scholarly journals Strange stars with a mirror-dark-matter core confronting with the observations of compact stars

2021 ◽  
Vol 104 (8) ◽  
Author(s):  
Shu-Hua Yang ◽  
Chun-Mei Pi ◽  
Xiao-Ping Zheng
Keyword(s):  
Dark Matter ◽  
Compact Stars ◽  
Strange Stars

Equation of state of strange stars with admissible dark matter: Derivation from galactic rotational curves

2021 ◽  
Vol 342 (1-2) ◽  
pp. 310-314
Author(s):  
Moisés Razeira ◽  
Fabio Köpp ◽  
Guilherme Volkmer ◽  
Magno Machado ◽  
Dimiter Hadjimichef ◽  
...  
Keyword(s):  
Dark Matter ◽  
Equation Of State ◽  
Strange Stars

scholarly journals Quadrupole moments of rotating compact stars

2012 ◽  
Vol 8 (S291) ◽  
pp. 536-536
Author(s):  
Martin Urbanec ◽  
John Miller ◽  
Zdenek Stuchlik
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Strange Star ◽  
Compact Stars ◽  
Quadrupole Moments ◽  
Strange Stars

AbstractWe present quadrupole moments of rotating neutron and strange stars calculated using standard Hartle Thorne approach. We demonstrate differences between neutron and strange star parameters connected with quadrupole moments and how this parameters could be, in the case of neutron stars, approximated almost independently on neutron star equation of state.

scholarly journals Constraint on Hybrid Stars with Gravitational Wave Events

Universe ◽  
2020 ◽  
Vol 6 (12) ◽  
pp. 231
Author(s):  
Kilar Zhang ◽  
Feng-Li Lin
Keyword(s):  
Black Hole ◽  
Dark Matter ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Compact Object ◽  
Compact Objects ◽  
Compact Stars ◽  
Hybrid Star ◽  
Hybrid Stars

Motivated by the recent discoveries of compact objects from LIGO/Virgo observations, we study the possibility of identifying some of these objects as compact stars made of dark matter called dark stars, or the mix of dark and nuclear matters called hybrid stars. In particular, in GW190814, a new compact object with 2.6 M⊙ is reported. This could be the lightest black hole, the heaviest neutron star, and a dark or hybrid star. In this work, we extend the discussion on the interpretations of the recent LIGO/Virgo events as hybrid stars made of various self-interacting dark matter (SIDM) in the isotropic limit. We pay particular attention to the saddle instability of the hybrid stars which will constrain the possible SIDM models.

scholarly journals Inelastic dark matter as an efficient fuel for compact stars

2010 ◽  
Vol 81 (10) ◽  
Author(s):  
Dan Hooper ◽  
Douglas Spolyar ◽  
Alberto Vallinotto ◽  
Nickolay Y. Gnedin
Keyword(s):  
Dark Matter ◽  
Compact Stars ◽  
Inelastic Dark Matter

Dark matter with chiral symmetry admixed hadronic matter in compact stars

2021 ◽  
Author(s):  
SiNa Wei ◽  
Zhaoqing Feng
Keyword(s):  
Dark Matter ◽  
Energy Density ◽  
Chiral Symmetry ◽  
Density Ratio ◽  
Compact Stars ◽  
Hadronic Matter ◽  
Meson Exchange ◽  
Maximum Mass ◽  
Central Energy ◽  
Two Fluid

Abstract With the two-fluid TOV equation, the properties of dark matter (DM) admixed NSs (DANSs) have been studied. Different from previous studies, we found that increase of the maximum mass and decrease of the radius of 1.4 $M_\odot$ can occur simultaneously in DANS. This stems from the fact that the equation of state (EOS) of DM can be very soft at low density but very stiff at high density. It is well known that the IU-FSU and XS models can not reproduce the neutron star (NS) with a maximum mass greater than 2.0 $M_\odot$. However, considering IU-FSU and XS models in DANS, there are always mass and interactions of DM that can reproduce a maximum mass greater than 2.0 $M_\odot$ and the radius of 1.4 $M_\odot$ below 13.7km. The difference of DANS between the DM with chiral symmetry (DMC) and the DM with meson exchange (DMM) becomes obvious when the central energy density ratio of the DM is greater than one of the NM. When the central energy density ratio of the DM is greater than one of the NM, the DMC model with the DM mass of 1000 MeV still can reproduce a maximum mass greater than 2.0 $M_\odot$ and the radius of 1.4 $M_\odot$ below 13.7km. In the same case, although the maximum mass of DANS with the DMM model is greater than 2.0 $M_\odot$ , the radius of 1.4 $M_\odot$ with the DMM model will surpass 13.7km obviously. \com{In two-fluid system, it is worth noting that the maximum mass of DANS can be larger than 3.0 $M_\odot$. As a consequence, the dimensionless tidal deformability $\Lambda_{CP}$ of DANS with 1.4 $M_\odot$, which increase with increasing the maximum mass of DANS, could be larger than 800 when the radius of DANS with 1.4 $M_\odot$ is about 13.0km.}

