Limiting rotational period of neutron stars

Glendenning, Norman K.

doi:10.1103/physrevd.46.4161

Cited by 72 publications

(76 citation statements)

References 42 publications

(19 reference statements)

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“…The limiting relation is analogous to a previously obtained lower limit on the Kepler period of a rotating star as a function of its mass ( [10,13]), and to an even earlier analysis of limits on the gravitational redshift from neutron stars ( [14]). …”

Section: Motivationsupporting

confidence: 81%

Lower Limit on Radius as a Function of Mass for Neutron Stars

Glendenning

2000

Phys. Rev. Lett.

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Section: Motivationsupporting

confidence: 81%

Lower Limit on Radius as a Function of Mass for Neutron Stars

Glendenning

2000

Phys. Rev. Lett.

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“…An EOS thus maximizes rotation if it maximizes the gravitational force at the equator of a rotating star -if it allows stars of large mass and small radius. To allow high mass stars, the EOS must be stiff at high density, and for the radius of the high-mass configuration to be small, the EOS must be softer at low density, allowing greater compression in the outer part of the star [46,47]. In our parameter space, a high angular velocity then restricts one to a region with large values of Γ 2 and Γ 3 , and small values of p 1 and Γ 1 .…”

Section: Maximum Spinmentioning

confidence: 99%

Constraints on a phenomenologically parametrized neutron-star equation of state

et al. 2009

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We introduce a parameterized high-density equation of state (EOS) in order to systematize the study of constraints placed by astrophysical observations on the nature of neutron-star matter. To obtain useful constraints, the number of parameters should be smaller than the number of neutronstar properties that have been measured or will have been measured in the next several years. And the set must be large enough to accurately approximate the large set of candidate EOSs. We find that a parameterized EOS based on piecewise polytropes with 3 free parameters matches to about 4% rms error an extensive set of candidate EOSs at densities below the central density of 1.4 M stars. Adding observations of more massive stars constrains the higher density part of the EOS and requires an additional parameter. We obtain constraints on the allowed parameter space set by causality and by present and near-future astronomical observations. In particular, we emphasize potentially stringent constraints on the EOS parameter space associated with two measured properties of a single star; and we find that a measurement of the moment of inertia of PSR J0737-3039A can strongly constrain the maximum neutron-star mass. We also present in an appendix a more efficient algorithm than has previously been used for finding points of marginal stability and the maximum angular velocity of stable stars.

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“…The region to the left of the Pt = 0.65 MeV fm −3 curve is forbidden if Vela glitches are due to angular momentum transfers between the crust and core, as discussed in Link, Epstein & Lattimer [94]. For comparison, the region excluded by causality alone lies to the left of the dashed curve labelled "causality" as determined by Lattimer et al [93] and Glendenning [113] constraint ∆I/I ≥ 0.014: R > 3.9 + 3.5M/M ⊙ − 0.08(M/M ⊙ ) 2 km .…”

Section: Crustal Fraction Of the Moment Of Inertiamentioning

confidence: 99%

Evolution of a Neutron Star from Its Birth to Old Age

Prakash

Lattimer

Pons

et al. 2001

Lecture Notes in Physics

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Abstract. The main stages in the evolution of a neutron star, from its birth as a proto-neutron star, to its old age as a cold, catalyzed configuration, are described. A proto-neutron star is formed in the aftermath of a successful supernova explosion and its evolution is dominated by neutrino diffusion. Its neutrino signal is a valuable diagnostic of its internal structure and composition. During its transformation from a hot, leptonrich to a cold, catalyzed remnant, the possibility exists that it can collapse into a black hole, which abruptly terminates neutrino emissions. The essential microphysics, reviewed herein, that controls its evolution are the equation of state of dense matter and its associated neutrino opacities. Several simulations of the proto-neutron star evolution, involving different assumptions about the composition of dense matter, are described. After its evolution into a nearly isothermal neutron star a hundred or so years after its birth, it may be observable through its thermal emission in X-rays during its life in the next million years. Its surface temperature will depend upon the rapidity of neutrino emission processes in its core, which depends on the composition of dense matter and whether or not its constituents exhibit superfluidity and superconductivity. Observations of thermal emission offer the best hope of a determination of the radius of a neutron star. The implications for the underlying dense matter equation of state of an accurate radius determination are explored.

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Limiting rotational period of neutron stars

Cited by 72 publications

References 42 publications

Lower Limit on Radius as a Function of Mass for Neutron Stars

Lower Limit on Radius as a Function of Mass for Neutron Stars

Constraints on a phenomenologically parametrized neutron-star equation of state

Evolution of a Neutron Star from Its Birth to Old Age

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