arXiv : Dark Matter Effects On Neutron Star Properties

Ellis, John; Kannike, Kristjan; Raidal, Martti; Vaskonen, Ville; Marzola, Luca; Hütsi, Gert

doi:10.1103/PhysRevD.97.123007

Article
Report number	arXiv:1804.01418 ; CERN-TH-2018-072 ; KCL-PH-TH/2018-13 ; KCL-PH-TH-2018-13
Title	Dark Matter Effects On Neutron Star Properties
Author(s)	Ellis, John (NICPB, Tallinn ; King's Coll. London ; CERN) ; Hütsi, Gert (NICPB, Tallinn ; Tartu U.) ; Kannike, Kristjan (NICPB, Tallinn) ; Marzola, Luca (NICPB, Tallinn) ; Raidal, Martti (NICPB, Tallinn) ; Vaskonen, Ville (NICPB, Tallinn)
Publication	2018-06-15
Imprint	2018-04-04
Number of pages	7
Note	* Temporary entry * 7 pages, 4 figures; minor changes to match the published version
In:	Phys. Rev. D 97 (2018) 123007
DOI	10.1103/PhysRevD.97.123007
Subject category	nucl-th ; Nuclear Physics - Theory ; hep-ph ; Particle Physics - Phenomenology ; astro-ph.CO ; Astrophysics and Astronomy
Abstract	We study possible effects of a dark matter (DM) core on the maximum mass of a neutron star (NS), on the mass-radius relation and on the NS tidal deformability parameter $\Lambda$. We show that all these quantities would in general be reduced in the presence of a DM core. In particular, our calculations indicate that the presence of a DM core with a mass fraction $\sim 5\%$ could affect significantly the interpretation of these NS data as constraints on the nuclear equation of state (EOS), potentially excluding some EOS models on the basis of the measured mass of PSR J0348+0432, while allowing other EOS models to become consistent with the LIGO/Virgo upper limit on $\Lambda$. Specific scenarios for generating such DM cores are explored in an Appendix.
Copyright/License	preprint: (License: arXiv nonexclusive-distrib 1.0) Publication: © 2018-2024 authors

$Effects of DM cores on the mass-radius relation for NSs. The color code denotes the different baryonic EOSs considered~\cite{Engvik:1995gn,Potekhin:2013qqa,Muther:1987xaa,Lackey:2005tk,Alford:2004pf,Akmal:1998cf,Douchin:2001sv,Mueller:1996pm}. The solid lines are for cases in which a NS contains no DM, whereas the dashed lines include the effect of a DM core contributing to 5\% of the total NS mass and $\sqrt{\sigma_{\rm D}}/m_{\rm D}^3 = 0.05\,{\rm GeV}^{-2}$. The horizontal lines show the bounds on the maximal NS mass $1.97 M_\odot < M_{\rm max} < 2.33 M_\odot$ inferred, respectively, by observations of PSR J0348+0432~\cite{Antoniadis:2013pzd} and an analysis of GW170817~\cite{Rezzolla:2017aly}, assuming that its merger product was a black hole.$ $The lighter regions show the parameter space where DM forms a core inside the NS, assuming the H4 EOS for the nuclear component. In the darker regions, to the contrary, the DM halo envelops a baryonic NS core. White areas are excluded by the stability constraint. All the plots are for a baryonic mass of $M_{\rm N} = 1.4M_\odot$. The left panel shows the sound velocities $c_{\rm N}$ and $c_{\rm D}$ in the baryonic and DM components, respectively, at the center of the NS. The middle panel shows the radii $R_{\rm N}$ and $R_{\rm D}$ of the baryonic and DM components, respectively, and the right panel shows the tidal deformability $\Lambda$. In each panel {the red dashed and dot-dashed curves show the contours $\Lambda=400$, and $\Lambda=800$, respectively.}$ $The lighter regions show the parameter space where DM forms a core inside the NS, assuming the H4 EOS for the nuclear component. In the darker regions, to the contrary, the DM halo envelops a baryonic NS core. White areas are excluded by the stability constraint. All the plots are for a baryonic mass of $M_{\rm N} = 1.4M_\odot$. The left panel shows the sound velocities $c_{\rm N}$ and $c_{\rm D}$ in the baryonic and DM components, respectively, at the center of the NS. The middle panel shows the radii $R_{\rm N}$ and $R_{\rm D}$ of the baryonic and DM components, respectively, and the right panel shows the tidal deformability $\Lambda$. In each panel {the red dashed and dot-dashed curves show the contours $\Lambda=400$, and $\Lambda=800$, respectively.}$ Show more plots

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