Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down

Glendenning, Norman K.; Pei, Shouyong; Weber, Fridolin

doi:10.1103/physrevlett.79.1603

Cited by 171 publications

(230 citation statements)

References 25 publications

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“…6. The apparently "backbending branch" in lower panel, as defined in the previous work (Glendenning et al 1997), consists mostly of configurations unstable with respect to axial perturbations. The BC segment is astrophysically irrelevant, and the B point correspond to an unstable termination of the back-bending branch (see Sect.…”

Section: Back-bending Phenomenonmentioning

confidence: 99%

“…The softening of the EOS could be due to a transition into a pure "exotic" phase, or to a mixture of an "exotic" phase with normal phase of dense matter. It has been suggested that the softening of the EOS due to a phase transition could lead to characteristic backbending phenomenon in the timing of spinning-down pulsars (Glendenning et al 1997) or produce characteristic period clustering in spinning-up neutron stars in low-mass X-ray binaries (Glendenning 2001;Glendenning & Weber 2002). An interesting conclusion of these papers was that both back-bending in spinning down pulsar and spin clustering in accreting millisecond pulsars stars is evidence of a phase transition taking place at the center of a spinning-down pulsar or a spinning-up accreting neutron star.…”

Section: Introductionmentioning

confidence: 99%

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Hyperon softening of the EOS of dense matter and the spin evolution of isolated neutron stars

Zdunik¹,

Haensel²,

Gourgoulhon³

et al. 2004

A&A

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Abstract. The effect of the hyperon softening of the equation of state (EOS) of dense matter on the spin evolution of isolated neutron stars is studied for a broad set of hyperonic EOSs. We use a multidomain 2-D code based on a spectral method, and show how important the precision of solving the equations of stationary motion is for the stability analysis. For some EOSs, the hyperon softening leads to spin-up by angular momentum loss, in the form of the back-bending phenomenon, for a rather broad range of stellar baryon mass. We show that large segments of the evolutionary tracks exhibiting the back-bending behaviour in the moment-of-inertia -rotation-frequency plane are unstable and therefore not astrophysically relevant. We show also that during the spin-up -angular-momentum-loss epoch, an isolated neutron star (e.g. a radio pulsar) can lose a sizable part of its initial angular momentum without significantly changing its rotation period. We propose also simple arguments and criteria allowing one to connect the presence of a back-bending epoch with the mass-radius relations and the stiffness and/or softness of the nucleon and hyperon EOSs of the neutron star core.

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Section: Back-bending Phenomenonmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Hyperon softening of the EOS of dense matter and the spin evolution of isolated neutron stars

Zdunik¹,

Haensel²,

Gourgoulhon³

et al. 2004

A&A

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show abstract

“…In contrast, the density jump associated with a strong first-order phase transition may cause sudden changes in the integral parameters of stars. Previous work concentrated on the phase transition to normal quark matter (Glendenning et al 1997;Chubarian et al 2000;Glendenning & Weber 2001;Spyrou & Stergioulas 2002;Grigorian et al 2003;Zdunik et al 2006;Dimmelmeier et al 2009;Abdikamalov et al 2009;Haensel et al 2009;Weber et al 2013). Contrary to this, we argue here that the transition for sufficiently cold stars occurs to one of the color-superconducting phases of quark matter.…”

Section: Phase Transition To a Color-superconducting State Via Spin Umentioning

confidence: 99%

“…A&A 559, A118 (2013) evolution of purely nucleonic stars. Because the spin-down compresses the matter within the star, it can induce a phase transition to the quark-matter phase once the critical density of the phase transition has been reached (Glendenning et al 1997;Chubarian et al 2000;Glendenning & Weber 2001;Spyrou & Stergioulas 2002;Grigorian et al 2003;Zdunik et al 2006;Dimmelmeier et al 2009;Abdikamalov et al 2009;Haensel et al 2009;Weber et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Rotating hybrid compact stars

Ayvazyan

Colucci

Rischke

et al. 2013

A&A

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Starting from equations of state of nucleonic and color-superconducting quark matter and assuming a first-order phase transition between these, we construct an equation of state of stellar matter, which contains three phases: a nucleonic phase, as well as twoflavor and three-flavor color-superconducting phases of quarks. Static sequences of the corresponding hybrid stars include massive members with masses of ∼2 M and radii in the range of 13 ≤ R ≤ 16 km. We investigate the integral parameters of rapidly rotating stars and obtain evolutionary sequences that correspond to constant rest-mass stars spinning down by electromagnetic and gravitational radiation. Physically new transitional sequences are revealed that are distinguished by a phase transition from nucleonic to color-superconducting matter for some configurations that are located between the static and Keplerian limits. The snapshots of internal structure of the star, displaying the growth or shrinkage of superconducting volume as the star's spin changes, are displayed for constant rest mass stars. We further obtain evolutionary sequences of rotating supramassive compact stars and construct pre-collapse models that can be used as initial data to simulate a collapse of color-superconducting hybrid stars to a black hole.

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“…[86] it was pointed out that since the compressibility of normal nuclear matter phase and the deconfined (almost free Fermi gas) of the QGP are different (the incompressibility of normal nuclear matter is greater than that of an almost free Fermi gas of quarks) a structural change will occur upon a change in frequency. This has important consequences in the spin-up or spin-down stages of millisecond pulsars [86,48]. As a millisecond pulsar spins-down, its central density may rise above the critical density for the QGP phase transition in dense nuclear matter and the central core changes to a phase with a softer equation of state.…”

Section: Qgp In the Core Of Pulsarsmentioning

confidence: 99%

Phase transitions in the early and the present Universe: from the big bang to heavy ion collisions

Boyanovsky

2001

Phase Transitions in the Early Universe: Theory and Observations

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In these lectures I discuss cosmological phase transitions with the goal of establishing the possibility of observational consequences. I argue that the only phase transition amenable of experimental study within the foreseeable future is that predicted by QCD and discuss some of the potential observational cosmological consequences associated with this phase transition(s). I describe the experimental effort to study the QCD phase transition(s) at RHIC and SPS and summarize some of the recent experimental results. The possibility of novel phases of QCD in the core of pulsars is discussed along with the suggested observational consequences. A brief review of standard big bang cosmology as well as the astrophysics of compact stars sets the stage for understanding the observational cosmological and astrophysical consequences of phase transitions in the standard model.

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Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down

Cited by 171 publications

References 25 publications

Hyperon softening of the EOS of dense matter and the spin evolution of isolated neutron stars

Hyperon softening of the EOS of dense matter and the spin evolution of isolated neutron stars

Rotating hybrid compact stars

Phase transitions in the early and the present Universe: from the big bang to heavy ion collisions

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