A new way to test the WIMP dark matter models. (arXiv:2011.11548v1 [astro-ph.CO])

A new way to test the WIMP dark matter models. (arXiv:2011.11548v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_W/0/1/0/all/0/1">Wei Cheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+He_Y/0/1/0/all/0/1">Yuan He</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diao_J/0/1/0/all/0/1">Jin-Wang Diao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_Y/0/1/0/all/0/1">Yu Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zeng_J/0/1/0/all/0/1">Jun Zeng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">Jia-Wei Zhang</a>

In this paper, we investigate the possibility of testing the weakly
interacting massive particle (WIMP) dark matter (DM) models by applying the
simplest phenomenological model which introduces an interaction term between
dark energy (DE) and WIMP DM, i.e., $Q = 3gamma_{DM} Hrho_{DM}$. In general,
the coupling strength $gamma_{DE}$ is close to $0$ due to the interaction
between DE and WIMP DM is very weak, thus the effect of $gamma_ {DE}$ on the
evolution of $Y$ associated with DM energy density can be safely ignored.
Meanwhile, our numerical calculation also indicates that $x_fapprox20$ is
associated with DM freeze-out temperature, which is the same as the vanishing
interaction scenario. As for DM relic density, it will be magnified by
$frac{2-3gamma_{DM}}{2}[{2pi g_* m_{DM}^3}/{(45 s_0 x_f^3})]^{gamma_{DM}}$
times, which provides a new way for us to test WIMP DM models. As an example,
we analyze the case in which WIMP DM is a scalar DM. (SGL+SNe+Hz) and
(GRBs+SNe+BAO+CMB) cosmological observations will give out
$gamma_{DM}=0.134^{+0.17}_{-0.069}$ and $gamma_{DM}=-0.0047pm0.0046$,
respectively. After further considering the constraints from both the DM direct
detection experiment and DM relic density, we observe that the allowed
parameter space of the scalar DM model will be completely excluded for the
former cosmological observations, while it will increase for the latter ones.
Those two cosmological observations lead to a paradoxical conclusion. Thus we
wish the more accuracy of the cosmological observation can be obtained in the
near future to test the WIMP DM models.

In this paper, we investigate the possibility of testing the weakly
interacting massive particle (WIMP) dark matter (DM) models by applying the
simplest phenomenological model which introduces an interaction term between
dark energy (DE) and WIMP DM, i.e., $Q = 3gamma_{DM} Hrho_{DM}$. In general,
the coupling strength $gamma_{DE}$ is close to $0$ due to the interaction
between DE and WIMP DM is very weak, thus the effect of $gamma_ {DE}$ on the
evolution of $Y$ associated with DM energy density can be safely ignored.
Meanwhile, our numerical calculation also indicates that $x_fapprox20$ is
associated with DM freeze-out temperature, which is the same as the vanishing
interaction scenario. As for DM relic density, it will be magnified by
$frac{2-3gamma_{DM}}{2}[{2pi g_* m_{DM}^3}/{(45 s_0 x_f^3})]^{gamma_{DM}}$
times, which provides a new way for us to test WIMP DM models. As an example,
we analyze the case in which WIMP DM is a scalar DM. (SGL+SNe+Hz) and
(GRBs+SNe+BAO+CMB) cosmological observations will give out
$gamma_{DM}=0.134^{+0.17}_{-0.069}$ and $gamma_{DM}=-0.0047pm0.0046$,
respectively. After further considering the constraints from both the DM direct
detection experiment and DM relic density, we observe that the allowed
parameter space of the scalar DM model will be completely excluded for the
former cosmological observations, while it will increase for the latter ones.
Those two cosmological observations lead to a paradoxical conclusion. Thus we
wish the more accuracy of the cosmological observation can be obtained in the
near future to test the WIMP DM models.

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