Constraining Dissipative Dark Matter Self-Interactions [electronic resource]
We study the gravothermal evolution of dark matter halos in the presence of dissipative dark matter self-interactions. Dissipative interactions are present in many particle-physics realizations of the dark-sector paradigm and can significantly accelerate the gravothermal collapse of halos compared t...
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Online Access (via OSTI) |
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| Format: | Government Document Electronic eBook |
| Language: | English |
| Published: |
Washington, D.C. : Oak Ridge, Tenn. :
United States. Department of Energy. High Energy Physics Division ; distributed by the Office of Scientific and Technical Information, U.S. Department of Energy,
2018.
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| Summary: | We study the gravothermal evolution of dark matter halos in the presence of dissipative dark matter self-interactions. Dissipative interactions are present in many particle-physics realizations of the dark-sector paradigm and can significantly accelerate the gravothermal collapse of halos compared to purely elastic dark matter self-interactions. This is the case even when the dissipative interaction timescale is longer than the free-fall time of the halo. Using a semi-analytical fluid model calibrated with isolated and cosmological $N$-body simulations, we calculate the evolution of the halo properties -- including its density profile and velocity dispersion profile -- as well as the core-collapse time as a function of the particle model parameters that describe the interactions. A key property is that the inner density profile at late times becomes cuspy again. Using 21 dwarf galaxies that exhibit a core-like dark matter density profile, we derive constraints on the strength of the dissipative interactions and the energy loss per collision. |
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| Item Description: | Published through SciTech Connect. 09/04/2018. "arxiv:1809.01144" " fermilab-pub-18-437-a" "1692779" TBD FT. Essig, Rouven; Yu, Hai-Bo; Zhong, Yi-Ming; Mcdermott, Samuel. |