Tidal deformability as a probe of dark matter in neutron stars

Karkevandi, Davood Rafiei; Shakeri, Soroush; Sagun, V. V.; Ivanytskyi, O.

doi:10.1142/9789811269776_0307

Cited by 4 publications

(4 citation statements)

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Section: Dark Matter In Neutron Starsmentioning

confidence: 99%

“…It is conjectured that DM could also exist within and around NSs, accreted into its interior forming a DM core [35][36][37][38] or as DM halo exceeding its radius [39][40][41][42][43][44][45]. The presence of DM in NSs would affect NS observables such as their mass, radius, tidal deformability, or cooling [35,[44][45][46][47][48][49][50][51][52][53][54][55][56][57][58]. If DM is present in NSs, it could affect gravitational wave emission through its effects on the global properties such as NS mass and radius, or its effect on unstable oscillation modes such as r-modes.…”

Section: Dark Matter In Neutron Starsmentioning

confidence: 99%

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R-modes as a new probe of dark matter in neutron stars

Shirke,

Ghosh,

Chatterjee

et al. 2023

J. Cosmol. Astropart. Phys.

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In this work, we perform the first systematic investigation of effects of the presence of dark matter on r-mode oscillations in neutron stars (NSs). Using a self-interacting dark matter (DM) model based on the neutron decay anomaly and a hadronic model obtained from the posterior distribution of a recent Bayesian analysis, we impose constraints on the DM self-interaction strength using recent multimessenger astrophysical observations. We also put new constraints on the DM fraction for this model of DM. The constrained DM interaction strength is then used to estimate DM self-interaction cross section and shear viscosity resulting from DM, which is found to be several orders of magnitude smaller than shear viscosity due to hadronic matter. Assuming chemical equilibrium among DM fermions and neutrons, we estimate the bulk viscosity resulting from the dark decay of neutrons considering different scenarios for the temperature dependence of the reaction rate and investigate the effect on the r-mode instability window. We conclude that DM shear and bulk viscosity may significantly modify the r-mode instability window compared with the minimal hadronic viscosities, depending on the temperature dependence of the process. We also found that for the window to be compatible with the X-ray and pulsar observational data, the rate for the dark decay process must be fast.

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Section: Dark Matter In Neutron Starsmentioning

confidence: 99%

Section: Dark Matter In Neutron Starsmentioning

confidence: 99%

R-modes as a new probe of dark matter in neutron stars

Shirke,

Ghosh,

Chatterjee

et al. 2023

J. Cosmol. Astropart. Phys.

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“…In recent years, multi-messenger observations of NSs have provided a unique opportunity to probe their internal structure and the possible existence of exotic configurations, including DM [29,30]. The impact of DM on NS properties has been investigated in various studies proposing a wide range of smoking guns [31][32][33][34][35][36][37]. Generally, the presence of DM can be considered through two scenarios: (i) a single-fluid object for which DM and BM interact also non-gravitationally via an EoS [18,19,[38][39][40][41][42], and (ii) two-fluid DM-admixed NSs where DM and BM are described by two EoSs and interact only by the gravitational force [10,[43][44][45][46][47][48][49].…”

Section: Introductionmentioning

confidence: 99%

“…In this research, in order to model DM, we consider a self-repulsive complex scalar field with sub-GeV bosonic particles and a coupling constant in the order of unity. Our DM EoS was first used in the pioneering work by Colpi et al [68] to describe boson stars [69,70] and was more recently revisited to model the two-fluid DM-admixed NSs [10,11,33]. For the BM component, we employ a widely used and well-known nuclear matter EoS called DD2.…”

Section: Introductionmentioning

confidence: 99%

Exploring the Distribution and Impact of Bosonic Dark Matter in Neutron Stars

Rafiei Karkevandi,

Shahrbaf,

Shakeri

et al. 2024

Particles

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The presence of dark matter (DM) within neutron stars (NSs) can be introduced by different accumulation scenarios in which DM and baryonic matter (BM) may interact only through the gravitational force. In this work, we consider asymmetric self-interacting bosonic DM, which can reside as a dense core inside the NS or form an extended halo around it. It is seen that depending on the boson mass (mχ), self-coupling constant (λ) and DM fraction (Fχ), the maximum mass, radius and tidal deformability of NSs with DM admixture will be altered significantly. The impact of DM causes some modifications in the observable features induced solely by the BM component. Here, we focus on the widely used nuclear matter equation of state (EoS) called DD2 for describing NS matter. We show that by involving DM in NSs, the corresponding observational parameters will be changed to be consistent with the latest multi-messenger observations of NSs. It is seen that for mχ≳200 MeV and λ≲2π, DM-admixed NSs with 4%≲Fχ≲20% are consistent with the maximum mass and tidal deformability constraints.

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