Consequences of neutron decay inside neutron stars

Husain, Wasif; Motta, Theo F.; Thomas, A. W.

doi:10.1088/1475-7516/2022/10/028

Cited by 11 publications

(17 citation statements)

References 95 publications

(83 reference statements)

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“…χ being the dark spin-half fermion with baryon number 1, and φ being a light dark boson. This possibility is also explored by various other recent works [61,79,80,105]. The light dark particle φ is assumed to escape the NS without any interaction, similar to neutrinos.…”

Section: Jcap12(2023)008mentioning

confidence: 97%

“…In recent years, there has been significant interest in this topic, and several investigations tried to impose constraints on DM models using astrophysical data [41,42,[60][61][62][63]. Moreover, Atreya et al [64] investigated the effect of DM shear viscosity on cosmological evolution.…”

Section: Dark Matter In Neutron Starsmentioning

confidence: 99%

Section: Neutron Star Modelmentioning

confidence: 99%

“…Various DM models can be constructed to describe DM in NSs [35,42,46,58,61,[67][68][69][70][71][72][73][74][75][76][77][78][79][80][81][82][83][84]. In this work, we adopt a DM model based on a recent work by [61,79,80] which is motivated by the fact that the neutron decay anomaly can be explained via the decay of the neutron to the dark sector [85][86][87]. The motivation for applying such a model is twofold: (i) firstly it can explain sufficient DM fraction in NSs which is an essential requirement for our investigation and (ii) secondly, the decay rate of neutrons fixes a key ingredient for the calculation of viscosity in NSs.…”

Section: Neutron Star Modelmentioning

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: Jcap12(2023)008mentioning

confidence: 97%

Section: Dark Matter In Neutron Starsmentioning

confidence: 99%

Section: Neutron Star Modelmentioning

confidence: 99%

Section: Neutron Star Modelmentioning

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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“…The mass-radius relation of neutron stars can significantly change if there is dark matter present. The modification of the global structure of neutron stars has been studied in detail for bosonic and fermionic dark matter with and without self-interactions (see Sandin & Ciarcelluti 2009;Ciarcelluti & Sandin 2011;Leung et al 2011;Li et al 2012;Xiang et al 2014;Mukhopadhyay et al 2017;Baym et al 2018;Ellis et al 2018b;McKeen et al 2018;Motta et al 2018;Ivanytskyi et al 2020;Husain et al 2022) and can even lead to exotic compact objects such as dark compact planets (Tolos et al 2015). Current and future gravitational wave detectors have the potential to detect the possible presence of dark matter in merging neutron stars and to constrain the properties of dark matter, such as its mass and its self-interaction strength (Ellis et al 2018a;Horowitz & Reddy 2019;Nelson et al 2019;Bauswein et al 2020;Dengler et al 2022;Karkevandi et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Exotic Compact Objects with Two Dark Matter Fluids

Marie¹,

Brisebois

Azeem

et al. 2023

ApJ

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The generic properties of compact objects made of two different fluids of dark matter are studied in a scale-invariant approach. We investigate compact objects with a core–shell structure, where the two fluids are separated, and with mixed dark matter components, where both dark matter fluids are immersed within each other. The constellations considered are combinations of incompressible fluids, free and interacting Fermi gases, and equations of state with a vacuum term, i.e., self-bound dark matter. We find novel features in the mass–radius relations for combined dark matter compact objects, which distinguishes them from compact objects with a single dark matter fluid and compact stars made of ordinary baryonic matter, such as white dwarfs, neutron stars, and quark stars. The maximum compactness of certain combined dark matter stars can reach values up to the causality limit for compact stars but not beyond that limit if causality of the dark matter fluids is ensured.

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