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Analyzing Fermionic Dark Matter scenarios with anomalous compact objects

Yaiza Cano, Jose Manuel Alarcón

Abstract

In this paper, we consider three compact objects (HESS J1731-347, PSR J1231-1411, XTE J1814-338) with anomalous mass-radius relation to analyze the possibility of being dark matter admixed neutron stars. We try to infer the dark matter particle properties, under the assumption of behaving as a free Fermi gas. The main novelty relies on the use of a baryonic equation of state obtained from first principles in the whole density range, that allows to eliminate the model dependence of the baryonic part of the calculation. Once the possible Dark Matter Admixed Neutron Star configurations are obtained, we check their stability and whether it is feasible for a Neutron Star to capture the necessary dark matter fraction. We show that two of the anomalous compact objects (HESS J1731-347 and PSR J1231-1411) can be explained with a small fraction of fermionic dark matter content in the star. The other compact object (XTE J1814-338) cannot be explained as a dark matter admixed neutron star, and becomes a potential candidate for a twin star.

Analyzing Fermionic Dark Matter scenarios with anomalous compact objects

Abstract

In this paper, we consider three compact objects (HESS J1731-347, PSR J1231-1411, XTE J1814-338) with anomalous mass-radius relation to analyze the possibility of being dark matter admixed neutron stars. We try to infer the dark matter particle properties, under the assumption of behaving as a free Fermi gas. The main novelty relies on the use of a baryonic equation of state obtained from first principles in the whole density range, that allows to eliminate the model dependence of the baryonic part of the calculation. Once the possible Dark Matter Admixed Neutron Star configurations are obtained, we check their stability and whether it is feasible for a Neutron Star to capture the necessary dark matter fraction. We show that two of the anomalous compact objects (HESS J1731-347 and PSR J1231-1411) can be explained with a small fraction of fermionic dark matter content in the star. The other compact object (XTE J1814-338) cannot be explained as a dark matter admixed neutron star, and becomes a potential candidate for a twin star.
Paper Structure (17 sections, 10 equations, 19 figures, 6 tables)

This paper contains 17 sections, 10 equations, 19 figures, 6 tables.

Table of Contents

  1. Introduction
  2. Methodology
  3. Baryonic Matter EoS
  4. Dark Matter EoS
  5. Hydrostatic equilibrium
  6. Stability Analysis
  7. DM content analysis
  8. Results
  9. $\mathbf{m_{DM} = 100}$ GeV
  10. $\mathbf{m_{DM} = 10}$ GeV
  11. $\mathbf{m_{DM} = 1}$ GeV
  12. $\mathbf{m_{DM} = 100}$ MeV
  13. $\mathbf{m_{DM} = 10}$ MeV
  14. $\mathbf{m_{DM} = 1}$ MeV
  15. Dark Matter content in a Neutron Star
  16. ...and 2 more sections

Figures (19)

  • Figure 1: Logarithmic plot of the baryonic equations of state used in this work.
  • Figure 2: Baryonic equations of state used in this work.
  • Figure 3: Mass-radius diagrams generated from the EoSs used in this work.
  • Figure 4: DM equations of state used in this work.
  • Figure 5: In this figure, we show the effect of the different fractions and different DM particle mass on the mass-radius diagram for one of the baryonic EoS.
  • ...and 14 more figures