http://arxiv.org/abs/2011.07718
Self-interacting dark matter is known to be one of the most appropriate candidates for dark matter. Due to its excellent success in removing many astrophysical problems, particularly in small scale structure, studying this model has taken on added significance. In this paper, we focus on the results of two previously performed simulations of cluster size halos with self-interacting dark matter and introduce a new function for the density profile of galaxy clusters, which can perfectly describe the result of these simulations. This density profile helps to find a velocity dispersion profile and also a relation between cluster mass and concentration parameter. Using these relations, we investigate two scaling relations of galaxy clusters, namely mass-velocity dispersion and mass-temperature relations. As an important discrepancy appears in the calculated masses for given temperatures regarding the obtained mass-temperature relation, we propose a new interacting model and show that this model can completely solve the problem. This model is a combination of self-interacting dark matter idea with another model of the dark sector in which dark matter particle mass is determined according to its interaction with dark energy. We find that in this super interacting dark sector (SIDS) model, the virial ratio changes to have higher values than $\frac{1}{2}$. Finally, we provide quantitative expressions that can describe the constants of this interacting model with the value of cross-section per unit mass of dark matter particles.
M. Naseri and J. Firouzjaee
Tue, 17 Nov 20
75/83
Comments: 20 pages, 13 figures, 3 tables
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