P-STARS

2004 ◽  
Vol 13 (09) ◽  
pp. 1917-1926 ◽  
Author(s):  
PAOLO CEA
Keyword(s):  
Dark Matter ◽  
Neutron Stars ◽  
Observational Data ◽  
Gravitational Collapse ◽  
Cold Dark Matter ◽  
Compact Stars ◽  
Cooling Curves ◽  
New Class

P-Stars are a new class of compact stars made of up and down quarks in β-equilibrium with electrons in an Abelian chromomagnetic condensate. We show that P-Stars are able to account for compact stars with R≲6 Km , as well as stars with radius comparable with canonical Neutron Stars. We find that cooling curves of P-Stars compare rather well with observational data. We suggest that P-Matter produced at the primordial deconfinement transition is a viable candidate for baryonic Cold Dark Matter. Finally, we show that P-Stars are able to overcome the gravitational collapse even for masses much greater than 106 M⊙.

Dark Matter Compact Stars in Pseudo-Complex General Relativity

2018 ◽  
pp. 149-167
Author(s):  
D. Hadjimichef ◽  
G. L. Volkmer ◽  
R. O. Gomes ◽  
C. A. Zen Vasconcellos
Keyword(s):  
General Relativity ◽  
Dark Matter ◽  
Compact Stars ◽  
Complex General Relativity

scholarly journals Some New Models of Strange Stars in 5-D Einstein-Gauss-Bonnet Gravity

2021 ◽  
Author(s):  
Manuel Malaver ◽  
Hamed Daei Kasmaei
Keyword(s):  
Equation Of State ◽  
Energy Density ◽  
Nonlinear Equation ◽  
Radial Pressure ◽  
Compact Stars ◽  
Coupling Constant ◽  
Strange Stars ◽  
Bonnet Gravity ◽  
New Models ◽  
Linear And Nonlinear

In this paper, we present some new models for anisotropic compact stars within the framework of 5-dimensional Einstein-Gauss-Bonnet (EGB) gravity with a linear and nonlinear equation of state considering a metric potential proposed for Thirukkanesh and Ragel (2012) and generalized for Malaver (2014). The new obtained models satisfy all physical requirements of a physically reasonable stellar object. Variables as energy density, radial pressure and the anisotropy are dependent of the values of the Gauss-Bonnet coupling constant

scholarly journals Possible maximum mass of dark matter existing in compact stars based on the self-interacting fermionic model

2019 ◽  
Vol 28 (11) ◽  
pp. 1950148
Author(s):  
Xu Dong Wang ◽  
Bin Qi ◽  
Gao Le Yang ◽  
Nai Bo Zhang ◽  
Shou Yu Wang
Keyword(s):  
Dark Matter ◽  
Energy Density ◽  
Strong Interaction ◽  
Milky Way ◽  
Compact Star ◽  
Compact Stars ◽  
Maximum Mass ◽  
Obvious Effect ◽  
Milky Way Galaxy ◽  
Fermionic Model

The dark matter admixed neutron stars (DANSs) are studied using the two-fluid TOV equations separately, in which the normal matter (NM) and dark matter (DM) are simulated by the relativistic mean field theory and self-interacting fermionic model, respectively. A universal relationship [Formula: see text] is suggested, where [Formula: see text] is the maximum mass of DM existing in DANSs, [Formula: see text] is the particle mass of DM ranging from 5[Formula: see text]GeV to 1[Formula: see text]TeV, [Formula: see text] is the interaction mass scale with the value 300[Formula: see text]GeV (0.1[Formula: see text]GeV) for weak (strong) interaction DM model. This simple formula connects directly the microcosmic nature of DM particle with its macrocosmic mass existing in DANSs. Meanwhile, such a formula exhibits that the existence of NM has little effect on [Formula: see text]. It is found that the ratio of radius of DM in DANSs over [Formula: see text] is a constant with the value about 12[Formula: see text] (7[Formula: see text]) for weak (strong) interaction DM cases. According to the calculated results, only for the strong interaction DM cases with [Formula: see text] to [Formula: see text][Formula: see text]GeV and central energy density [Formula: see text][Formula: see text]MeV/fm3, DM has obvious effect on the mass of compact star. Compared with the energy density of DM in the Milky Way galaxy, [Formula: see text][Formula: see text]MeV/fm3, the existence of DM might hardly affect the mass of compact stars in the Milky Way galaxy.

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