Effect of nuclear saturation parameters on a possible maximum mass of neutron stars

Sotani, Hajime

doi:10.1103/physrevc.95.025802

Cited by 27 publications

(23 citation statements)

References 19 publications

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“…Other relationships between NS observables and physical parameters can be found in the literature, for example, the upper limit on the mass and rotation speed set by causality [71] or the value of the fiducial energy density up to which the modern neutron star matter EoSes are believe to be reliable [72]. Another interesting relationship has recently been proposed between the maximum mass of a compact object and the maximum speed of sound of matter in the inner core of neutron stars [73]. If the existence of a mixed phase is considered using our heuristic model, families of compact objects with lower maximum masses are obtained.…”

Section: Resultsmentioning

confidence: 99%

Oscillation modes of hybrid stars within the relativistic Cowling approximation

Ranea‐Sandoval

Guilera

Mariani

et al. 2018

J. Cosmol. Astropart. Phys.

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The first direct detection of gravitational waves has opened a new window to study the Universe and would probably start a new era: the gravitational wave Astronomy. Gravitational waves emitted by compact objects like neutron stars could provide significant information about their structure, composition and evolution.In this paper we calculate, using the relativistic Cowling approximation, the oscillations of compact stars focusing on hybrid stars, with and without a mixed phase in their cores. We study the existence of a possible hadron-quark phase transition in the central regions of neutron stars and the changes it produces on the gravitational modes frequencies emitted by these stars. We pay particular attention to the g-modes, which are extremely important as they could signal the existence of pure quark matter inside neutron stars. Our results show a relationship between the frequency of the g-modes and the constant speed of sound parametrization for the quark matter phase. We also show that the inclusion of color superconductivity produces an increase on the oscillation frequencies.We propose that observations of g-modes with frequencies f g between 1 kHz and 1.5 kHz should be interpreted as an evidence of a sharp hadron-quark phase transition in the core of a compact object.

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Section: Resultsmentioning

confidence: 99%

Oscillation modes of hybrid stars within the relativistic Cowling approximation

Ranea‐Sandoval

Guilera

Mariani

et al. 2018

J. Cosmol. Astropart. Phys.

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“…As it was shown in [13], in the general relativistic framework there is a difficulty in explaining the observed masses of PSR J1614-2230 and PSR J0348+0432 under the assumption that the maximum sound velocity in the core is smaller than c/ √ 3 [37]. However, at this range of sound velocity values, scalarization allows for neutron stars with masses even larger than the observed ones.…”

Section: The Maximum Mass Limit Of Neutron Stars In Scalar-tensormentioning

confidence: 93%

“…In general relativity, the dependence of the maximum mass on the parameter η, was extensively discussed in [13], were also fitting formulae have been derived. Here, we extent this study by taking into account the dependence of the maximum mass limit on η for scalarized neutron star models.…”

Section: The Maximum Mass Limit Of Neutron Stars In Scalar-tensormentioning

confidence: 99%

Maximum mass limit of neutron stars in scalar-tensor gravity

Sotani

Kokkotas

2017

Phys. Rev. D

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The maximum mass limits of neutron stars in scalar-tensor gravity is discussed and compared with the limits set by general relativity. The limit is parametrized with respect to the combination of the nuclear saturation parameters and the maximum sound velocity in the core. It is shown that, for smaller values of the sound velocity in the core, the maximum mass limit of the scalarized neutron stars is larger than that of in general relativity. However, for stiff equations of state with sound velocity higher than 79% of the velocity of light, the maximum mass limit in general relativity is larger than that of in scalar-tensor gravity. The results suggest that future observations of massive neutron stars, may constrain the maximum sound velocity as well as the coupling parameter in scalar-tensor gravity.

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“…As in Refs. [34,35], we construct the maximum mass neutron star models in general relativity and the scalarized models with maximum mass for β = −5. The mass of scalarized neutron stars for the values of β allowed by observations can not reach the maximum mass of the corresponding models in general relativity for the case of v 2 s > ∼ 0.6 [35].…”

Section: Compactness For the Maximum Mass Neutron Starmentioning

confidence: 99%

Compactness of neutron stars and Tolman VII solutions in scalar-tensor gravity

Sotani

Kokkotas

2018

Phys. Rev. D

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We systematically examine the compactness of neutron stars as Tolman VII solutions in scalar-tensor theory of gravity. As a result, when the coupling constant is confined to values provided by astronomical observations we show that the maximum compactness of neutron stars in general relativity is higher than that in scalar-tensor gravity. In addition, we show that although ultra-compact stars, with radius smaller than the Regge-Wheeler potential peak, can exist in general relativity (e.g., Tolman VII solution), their scalarized counterparts cannot be constructed even in the limiting case of uniform density stars.

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Effect of nuclear saturation parameters on a possible maximum mass of neutron stars

Cited by 27 publications

References 19 publications

Oscillation modes of hybrid stars within the relativistic Cowling approximation

Oscillation modes of hybrid stars within the relativistic Cowling approximation

Maximum mass limit of neutron stars in scalar-tensor gravity

Compactness of neutron stars and Tolman VII solutions in scalar-tensor gravity

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