No X-ray bursts, dips, or eclipses were detected. The neutron star is in a circular 2.46 hr orbit with a very low-mass donor, most likely a brown dwarf. The binary parameters of the system are similar to those of the first known accreting millisecond pulsar, SAX J1808.4Ϫ3658. Assuming that the mass transfer is driven by gravitational radiation and that the 2004 outburst fluence is typical, the 3 yr recurrence time implies a distance of at least 4 kpc.

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Millisecond X-Ray Pulsars in Low-mass X-Ray Binaries

Cited by 108 publications

References 21 publications

Spin and Magnetism in Old Neutron Stars

Spin and Magnetism in Old Neutron Stars

Discovery of X‐Ray Burst Oscillations from a Neutron Star X‐Ray Transient in the Globular Cluster NGC 6440

Discovery of the Accretion-powered Millisecond X-Ray Pulsar IGR J00291+5934

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