Rapidly rotating neutron stars in general relativity: Realistic equations of state

Cook, G.G.; Shapiro, Stuart L.; Teukolsky, Saul A.

doi:10.1086/173934

Cited by 630 publications

(759 citation statements)

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“…and a unit time-like description for the four velocity vector we can decompose the Einstein field equations projected onto the frame of reference of a Zero Angular Momentum Observer (ZAMO) to yield three elliptic equations for γ, ρ and ω and a linear ordinary differential equation for α (Cook et al 1994). The elliptic equations are then converted to integral equations using the Green's function approach.…”

Section: Computation Of Rapidly Spinning Stellar Structuresmentioning

confidence: 99%

“…In addition to this instability limit, there are three other limits: (1) the static or nonspinning limit, where ν → 0 and J → 0; (2) the mass-shed limit, at which the compact star spins too fast to keep matter bound to the surface; and (3) the low-mass limit, below which a compact star cannot form. These four limits together define the stable stellar parameter space for an EoS model (Cook et al 1994). Here, apart from the instability limit, we calculate the static and massshed limit sequences, but we do not attempt to determine the low-mass limit, where the numerical solutions are less accurate (Cook et al 1994).…”

Section: Computation Of Rapidly Spinning Stellar Structuresmentioning

confidence: 99%

“…These four limits together define the stable stellar parameter space for an EoS model (Cook et al 1994). Here, apart from the instability limit, we calculate the static and massshed limit sequences, but we do not attempt to determine the low-mass limit, where the numerical solutions are less accurate (Cook et al 1994). …”

Section: Computation Of Rapidly Spinning Stellar Structuresmentioning

confidence: 99%

See 2 more Smart Citations

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Bhattacharyya

Bombaci

Logoteta

et al. 2016

Mon. Not. R. Astron. Soc.

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For a set of equation of state (EoS) models involving interacting strange quark matter, characterized by an effective bag constant (B eff ) and a perturbative QCD corrections term (a 4 ), we construct fully general relativistic equilibrium sequences of rapidly spinning strange stars for the first time. Computation of such sequences is important to study millisecond pulsars and other fast spinning compact stars. Our EoS models can support a gravitational mass (M G ) and a spin frequency (ν) at least up to ≈ 3.0M ⊙ and ≈ 1250 Hz respectively, and hence are fully consistent with measured M G and ν values. This paper reports the effects of B eff and a 4 on measurable compact star properties, which could be useful to find possible ways to constrain these fundamental quark matter parameters, within the ambit of our EoS models. We confirm that a lower B eff allows a higher mass. Besides, for known M G and ν, measurable parameters, such as stellar radius, radius-to-mass ratio and moment of inertia, increase with the decrease of B eff . Our calculations also show that a 4 significantly affects the stellar rest mass and the total stellar binding energy. As a result, a 4 can have signatures in evolutions of both accreting and non-accreting compact stars, and the observed distribution of stellar mass and spin and other source parameters. Finally, we compute the parameter values of two important pulsars, PSR J1614-2230 and PSR J1748-2446ad, which may have implications to probe their evolutionary histories, and for constraining EoS models.

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Section: Computation Of Rapidly Spinning Stellar Structuresmentioning

confidence: 99%

Section: Computation Of Rapidly Spinning Stellar Structuresmentioning

confidence: 99%

Section: Computation Of Rapidly Spinning Stellar Structuresmentioning

confidence: 99%

See 1 more Smart Citation

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Bhattacharyya

Bombaci

Logoteta

et al. 2016

Mon. Not. R. Astron. Soc.

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“…This allows us to obtain an approximate set of trajectories by using null geodesics of the Kerr metric. For our chosen pulsar period, mass and radius, we estimate appropriate values for a(\J/M) using the numerical models calculated by Cook, Shapiro, & Teukolsky (1994). We adopt a \ 0.47/P (ms) measured in units of M as appropriate to their moderately soft "" FPS ÏÏ model at M \ 1.4 M _ and low…”

Section: Kerr Propagationmentioning

confidence: 99%

Light Curves of Rapidly Rotating Neutron Stars

Braje

Romani

Rauch

2000

ApJ

116

106

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We consider the e †ect of rapid rotation on the light curves of neutron stars with hot polar caps. For P B 3 ms spin periods, the pulse fractions can be as much as an order of magnitude larger than with simple, slowly rotating (Schwarzschild) estimates. Doppler boosting, in particular, leads to characteristic distortion and "" soft lags ÏÏ in the pulse proÐles, which are easily measurable in light curves with moderate energy resolution. With D105 photons it should also be possible to isolate the more subtle distortions of light travel time variations and frame dragging. Detailed analysis of high-quality millisecond pulsar data from upcoming X-ray missions must include these e †ects.

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“…The dashed line shows the gravitational mass corresponding to a rest mass of 1.4 M⊙ if the binding energy per mass is uniform throughout a star and equal to its surface value. In practice, this provides a strong lower limit to the gravitational mass (see, e.g., the numerical calculations of Cook, Shapiro, & Teukolsky 1994).…”

Section: Results: Vela X-1mentioning

confidence: 99%

Constraints on Superdensematter From X-Ray Binaries

Miller

2006

NATO Science Series II: Mathematics, Physics and Chemistry

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From the earliest measurements of the masses of binary pulsars, observations of neutron stars have placed interesting constraints on the properties of high-density matter. The last few years have seen a number of observational developments that could place strong new restrictions on the equilibrium state of cold matter at supranuclear densities. We review these astronomical constraints and their context, and speculate on future prospects.

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Rapidly rotating neutron stars in general relativity: Realistic equations of state

Cited by 630 publications

References 0 publications

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Light Curves of Rapidly Rotating Neutron Stars

Constraints on Superdensematter From X-Ray Binaries

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