Super Interacting Dark Sector: An Improvement on Self-Interacting Dark
  Matter via Scaling Relations of Galaxy Clusters
  Self-interacting dark matter is known as 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 sized 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. The scaling
relations reveal that in the self-interacting dark matter model, halos are more
massive than what the standard non-interacting model predicts for any fixed
temperature. We also study the mass-temperature relation for a hybrid
interacting model, which 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. This super
interacting dark sector (SIDS) model can change the mass-temperature relation
to a modified form that has the same result as a non-interacting model.
Finally, we provide quantitative expressions which can describe the constants
of this interacting model with the value of cross-section per unit mass of dark
matter particles.
