Rotating stars in relativity

Paschalidis, Vasileios; Stergioulas, Nikolaos

doi:10.1007/s41114-017-0008-x

Cited by 194 publications

(163 citation statements)

References 799 publications

(1,062 reference statements)

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“…6b and Eq. (15), that if we have a measurement of moment of inertia, or compactness parameter, we could extract the interval where the other parameter can lie. An average empirical relation had been also created, given by the expression As a consequence, by constraining simultaneously these two quantities, we could impose strong constraints on the radius of neutron stars, which still remains an open problem.…”

Section: B Moment Of Inertia and Eccentricitymentioning

confidence: 99%

Effects of the equation of state on the bulk properties of maximally rotating neutron stars

Koliogiannis

Moustakidis

2020

Phys. Rev. C

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Neutron stars are among the densest known objects in the universe and an ideal laboratory for the strange physics of super-condensed matter. While the simultaneously measurement of mass and radius of non-rotating neutron stars may impose strong constraints on the properties of the dense nuclear matter, the observation and study of rapidly-rotating ones, close to the mass-shedding limit, may lead to significantly further constraints. Theoretical predictions allow neutron stars to rotate extremely fast (even more than 2000 Hz). However, until this moment, the fastest observed rotating pulsar has a frequency of 716 Hz, much lower compared to the theoretical predictions. There are many suggestions for the mechanism that leads to this situation. In any case, the theoretical study of uniformly rotating neutron stars, along with the accurate measurements, may offer rich information concerning the constraints on the high density part of the equation of state. In addition, neutron stars through their evolution, may provide us with a criteria to determine the final fate of a rotating compact star. Sensitivity of bulk neutron stars properties on the equation of state at the mass-shedding limit, are the main subject of the present study.

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Section: B Moment Of Inertia and Eccentricitymentioning

confidence: 99%

Effects of the equation of state on the bulk properties of maximally rotating neutron stars

Koliogiannis

Moustakidis

2020

Phys. Rev. C

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“…We have constructed the maximum mass configuration (we consider that to a very good accuracy this configuration is identified with the maximum permitted rotational frequency (Keplerian velocity) [5,6]) by considering the following two structures for the neutron star EoS: a) Maximum angular velocity for known low-density EoS b) Maximum angular velocity from the relativistic kinetic theory…”

Section: Speed Of Sound Bounds and Maximum Mass Configurationmentioning

confidence: 99%

Speed of sound constraints on maximally rotating neutron stars

2020

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The observation of maximally-rotating neutron stars (in comparison with non-rotating ones) may provide more information on the behavior of nuclear matter at high densities. In the present work we provide a theoretical treatment concerning the effects of the upper bound of the sound speed in dense matter on the bulk properties of maximally-rotating (at mass-shedding limit) neutron stars. In particular, we consider two upper bounds for the speed of sound, vs = c and vs = c/ √ 3, and the one provided by the relativistic kinetic theory. We investigate to what extent the possible predicted (from various theories and conjectures) upper bounds on the speed of sound constrain the ones of various key quantities, including the maximum mass and the corresponding radius, Keplerian frequency, Kerr parameter and moment of inertia. We mainly focus on the lower proposed limit, vs = c/ √ 3, and we explore in which mass region a rotating neutron star collapses to a black hole. In any case, useful relations of the mentioned bulk properties with the transition density are derived and compared with the corresponding non-rotating cases. We concluded that the proposed limit vs = c/ √ 3 leads to dramatic decrease on the values of the maximum mass, Kerr parameter and moment of inertia preventing a neutron star to reach values which derived with the consideration of realistic equations of state or from other constraints. Possible measurements of the Kerr parameter and moment of inertia would shed light on these issues and help to reveal the speed of sound bound in dense matter.

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“…Despite the enormous amount of work done in the field of rotating stars [14,15] full general relativistic (GR) numerical simulations that investigate the stability and accurately quantify the GW signature of single, uniformly rotating, triaxial stars have not been performed. One of the reasons is the scarcity of accurate initial models needed to study their evolution.…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave content and stability of uniformly, rotating, triaxial neutron stars in general relativity

et al. 2017

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Targets for ground-based gravitational wave interferometers include continuous, quasiperiodic sources of gravitational radiation, such as isolated, spinning neutron stars. In this work we perform evolution simulations of uniformly rotating, triaxially deformed stars, the compressible analogues in general relativity of incompressible, Newtonian Jacobi ellipsoids. We investigate their stability and gravitational wave emission. We employ five models, both normal and supramassive, and track their evolution with different grid setups and resolutions, as well as with two different evolution codes. We find that all models are dynamically stable and produce a strain that is approximately one-tenth the average value of a merging binary system. We track their secular evolution and find that all our stars evolve towards axisymmetry, maintaining their uniform rotation, kinetic energy, and angular momentum profiles while losing their triaxiality.

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Rotating stars in relativity

Cited by 194 publications

References 799 publications

Effects of the equation of state on the bulk properties of maximally rotating neutron stars

Effects of the equation of state on the bulk properties of maximally rotating neutron stars

Speed of sound constraints on maximally rotating neutron stars

Gravitational wave content and stability of uniformly, rotating, triaxial neutron stars in general relativity

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