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
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基于密度依赖夸克质量模型的致密星观测对奇异星非牛顿引力的约束
DOI：
10.1103/physrevd.103.043012
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发表时间：
2021-01
影响因子：
5
通讯作者：
Fridolin Weber
中科院分区：
文献类型：
--
作者：
Shu-Hua Yang;Chun-Mei Pi;Xiao-Ping Zheng;Fridolin Weber
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 $\mathrm{J}0740+6620$ and the tidal deformability of GW170817. We find that for the 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 ${m}_{u0}=2.16\text{ }\text{ }\mathrm{MeV}$, ${m}_{d0}=4.67\text{ }\text{ }\mathrm{MeV}$, and ${m}_{s0}=93\text{ }\text{ }\mathrm{MeV}$, we find that a strange star can exist for values of the non-Newtonian gravity parameter ${g}^{2}/{\ensuremath{\mu}}^{2}$ in the range of $4.58\text{ }\text{ }{\mathrm{GeV}}^{\ensuremath{-}2}\ensuremath{\le}{g}^{2}/{\ensuremath{\mu}}^{2}\ensuremath{\le}9.32\text{ }\text{ }{\mathrm{GeV}}^{\ensuremath{-}2}$, and that the parameters $D$ and $C$ of the QMDD model are restricted to $158.3\text{ }\text{ }\mathrm{MeV}\ensuremath{\le}{D}^{1/2}\ensuremath{\le}181.2\text{ }\text{ }\mathrm{MeV}$ and $\ensuremath{-}0.65\ensuremath{\le}C\ensuremath{\le}\ensuremath{-}0.12$. It is found that the largest possible maximum mass of a strange star obtained with the QMDD model is $2.42\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ and that the secondary component of GW190814 with a mass of ${2.59}_{\ensuremath{-}0.09}^{+0.08}\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ could not be a static strange star. We also find that for the mass and radius of PSR $\mathrm{J}0030+0451$ 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 $\mathrm{J}0740+6620$, GW170817 and PSR $\mathrm{J}0030+0451$ simultaneously. However, for the mass and radius given by Miller et al., no such parameter space exist.
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 $\mathrm{J}0740+6620$ and the tidal deformability of GW170817. We find that for the 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 ${m}_{u0}=2.16\text{ }\text{ }\mathrm{MeV}$, ${m}_{d0}=4.67\text{ }\text{ }\mathrm{MeV}$, and ${m}_{s0}=93\text{ }\text{ }\mathrm{MeV}$, we find that a strange star can exist for values of the non-Newtonian gravity parameter ${g}^{2}/{\ensuremath{\mu}}^{2}$ in the range of $4.58\text{ }\text{ }{\mathrm{GeV}}^{\ensuremath{-}2}\ensuremath{\le}{g}^{2}/{\ensuremath{\mu}}^{2}\ensuremath{\le}9.32\text{ }\text{ }{\mathrm{GeV}}^{\ensuremath{-}2}$, and that the parameters $D$ and $C$ of the QMDD model are restricted to $158.3\text{ }\text{ }\mathrm{MeV}\ensuremath{\le}{D}^{1/2}\ensuremath{\le}181.2\text{ }\text{ }\mathrm{MeV}$ and $\ensuremath{-}0.65\ensuremath{\le}C\ensuremath{\le}\ensuremath{-}0.12$. It is found that the largest possible maximum mass of a strange star obtained with the QMDD model is $2.42\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ and that the secondary component of GW190814 with a mass of ${2.59}_{\ensuremath{-}0.09}^{+0.08}\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ could not be a static strange star. We also find that for the mass and radius of PSR $\mathrm{J}0030+0451$ 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 $\mathrm{J}0740+6620$, GW170817 and PSR $\mathrm{J}0030+0451$ simultaneously. However, for the mass and radius given by Miller et al., no such parameter space exist.
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DOI：
10.1103/physrevd.81.123016
发表时间：
2009-11
期刊：
Bulletin of the American Physical Society
影响因子：
--
作者：
T. Hinderer;B. Lackey;R. Lang;J. Read
通讯作者：
T. Hinderer;B. Lackey;R. Lang;J. Read
影响因子：
1.8
作者：
Lu Zhen Yan;Peng Guang Xiong;Zhou Kai
通讯作者：
Zhou Kai
影响因子：
9.6
作者：
F. Weber
通讯作者：
F. Weber
影响因子：
8.6
作者：
Dehua Wen;Bao-An Li;Lie-Wen Chen
通讯作者：
Dehua Wen;Bao-An Li;Lie-Wen Chen
影响因子：
14.1
作者：
Capano, Collin D.;Tews, Ingo;Reddy, Sanjay
通讯作者：
Reddy, Sanjay