Type II critical phenomena of neutron star collapse

Noble, Scott C.; Choptuik, Matthew W.

doi:10.1103/physrevd.78.064059

Cited by 18 publications

(35 citation statements)

References 42 publications

(118 reference statements)

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“…As discussed in section 4.1, the central rest-mass density of the linearly unstable models can be used as a critical parameter for the gravitational collapse of a linearly unstable spherical star, in contrast to what has been observed for example by Novak in [7] or by Noble and Choptuik in [9]. We believe that this is due to the very different set of initial data selected here and in [7,9].…”

Section: Perturbation Of Nearly Critical Solutionsmentioning

confidence: 78%

“…He confirmed the observation by Novak that a minimum mass is required to trigger collapse and also found that, for very high mass spherical stars, a type I critical phenomenon is observed with each model oscillating around a corresponding solution on the unstable branch. More recently, Noble and Choptuik [9] performed an accurate study using the same setup of [7] and were able to show that, even for initial data of spherical stars, the scaling exponent in the mass relation law is compatible with the exponent in the corresponding ultra-relativistic case.…”

Section: Introductionmentioning

confidence: 93%

“…Conversely, the spherical stars considered in the above-mentioned works were evolved using either an ultra-relativistic EOS [5] (which, as commented in the Introduction, are intrinsically 5 In our notation, the point {U 0 , ρ * c (U 0 )} is the critical solution with initial velocity perturbation given by equation (19) with U = U 0 . Similarly, a configuration {U 0 , ρ * c (0)} will be a member of the family with initial velocity perturbation U 0 , but with a central density which is the critical one for a model with U = 0. scale-free) or with very strong perturbations [7,9], thus in a regime of the EOS which is approximatively ultra-relativistic [13].…”

Section: Perturbation Of Nearly Critical Solutionsmentioning

confidence: 99%

See 2 more Smart Citations

Critical phenomena in neutron stars: I. Linearly unstable nonrotating models

Radice¹,

Rezzolla²,

Kellerman³

2010

Class. Quantum Grav.

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We consider the evolution in full general relativity of a family of linearly unstable isolated spherical neutron stars under the effects of very small perturbations as induced by the truncation error. Using a simple idealfluid equation of state, we find that this system exhibits a type I critical behaviour, thus confirming the conclusions reached by Liebling et al (2010 arXiv:1001.0575v1) for rotating magnetized stars. Exploiting the relative simplicity of our system, we are able to carry out a more in-depth study providing solid evidence of the criticality of this phenomenon and also to give a simple interpretation of the putative critical solution as a spherical solution with the unstable mode being the fundamental F-mode. Hence for any choice of the polytropic constant, the critical solution will distinguish the set of subcritical models migrating to the stable branch of the models of equilibrium from the set of subcritical models collapsing to a black hole. Finally, we study how the dynamics changes when the numerical perturbation is replaced by a finitesize, resolution-independent velocity perturbation and show that in such cases a nearly critical solution can be changed into either a sub-or supercritical one. The work reported here also lays the basis for the analysis carried in a companion paper, where the critical behaviour in the head-on collision of two neutron stars is instead considered (Kellerman et al 2010 Class. Quantum Grav. 27 235016).

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Section: Perturbation Of Nearly Critical Solutionsmentioning

confidence: 78%

Section: Introductionmentioning

confidence: 93%

Section: Perturbation Of Nearly Critical Solutionsmentioning

confidence: 99%

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Critical phenomena in neutron stars: I. Linearly unstable nonrotating models

Radice¹,

Rezzolla²,

Kellerman³

2010

Class. Quantum Grav.

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“…The Choptuik scaling has been discussed in the context of AdS/CFT in recent works [42][43][44][45]. The analogue of Choptuik scaling has been observed in the (driven) collapse of neutron stars [46,47], 41 so it would presumably be relevant for the collapse of our star and might have an interesting interpretation in the dual gauge theory. 40 We are always working in the microcanonical ensemble so the total energy is conserved.…”

Section: Discussionmentioning

confidence: 98%

Degenerate stars and gravitational collapse in AdS/CFT

Arsiwalla

Boer

Papadodimas

et al. 2011

J. High Energ. Phys.

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We construct composite CFT operators from a large number of fermionic primary fields corresponding to states that are holographically dual to a zero temperature Fermi gas in AdS space. We identify a large N regime in which the fermions behave as free particles. In the hydrodynamic limit the Fermi gas forms a degenerate star with a radius determined by the Fermi level, and a mass and angular momentum that exactly matches the boundary calculations. Next we consider an interacting regime, and calculate the effect of the gravitational back-reaction on the radius and the mass of the star using the Tolman-Oppenheimer-Volkoff equations. Ignoring other interactions, we determine the "Chandrasekhar limit" beyond which the degenerate star (presumably) undergoes gravitational collapse towards a black hole. This is interpreted on the boundary as a high density phase transition from a cold baryonic phase to a hot deconfined phase.

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“…Here, σ denotes the time scaling exponent, which controls the sharpness of the threshold behaviour near black hole A thorough investigation of the critical collapse dynamics of low-mass neutron stars has been presented in [13], where the scaling behaviour of black hole formation was studied. This letter aims to extend the previous work in [5][6][7]13] and to investigate radial oscillations of large amplitudes in the vicinity of the maximum-mass configuration, taking into account non-linear effects. Specifically, we want to address the question, how strong the perturbation should be, in order to traverse the barrier and cause a collapse to a black hole (see fig.…”

Section: Introductionmentioning

confidence: 99%

Nonlinear oscillations of compact stars in the vicinity of the maximum mass configuration

Brillante

Mishustin

2015

EPL

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We solve the dynamical GR equations for the spherically symmetric evolution of compact stars in the vicinity of the maximum mass, for which instability sets in according to linear perturbation theory. The calculations are done with the analytical Zeldovich-like EOS P = a (ρ − ρ 0 ) and with the TM1 parametrisation of the RMF model. The initial configurations for the dynamical calculations are represented by spherical stars with equilibrium density profile, which are perturbed by either (i) an artificially added inward velocity field proportional to the radial coordinate, or (ii) a rarefaction corresponding to a static and expanded star. These configurations are evolved using a one-dimensional GR hydro code for ideal and barotropic fluids.Depending on the initial conditions we obtain either stable oscillations or the collapse to a black hole. The minimal amplitude of the perturbation, needed to trigger gravitational collapse is evaluated. The approximate independence of this energy on the type of perturbation is pointed out. At the threshold we find type I critical behaviour for all stellar models considered and discuss the dependence of the time scaling exponent on the baryon mass and EOS.

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Type II critical phenomena of neutron star collapse

Cited by 18 publications

References 42 publications

Critical phenomena in neutron stars: I. Linearly unstable nonrotating models

Critical phenomena in neutron stars: I. Linearly unstable nonrotating models

Degenerate stars and gravitational collapse in AdS/CFT

Nonlinear oscillations of compact stars in the vicinity of the maximum mass configuration

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