Hybrid Stars that Masquerade as Neutron Stars

Alford, Mark; Braby, Matt; Paris, Mark W.; Reddy, Sanjay

doi:10.1086/430902

Cited by 713 publications

(758 citation statements)

References 60 publications

(75 reference statements)

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“…The second term on the right hand side of Eq. (1) accounts for the perturbative QCD corrections to O(α 2 s ) (Fraga et al 2001;Alford et al 2005;Weissenborn et al 2011) and its value represents the degree of deviations from an ideal relativistic Fermi gas EoS, with a4 = 1 corresponding to the ideal gas. The baryon chemical potential µ b can be written in terms of the u, d and s quark chemical potentials as µ b = µu + µ d + µs.…”

Section: The Modified Bag Model Equation Of State For Strange Quark Mmentioning

confidence: 99%

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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: The Modified Bag Model Equation Of State For Strange Quark Mmentioning

confidence: 99%

“…The modified bag model EoS has already been used to calculate the structure of non-spinning strange stars (Fraga et al 2001;Alford et al 2005;Weissenborn et al 2011;Fraga et al 2014) and hybrid stars (Alford et al 2005;Weissenborn et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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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“…The reason is that even for the matter densities achievable in compact stars we expect that QCD is non perturbative. Nonetheless, it is reasonable to expect that at sufficiently large densities the grand potential is a function of the average baryon chemical potential, μ, and a Taylor expansion gives [15] …”

Section: Equilibrium Configurationsmentioning

confidence: 99%

“…where a 4 , a 2 and B eff are independent of μ; see [15] for a discussion of the relevant range of values of each parameter. In order to take into account the impact of the uncertainty of these coefficients on our results, we consider two extreme situations, namely A (a 4 = 0.7, a 2 = (200 MeV) 2 and B eff = (165 MeV) 4 ) and B (a 4 = 0.7, a 2 = 0 and B eff = (145 MeV) 4 ).…”

Section: Equilibrium Configurationsmentioning

confidence: 99%

Torsional oscillations of strange stars

Mannarelli

2014

EPJ Web of Conferences

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Abstract. Strange stars are one of the hypothetical compact stellar objects that can be formed after a supernova explosion. The existence of these objects relies on the absolute stability of strange collapsed quark matter with respect to standard nuclear matter. We discuss simple models of strange stars with a bare quark matter surface, thus standard nuclear matter is completely absent. In these models an electric dipole layer a few hundreds Fermi thick should exist close to the star surface. Studying the torsional oscillations of the electrically charged layer we estimate the emitted power, finding that it is of the order of 10 45 erg/s, meaning that these objects would be among the brightest compact sources in the heavens. The associated relaxation times are very uncertain, with values ranging between microseconds and minutes, depending on the crust thickness. Although part of the radiated power should be absorbed by the electrosphere surrounding the strange star, a sizable fraction of photons should escape and be detectable.

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“…Massive stable compact stars with color-superconducting cores were obtained only in a few studies prior to these observations (Alford et al 2005;Ippolito et al 2008;Knippel & Sedrakian 2009;Agrawal & Dhiman 2009;Kurkela et al 2010). Rotating configurations of colorsuperconducting stars were previously constructed by Ippolito et al (2008); however, evolutionary aspects of the problem were not discussed so far.…”

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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Hybrid Stars that Masquerade as Neutron Stars

Cited by 713 publications

References 60 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

Torsional oscillations of strange stars

Rotating hybrid compact stars

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