On the Stability of Strange Dwarf Hybrid Stars

Alford, Mark; Harris, Steven P.; Sachdeva, Pratik S.

doi:10.3847/1538-4357/aa8509

Cited by 30 publications

(35 citation statements)

References 22 publications

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“…When considering twin starts, there may be more than one stable branch, so it is important to continue to solve the TOV equations passed the first stable branch. Note that the second branch is only stable if the mass-radius curve rotates clockwise with increasing central pressure at the extremum that gives raise to it [89]. Alternatively, a slow conversion from hadronic to quark phase inside stars could turn dM/dε c < 0 stars dynamic stable due to how the phase interface moves under stellar pulsation (see Ref.…”

Section: A Observable Quantitiesmentioning

confidence: 99%

Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions

Tan,

Dore,

Dexheimer

et al. 2021

Preprint

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The speed of sound of the matter within neutron stars may contain non-smooth structure related to first-order phase transitions or crossovers. Here we investigate what are the observable consequences of structure in the speed of sound, such as bumps, spikes, step functions, plateaus, and kinks. One of the main consequences is the possibility of ultra-heavy neutron stars (with masses larger than 2.5 solar masses) and mass twins in heavy (with masses larger than 2 solar masses) and ultra-heavy neutron stars. These stars pass all observational and theoretical constraints, including those imposed by recent LIGO/Virgo gravitational-wave observations and NICER X-ray observations. We thoroughly investigate other consequences of this structure in the speed of sound to develop an understanding of how non-smooth features affect astrophysical observables, such as stellar radii, tidal deformability, moment of inertia, and Love number. Our results have important implications for future gravitational wave and X-ray observations of neutron stars and their impact in nuclear astrophysics.

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Section: A Observable Quantitiesmentioning

confidence: 99%

Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions

Tan,

Dore,

Dexheimer

et al. 2021

Preprint

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show abstract

“…[45]). They might also shed light onto the phenomenology of strange dwarfs, which seem to be unstable under radial perturbations [46,47], or more exotic forms including the existence of condensed dark matter in neutron stars [48] and strange stars [49].…”

Section: Summary and Final Remarksmentioning

confidence: 99%

Radial oscillations of quark stars from perturbative QCD

Jiménez

Fraga

2019

Phys. Rev. D

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“…The other method consists in solving the relevant Sturm-Liouville equation to explicitly obtain the radial oscillation eigenmodes, following [85]. This is used by [58,86] and by us in what follows.…”

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confidence: 99%

Dark compact objects: An extensive overview

et al. 2019

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We study the structure of compact objects that contain non-self annihilating, self-interacting dark matter admixed with ordinary matter made of neutron star and white dwarf materials. We extend the previous work Phys. Rev. D 92 123002 (2015) on these dark compact objects by analyzing the effect of weak and strongly interacting dark matter with particle masses in the range of 1-500 GeV, so as to set some constraints in the strength of the interaction and the mass of the dark matter particle. We find that the total mass of the compact objects increases with decreasing dark matter particle mass. In the strong interacting case and for dark matter particle masses in the range 1-10 GeV, the total mass of the compact objects largely exceeds the 2M constraint for neutron star masses and the nominal 1M for white dwarfs, while for larger dark matter particle masses or in the weakly interacting case the compact objects show masses in agreement or smaller than these constraints, thus hinting at the exclusion of strongly self-interacting dark matter of masses 1-10 GeV in the interior of these compact objects. Moreover, we observe that the smaller the dark matter particle mass, the larger the quantity of dark matter captured is, putting constraints on the dark matter mass trapped in the compact objects so as to fullfill 2M observations. Finally, the inhomogeneity of distribution of dark matter in the Galaxy implies a mass dependence of compact objects from the environment which can be used to put constraints on the characteristics of the Galaxy halo DM profile and on particle mass. In view of the these results, we discuss the formation of the dark compact objects in an homogeneous and non-homogeneous dark matter environment. In the ΛCDM model, a parameterization of the big-bang cosmology with six parameters, the DE is associated with the cosmological constant Λ, and the material components of the Universe are the ones indicated previously. The quoted ΛCDM paradigm, describes correctly many of the observations[2, 6-9], but has some drawbacks. On large scale CMB shows some anomalies, such as that the Planck 2015 data are in tension with the CFHTLenS weak lensing [10], and σ 8 [11]. There is also another tension with the value of the Hubble parameter measured by SNIa 1 . Another big issue of the paradigm is the nature of DM. A "zoo" of candidates have been proposed, with masses in the range of 10 −33 GeV (Fuzzy DM) to 10 15 GeV (Wimpzillas). In that large "zoo", 1 The ΛCDM paradigm has some other drawbacks, as the cosmological constant problem [12,13], the unknown nature of DE [14-16] and the so called "small scale problems" [17].

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On the Stability of Strange Dwarf Hybrid Stars

Cited by 30 publications

References 22 publications

Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions

Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions

Radial oscillations of quark stars from perturbative QCD

Dark compact objects: An extensive overview

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