On the Maximum Mass of Neutron Stars

Chamel, Nicolas; Haensel, P.; Zdunik, J. L.; Fantina, Anthea

doi:10.1142/s021830131330018x

Cited by 90 publications

(85 citation statements)

References 108 publications

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“…However, we point out that over the time, with new planned observatories and technology advancement in astrometry, it is not impossible to have accurately measured pulsar mass of higher than 2.1 M ⊙ in the future. 8,10,11 For the latest review on neutron star masses and their implications we refer the reader to Refs. [8][9][10][11].…”

Section: Introductionmentioning

confidence: 99%

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Anisotropic pressure and hyperons in neutron stars

Sulaksono

2015

Int. J. Mod. Phys. E

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We study the effects of anisotropic pressure on properties of the neutron stars with hyperons inside its core within the framework of extended relativistic mean field. It is found that the main effects of anisotropic pressure on neutron star matter is to increase the stiffness of the equation of state, which compensates for the softening of the EOS due to the hyperons. The maximum mass and redshift predictions of anisotropic neutron star with hyperonic core are quite compatible with the result of recent observational constraints if we use the parameter of anisotropic pressure model h ≤ 0.8 1 and Λ ≤ −1.15. 2 The radius of the corresponding neutron star at M =1.4 M ⊙ is more than 13 km, while the effect of anisotropic pressure on the minimum mass of neutron star is insignificant. Furthermore, due to the anisotropic pressure in the neutron star, the maximum mass limit of higher than 2.1 M ⊙ cannot rule out the presence of hyperons in the neutron star core.

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Section: Introductionmentioning

confidence: 99%

“…8,10,11 For the latest review on neutron star masses and their implications we refer the reader to Refs. [8][9][10][11]. It is also worthy to note that actually accurate measurements of the NS radii would also strongly constrain the properties of the matter in NS core.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic pressure and hyperons in neutron stars

Sulaksono

2015

Int. J. Mod. Phys. E

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“…[3] and in this paper only the non-rotating solutions are investigated. Furthermore, there exist enough successful models for explaining massive pulsars in the literature (see for examples Refs [9][10][11]). …”

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confidence: 99%

Bosons star at finite temperature

2014

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By using a simple thermodynamical method we confirm the finding of Chavanis and Harko that stable Bose-Einstein condensate stars can form. However, by using a thermodynamically consistent boson equation of state, we obtain a less massive Bose-Einstein condensate star compared to the one predicted by Chavanis and Harko. We also obtain that the maximum mass of a boson star is insensitive to the change of matter temperature. However, the mass of boson star with relatively large radius depends significantly on the temperature of the boson matter.

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“…However, in this framework if NS with the mass of greater than 2.1M can be accurately measured in the future, it is quite difficult to reconcile the existence of exotic particles such as hyperons in NS core as well as the small measured radius, respectively [6]. For recent review about the status of this approach see Reference [7] and the references therein. Recently, the author of Reference [8] showed, if the isotropic assumption is relaxed by considering that the pressure in NS could be anisotropic, the maximal mass around 2.1M can be easily reached by adjusting anisotropic parameter of the anisotropic models.…”

Section: Introductionmentioning

confidence: 99%

Cracking on anisotropic neutron stars

Setiawan¹,

Sulaksono²

2017

AIP Conference Proceedings

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Abstract. We study the effect of cracking of a local anisotropic neutron star (NS) due to small density fluctuations. It is assumed that the neutron star core consists of leptons, nucleons and hyperons. The relativistic mean field model is used to describe the core of equation of state (EOS). For the crust, we use the EOS introduced by Miyatsu et al. [1]. Furthermore, two models are used to describe pressure anisotropic in neutron star matter. One is proposed by Doneva-Yazadjiev (DY) [2] and the other is proposed by Herrera-Barreto (HB) [3]. The anisotropic parameter of DY and HB models are adjusted in order the predicted maximum mass compatible to the mass of PSR J1614-2230 [4] and PSR J0348+0432 [5]. We have found that cracking can potentially present in the region close to the neutron star surface. The instability due cracking is quite sensitive to the NS mass and anisotropic parameter used.

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On the Maximum Mass of Neutron Stars

Cited by 90 publications

References 108 publications

Anisotropic pressure and hyperons in neutron stars

Anisotropic pressure and hyperons in neutron stars

Bosons star at finite temperature

Cracking on anisotropic neutron stars

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