Diagnosis and Monitoring of Primary Angle Closure

Sudhakar, R.; Chen, Lian

doi:10.1007/s40135-015-0063-y

Cited by 25 publications

(27 citation statements)

References 57 publications

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“…However, as the observations, evolutionary arguments, and numerical simulations tend to suggest, NS that become radio pulsars are not born with ∼1 -3 ms periods, but with much longer periods of ∼20 − 150 ms, see Faucher-Giguère & Kaspi (2006), Kramer et al (2003), Table 7.6 in Lyne & Graham-Smith (1998), and references therein (a specific class of NS with millisecond periods at birth in massive core-collapse supernovae are thought to be progenitors of magnetars, which are observed as soft-gamma ray repeaters or anomalous X-ray pulsars, see e.g., Kargaltsev & Pavlov 2008). Then, after slowing down to a period of a few seconds and entering the pulsar graveyard, they gain their angular momentum, as well as mass, during long-term accretion processes in low-mass binary systems (in the so-called recycling of dead pulsars, see Alpar et al 1982;Radhakrishnan & Srinivasan 1982;Wijnands & van der Klis 1998), and it is possible that some of them enter the strong phase transition instability strip sometime in their evolution. Sufficiently massive and sufficiently rapidly rotating NS will then migrate dynamically along the M b = const.…”

Section: Discussionmentioning

confidence: 99%

Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars

Bejger

Blaschke

Haensel

et al. 2017

A&A

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Aims. We explore the implications of a strong first-order phase transition region in the dense matter equation of state in the interiors of rotating neutron stars, and the resulting creation of two disjoint families of neutron-star configurations (the so-called high-mass twins). Methods. We numerically obtained rotating, axisymmetric, and stationary stellar configurations in the framework of general relativity, and studied their global parameters and stability. Results. The instability induced by the equation of state divides stable neutron star configurations into two disjoint families: neutron stars (second family) and hybrid stars (third family), with an overlapping region in mass, the high-mass twin-star region. These two regions are divided by an instability strip. Its existence has interesting astrophysical consequences for rotating neutron stars. We note that it provides a natural explanation for the rotational frequency cutoff in the observed distribution of neutron star spins, and for the apparent lack of back-bending in pulsar timing. It also straightforwardly enables a substantial energy release in a mini-collapse to another neutron-star configuration (core quake), or to a black hole.

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Section: Discussionmentioning

confidence: 99%

Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars

Bejger

Blaschke

Haensel

et al. 2017

A&A

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“…These are believed to be old NS that have been "recycled" i.e. spun-up to millisecond periods by the accretion of matter from a binary companion [31,32].…”

Section: Spin Frequencymentioning

confidence: 99%

Rotating neutron stars with exotic cores: masses, radii, stability

Haensel¹,

Bejger²,

Fortin³

et al. 2016

Eur. Phys. J. A

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Abstract.A set of theoretical mass-radius relations for rigidly rotating neutron stars with exotic cores, obtained in various theories of dense matter, is reviewed. Two basic observational constraints are used: the largest measured rotation frequency (716 Hz) and the maximum measured mass (2M ). The present status of measuring the radii of neutron stars is described. The theory of rigidly rotating stars in general relativity is reviewed and limitations of the slow rotation approximation are pointed out. Mass-radius relations for rotating neutron stars with hyperon and quark cores are illustrated using several models. Problems related to the non-uniqueness of the crust-core matching are mentioned. Limits on rigid rotation resulting from the mass-shedding instability and the instability with respect to the axisymmetric perturbations are summarized. The problem of instabilities and of the back-bending phenomenon are discussed in detail. Metastability and instability of a neutron star core in the case of a first-order phase transition, both between pure phases, and into a mixed-phase state, are reviewed. The case of two disjoint families (branches) of rotating neutron stars is discussed and generic features of neutron-star families and of core-quakes triggered by the instabilities are considered.

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“…If the accretor was a neutron star it may have been spun up by accreting angular momentum along with mass. This spinup can cause the neutron star to turn on again as a radio pulsar, a process known as recycling (Radhakrishnan & Srinivasan, 1982). However if almost all the mass reaches the neutron star in super-Eddington outbursts, the efficiency of both mass and angular momentum gain will be extremely low.…”

Section: Long-period Sxtsmentioning

confidence: 99%

Accretion in compact binaries

King

2006

Compact Stellar X-Ray Sources

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Contents1 Accretion in Compact Binaries page 1.1 Introduction 1.2 Accretion disc theory 1.3 Dwarf novae: the nature of the outbursts 1.4 Dwarf novae: the occurrence of the outbursts 1.5 Soft X-ray transients: the nature of the outbursts 1.6 Soft X-ray transients: the occurrence of the outbursts 1.7 Quiescent transients and black hole horizons 1.8 Ultraluminous X-ray sources 1.9 Conclusions References i

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Diagnosis and Monitoring of Primary Angle Closure

Cited by 25 publications

References 57 publications

Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars

Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars

Rotating neutron stars with exotic cores: masses, radii, stability

Accretion in compact binaries

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