Properties of fermionic dark stars at finite temperature

In Cold Collisionless Dark Matter (CCDM) models, the impact of the temperature is to weaken the stiffness of the Equation of State (EoS) of dark matter (DM). Few discrepancies between the CDDM predictions with observations on a smaller scale such as galactic and sub-galactic structure was reported....

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Bibliographic Details
Main Authors: Aprilia, A., Sulaksono, A.
Format: Conference Proceeding
Language:English
Subjects:
Bosons
Dark matter
Entropy
Equations of state
Fermions
Galactic structure
Stiffness
Online Access:Get full text
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Summary:In Cold Collisionless Dark Matter (CCDM) models, the impact of the temperature is to weaken the stiffness of the Equation of State (EoS) of dark matter (DM). Few discrepancies between the CDDM predictions with observations on a smaller scale such as galactic and sub-galactic structure was reported. The interacting DM is one of the possible answers to this issue. Here we study the impact of finite temperature on dark stars (DSs) composed by interacting fermion dark particles for the cases of fixed temperature and fixed entropy. We assume that the self-interaction among the fermionic dark particles is through the exchange of scalar and vector bosons, and we also use the relativistic mean-field (RMF) model to obtain the EoSs. The Tolman Oppenheimer Volkoff (TOV) equation is used to calculate the mass and radius of DS. For fixed entropy, we use entropy with a range of 5–7, while for a fixed temperature, we use temperature with a variety of 30–50 MeV. In general, we have found that the effects of increasing temperature and entropy make the DS EoS softer, and as the consequences are the maximum mass and the corresponding radius increase.
ISSN:0094-243X
1551-7616
DOI:10.1063/5.0007856