Primordial Black Hole Merger Rate in Self-Interacting Dark Matter Halo Models. (arXiv:2106.06265v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Fakhry_S/0/1/0/all/0/1">Saeed Fakhry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naseri_M/0/1/0/all/0/1">Mahdi Naseri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Firouzjaee_J/0/1/0/all/0/1">Javad T. Firouzjaee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farhoudi_M/0/1/0/all/0/1">Mehrdad Farhoudi</a>
We study the merger rate of primordial black holes (PBHs) in the
self-interacting dark matter (SIDM) halo models. To explore a numerical
description for the density profile of the SIDM halo models, we use the result
of a previously performed simulation for the SIDM halo models with
$sigma/m=10~cm^{2}g^{-1}$. We also propose a concentration-mass-time relation
that can explain the evolution of the halo density profile related to the SIDM
models. Furthermore, we investigate the encounter condition of PBHs that may
have been distributed in the medium of dark matter halos randomly. Under these
assumptions, we calculate the merger rate of PBHs within each halo considering
the SIDM halo models and compare the results with the one obtained for the cold
dark matter (CDM) halo models. To do this, we employ the definition of the time
after halo virtualization as a function of halo mass. We indicate that the
merger rate of PBHs for the SIDM halo models, for $f_{rm PBh}>0.32$, can
generate sufficient PBH mergers in a way that those exceed the one resulted
from the CDM halo models. By considering the spherical-collapse halo mass
function, we obtain similar results for the cumulative merger rate of PBHs.
Moreover, we calculate the redshift evolution of the PBH total merger rate. To
determine a constraint on the PBH abundance, we study the merger rate of PBHs
in terms of their fraction and masses and compare those with the black hole
merger rate estimated by the Advanced LIGO (aLIGO) detectors during the third
observing run. The results demonstrate that within the context of the SIDM halo
models during the second epoch, the merger rate of $10~M_{odot}-10~M_{odot}$
events falls within the aLIGO window. We also estimate a relation between the
fraction of PBHs and their masses, which is well consistent with our findings.
We study the merger rate of primordial black holes (PBHs) in the
self-interacting dark matter (SIDM) halo models. To explore a numerical
description for the density profile of the SIDM halo models, we use the result
of a previously performed simulation for the SIDM halo models with
$sigma/m=10~cm^{2}g^{-1}$. We also propose a concentration-mass-time relation
that can explain the evolution of the halo density profile related to the SIDM
models. Furthermore, we investigate the encounter condition of PBHs that may
have been distributed in the medium of dark matter halos randomly. Under these
assumptions, we calculate the merger rate of PBHs within each halo considering
the SIDM halo models and compare the results with the one obtained for the cold
dark matter (CDM) halo models. To do this, we employ the definition of the time
after halo virtualization as a function of halo mass. We indicate that the
merger rate of PBHs for the SIDM halo models, for $f_{rm PBh}>0.32$, can
generate sufficient PBH mergers in a way that those exceed the one resulted
from the CDM halo models. By considering the spherical-collapse halo mass
function, we obtain similar results for the cumulative merger rate of PBHs.
Moreover, we calculate the redshift evolution of the PBH total merger rate. To
determine a constraint on the PBH abundance, we study the merger rate of PBHs
in terms of their fraction and masses and compare those with the black hole
merger rate estimated by the Advanced LIGO (aLIGO) detectors during the third
observing run. The results demonstrate that within the context of the SIDM halo
models during the second epoch, the merger rate of $10~M_{odot}-10~M_{odot}$
events falls within the aLIGO window. We also estimate a relation between the
fraction of PBHs and their masses, which is well consistent with our findings.
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