Confronting nuclear equation of state in the presence of dark matter using GW170817 observation in relativistic mean field theory approach

Das, Arpan; Malik, Tuhin; Nayak, A.

doi:10.1103/physrevd.99.043016

Cited by 66 publications

(114 citation statements)

References 65 publications

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“…7), astronomical observations can also be used to place constraints on the relevant parameter space. In general, since GW170817 provided an upper limit onΛ, any physical effect that results in a softening of the equation of state can be consistent with the data [88,[240][241][242][243][244][245][246] As such, a strong first-order phase transition might make an equation of state model compatible with the GW170817 data, even if the hadronic part on its own is not [152,[247][248][249][250]. A number of studies have constructed models that can successfully interpret the inspiral signal from GW170817 as the coalescence of any combination of hadronic and hybrid hadronic-quark neutron stars and place corresponding constraints on the relevant model parameter space [149,247,248,[251][252][253][254][255][256][257][258][259][260].…”

Section: Microscopic Propertiesmentioning

confidence: 67%

Neutron-star tidal deformability and equation-of-state constraints

2020

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Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars' macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational wave emission, this deformation, quantified through a parameter termed the tidal deformability, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature's most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron star coalescence with gravitational waves as of the time of writing.

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Section: Microscopic Propertiesmentioning

confidence: 67%

Neutron-star tidal deformability and equation-of-state constraints

2020

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“…The meson fields for the NM system are calculated by solving the mean-field equation of motions (Kumar et al 2017(Kumar et al , 2018Das et al 2019) in a self-consistent way. The energy density (E nucl. )…”

Section: Construction Of Eos Using Rmf Approachmentioning

confidence: 99%

“…The detailed discussions can be found in our previous calculations (Das et al 2020). As we know that the addition of DM softens the EoS, reduce mass-radius of the NS (Li et al 2012;Das et al 2019;Bhat & Paul 2020;Quddus et al 2020;Das et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Effects of dark matter on the nuclear and neutron star matter

Das

Kumar

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the dark matter (DM) effects on the nuclear matter (NM) parameters characterizing the equation of states of super dense neutron-rich nucleonic matter. The observables of the NM, i.e. incompressibility, symmetry energy and its higher order derivatives in the presence DM for symmetric and asymmetric NM are analysed with the help of an extended relativistic mean field model. The calculations are also extended to β-stable matter to explore the properties of the neutron star (NS). We analyse the DM effects on symmetric NM, pure neutron matter, and NS using NL3, G3, and IOPB-I forces. The binding energy per particle and pressure is calculated with and without considering the DM interaction with the NM systems. The influences of DM are also analysed on the symmetry energy and its different coefficients. The incompressibility and the skewness parameters are affected considerably due to the presence of DM in the NM medium. We extend the calculations to the NS and find its mass, radius and the moment of inertia for static and rotating NS with and without DM contribution. The mass of the rotating NS is considerably changing due to rapid rotation with the frequency in the mass-shedding limit. The effects of DM are found to be important for some of the NM parameters, which are crucial for the properties of astrophysical objects.

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“…The accreted DM particles interact with baryons by exchanging standard model Higgs. The interacting Lagrangian is given in the form [38][39][40]44,56,65,66]:…”

Section: Formalism 21 Dark Matter Admixed Neutron Star Eosmentioning

confidence: 99%

“…To know its exact nature, a large number of experiments along with various theoretical modelling are carried on; a concrete picture on this DM is not yet drawn. The popular DM candidates are the weakly interacting massive particles (WIMPs) [41], Neutralino [42][43][44], feebly interacting massive particles (FIMPs) [45,46], Axions [47] etc. Recently, the Cryogenic Dark Matter Search (CDMS) experiment at Fermi lab in Illinois [48] and the Large Underground Xenon (LUX) experiment in South Dakota [49] reported the results from their searches for DM candidate particles known as WIMPs.…”

Section: Introductionmentioning

confidence: 99%

Dark Matter Effects on the Compact Star Properties

Das

Kumar

et al. 2022

Galaxies

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The neutron star properties are generally determined by the equation of state of β-equilibrated dense matter. In this work, we consider the interaction of fermionic dark matter (DM) particles with nucleons via Higgs exchange and investigate the effect on the neutron star properties with the relativistic mean-field model equation of state coupled with DM. We deduce that DM significantly affects the neutron star properties, such as considerably reducing the maximum mass of the star, which depends on the percentage of the DM considered inside the neutron star. The tidal Love numbers both for electric and magnetic cases and surficial Love numbers are also studied for DM admixed NS. We observed that the magnitude of tidal and surficial Love numbers increases with a greater DM percentage. Further, we present post-Newtonian tidal corrections to gravitational waves decreased by increasing the DM percentage. The DM effect on the GW signal is significant during the late inspiral and merger stages of binary evolution for GW frequencies >500 Hz.

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Confronting nuclear equation of state in the presence of dark matter using GW170817 observation in relativistic mean field theory approach

Cited by 66 publications

References 65 publications

Neutron-star tidal deformability and equation-of-state constraints

Neutron-star tidal deformability and equation-of-state constraints

Effects of dark matter on the nuclear and neutron star matter

Dark Matter Effects on the Compact Star Properties

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