Effects of in-Medium Modification of Weakly Interacting Light Boson Mass in Neutron Stars

Sulaksono, A.; Marliana,; Kasmudin,

doi:10.1142/s0217732311034827

Cited by 14 publications

(9 citation statements)

References 23 publications

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“…These results can be achieved without adjusting the hyperons coupling constant, introducing hypothetical particle like WILB or modifying the nonlinear terms in the strange meson sector. [29][30][31][32][33] Furthermore, by assuming that NS matter may have anisotropic pressure, the NS maximum mass limit higher than 2.1 M ⊙ cannot rule out the presence of exotica in the form of hyperons, boson condensations or quark matter inside the NS core. For I-P case, the canonical radius with hyperons is R 1.4 =12.57 km, and R 1.4 =12.61 km without hyperons.…”

Section: Resultsmentioning

confidence: 99%

“…In relativistic mean field (RMF) models, the situation is quite similar, M max ∼ 2.1 M ⊙ can be reached only by adjusting the model parameters in the hyperon sector or modifying nonlinear in the strange sector or introducing hypothetical weakly interacting light boson (WILB). [29][30][31][32][33] The puzzle that whether or not the hyperons are present in the NS core has triggered the theoreticians to revisit the NS models (see Refs. 34-40 for details).…”

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: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Anisotropic pressure and hyperons in neutron stars

Sulaksono

2015

Int. J. Mod. Phys. E

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“…Effects of non-Newtonian gravity on the properties of neutron stars and SSs have been studied extensively [e.g., [11][12][13][14][15][16][17][18][19]. The conventional inverse-square-law of gravity is expected to be violated in the efforts of trying to unify gravity with the other three fundamental forces, namely, the electromagnetic, weak and strong interactions [20][21][22].…”

Section: Introductionmentioning

confidence: 99%

Constraints from compact star observations on non-Newtonian gravity in strange stars based on a density dependent quark mass model

Yang,

Pi,

Zheng

et al. 2021

Preprint

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Using a density dependent quark mass (QMDD) model for strange quark matter, we investigate the effects of non-Newtonian gravity on the properties of strange stars and constrain the parameters of the QMDD model by employing the mass of PSR J0740+6620 and the tidal deformability of GW170817. We find that for QMDD model these mass and tidal deformability observations would rule out the existence of strange stars if non-Newtonian gravity effects are ignored. For the current quark masses of m u0 = 2.16 MeV, m d0 = 4.67 MeV, and m s0 = 93 MeV, we find that a strange star can exist for values of the non-Newtonian gravity parameter g 2 /µ 2 in the range of 4.58 GeV −2 ≤ g 2 /µ 2 ≤ 9.32 GeV −2 , and that the parameters D and C of the QMDD model are restricted to 158.3 MeV≤ D 1/2 ≤ 181.2 MeV and −0.65 ≤ C ≤ −0.12. It is found that the largest possible maximum mass of a strange star obtained with the QMDD model is 2.42 M ⊙ , and that the secondary component of GW190814 with a mass of 2.59 +0.08 −0.09 M ⊙ could not be a static strange star. We also find that for the mass and radius of PSR J0030+0451 given by Riley et al. through the analysis of observational data of NICER, there exists a very tiny allowed parameter space for which strange stars computed for the QMDD model agree with the observations of PSR J0740+6620, GW170817 and PSR J0030+0451 simultaneously. However, for the mass and radius given by Miller et al., no such parameter space exist.

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“…In addition, this issue has attracted a great deal of attention in a nuclear physics context, for instance, it has strong effects on finite nuclei (Xu et al 2013), dark matter (Schmidt 1990), nuclear matter (Wen et al 2009;Zhang et al 2011), and neutron star processes (Sulaksono et al 2011;Wen & Zhou 2013).…”

Section: Introductionmentioning

confidence: 99%

Effects of non-Newtonian gravity on the properties of strange stars

Lù

Peng

Zhou

2017

Res. Astron. Astrophys.

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The properties of strange star matter are studied in the equivparticle model with inclusion of non-Newtonian gravity. It is found that the inclusion of non-Newtonian gravity makes the equation of state stiffer if Witten's conjecture is true. Correspondingly, the maximum mass of strange stars becomes as large as two times the solar mass, and the maximum radius also becomes bigger. The coupling to boson mass ratio has been constrained within the stability range of strange quark matter.

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Effects of in-Medium Modification of Weakly Interacting Light Boson Mass in Neutron Stars

Cited by 14 publications

References 23 publications

Anisotropic pressure and hyperons in neutron stars

Anisotropic pressure and hyperons in neutron stars

Constraints from compact star observations on non-Newtonian gravity in strange stars based on a density dependent quark mass model

Effects of non-Newtonian gravity on the properties of strange stars

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