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

Lù, Zhongwen; Peng, Guang-Xiong; Zhou, Kai

doi:10.1088/1674-4527/17/2/11

Cited by 10 publications

(10 citation statements)

References 49 publications

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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%

“…The contribution of the Yukawa correction V Y (r) of Eq. ( 13) to the energy density of SQM is obtained by integrating over the quark densities n b ( x 1 ) and n b ( x 2 ) inside a given volume V [11,12,17,51],…”

Section: Introductionmentioning

confidence: 99%

“…Equation ( 16) can be evaluated further since the quark densities n b ( x 1 ) = n b ( x 2 ) ≡ n b are essentially independent of position [7][8][9][10]. Moving n b outside of the integral then leads for the energy density of SQM inside of V = 4πR 3 /3 (for simplicity taken to be spherical 2 ) to [17,19]…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…[17] and references therein). Effects of non-Newtonian gravity on the properties of NSs and QSs have been studied [18][19][20][21][22], and it is found that the inclusion of non-Newtonian gravity will lead to the stiffening of the EOS and a bigger maximum mass of the stars.…”

mentioning

confidence: 99%

“…Non-Newtonian gravity will be introduced following Refs. [18][19][20]. According to Fujii [16], non-Newtonian gravity can be described by adding a Yukawa term to the conventional potential between two objects with masses m 1 and m 2 , i.e.,…”

mentioning

confidence: 99%

Non-Newtonian gravity in strange quark stars and constraints from the observations of PSR J0740+6620 and GW170817

Yang,

PI,

Zheng

et al. 2019

Preprint

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We investigate the effects of non-Newtonian gravity on the properties of strange quark stars (QSs) and constrain the parameters of strange quark matter (SQM) model (namely, the modified bag model) employing the mass of PSR J0740+6620 and the tidal deformability of GW170817. We find that the existence of QSs without the inclusion of non-Newtonian gravity effects is ruled out by the observations. We also find that QSs can exist for 1.95GeV −2 ≤ g 2 /µ 2 ≤ 7.28GeV −2 (g 2 /µ 2 is the non-Newtonian gravity parameter), and the parameters of SQM model are restricted to 141.8MeV≤ B 1/4 ≤ 150.4MeV and α S ≤ 0.52.

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Strange stars confronting with the observations: Non‐Newtonian gravity effects, or the existence of a dark‐matter core

Yang

2022

Astron Nachr

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We find that the existence of strange stars is ruled out by the dimensionless tidal deformability of a 1.4 M ⊙ star of GW170817 and the mass of PSR J0740 + 6620, both for the standard MIT bag model and for the density-dependent quark mass model. However, if non-Newtonian gravity effects are considered, strange stars can exist for certain ranges of the values of the non-Newtonian gravity parameter. An alternative explanation to these observations is to suppose that strange stars in GW170817 have a dark-matter core.

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

Cited by 10 publications

References 49 publications

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

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

Non-Newtonian gravity in strange quark stars and constraints from the observations of PSR J0740+6620 and GW170817

Strange stars confronting with the observations: Non‐Newtonian gravity effects, or the existence of a dark‐matter core

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