Lower Limit on Radius as a Function of Mass for Neutron Stars

Glendenning, Norman K.

doi:10.1103/physrevlett.85.1150

Cited by 25 publications

(22 citation statements)

References 21 publications

(25 reference statements)

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“…The matter of star satisfies dP/dρ ≥ 0 which is a necessary condition of a stable body both as a whole and also with respect to the non-equilibrium elementary regions with spontaneous contraction or expansion (Le Chatelier's principle) [115]. As one can see, in Fig.…”

Section: Le Chatelier's Principlementioning

confidence: 97%

Neutron stars structure in the context of massive gravity

Hendi

Bordbar

Panah

et al. 2017

J. Cosmol. Astropart. Phys.

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Motivated by the recent interests in spin−2 massive gravitons, we study the structure of neutron star in the context of massive gravity. The modifications of TOV equation in the presence of massive gravity are explored in 4 and higher dimensions. Next, by considering the modern equation of state for the neutron star matter (which is extracted by the lowest order constrained variational (LOCV) method with the AV18 potential), different physical properties of the neutron star (such as Le Chatelier's principle, stability and energy conditions) are investigated. It is shown that consideration of the massive gravity has specific contributions into the structure of neutron star and introduces new prescriptions for the massive astrophysical objects. The mass-radius relation is examined and the effects of massive gravity on the Schwarzschild radius, average density, compactness, gravitational redshift and dynamical stability are studied. Finally, a relation between mass and radius of neutron star versus the Planck mass is extracted.

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Section: Le Chatelier's Principlementioning

confidence: 97%

Neutron stars structure in the context of massive gravity

Hendi

Bordbar

Panah

et al. 2017

J. Cosmol. Astropart. Phys.

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“…It was found in Li et al [5] that the star 4U 1728−34 may have a mass less than that of the SAX and yet have a smaller radius. Another serious difference is that the EOS of D98, using the formalism of large N c approximation, indeed shows a bound state in the sense of having a minimum at about 4.8 n 0 , whereas in Glendenning [24] one of the assumptions is that strange matter has no bound state.…”

Section: Introductionmentioning

confidence: 99%

“…Recently Glendenning [24] has argued that the SAX could be explained as a neutron star rather than a bare SS, not with any of the existing known EOS, but with a hypothetical one, satisfying however, the well-accepted restrictions based on general physical principles and having a core density about 26 ρ 0 . Of course, such high density cores imply hybrid strange stars, subject to Glendenning's assumption that such stars can exist with matching EOS for two phases.…”

Section: Introductionmentioning

confidence: 99%

Stability of Strange Stars (Ss) Derived From a Realistic Equation of State

Sinha

Dey

et al. 2002

Mod. Phys. Lett. A

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A realistic EOS (equation of state) leads to strange stars (ReSS) which are compact in the mass radius plot, close to the Schwarzchild limiting line [1]. Many of the observed stars fit in with this kind of compactness, irrespective of whether they are X-ray pulsars, bursters or soft γ repeaters or even radio pulsars. We point out that a change in the radius of a star can be small or large, when its mass is increasing and this depends on the position of a particular star on the mass radius curve. We carry out a stability analysis against radial oscillations and compare with the EOS of other SS models. We find that the ReSS is stable and an M-R region can be identified to that effect.

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“…The pulsar SAX J1808.4-3658, with a rotation period of 2.5 ms, is the fastest spinning x-ray pulsar ever observed. Based on a study of its mass-radius relation it has been concluded that SAX J1808.4-3658 is a likely strange-star candidate [6], although this interpretation remains controversial [7,8]. Still, the discovery of such a fastly-rotating pulsar appears to have made the detection of strange matter within observational reach.…”

Section: Introductionmentioning

confidence: 99%

Modeling the strangeness content of hadronic matter

Sánchez

Piekarewicz

2002

Phys. Rev. C

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The strangeness content of hadronic matter is studied in a string-flip model that reproduces various aspects of the QCD-inspired phenomenology, such as quark clustering at low density and color deconfinement at high density, while avoiding long range van der Waals forces. Hadronic matter is modeled in terms of its quark constituents by taking into account its internal flavor (u,d,s) and color (red, blue, green) degrees of freedom. Variational MonteCarlo simulations in three spatial dimensions are performed for the groundstate energy of the system. The onset of the transition to strange matter is found to be influenced by weak, yet not negligible, clustering correlations. The phase diagram of the system displays an interesting structure containing both continuous and discontinuous phase transitions. Strange matter is found to be absolutely stable in the model. 24.85.+p, 26.60.+c

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Lower Limit on Radius as a Function of Mass for Neutron Stars

Cited by 25 publications

References 21 publications

Neutron stars structure in the context of massive gravity

Neutron stars structure in the context of massive gravity

Stability of Strange Stars (Ss) Derived From a Realistic Equation of State

Modeling the strangeness content of hadronic matter

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