期刊
PHYSICAL REVIEW LETTERS
卷 123, 期 12, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.123.121102
关键词
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资金
- National Science Foundation [NSF PHY-1748958]
- U.S. Department of Energy [DE-SC0015845, DE-SC0008541, DE-SC0017938]
- Fermi Research Alliance, LLC [DE-AC02-07CH11359]
- U.S. Department of Energy, Office of Science, Office of High Energy Physics
- UCR Regents' Faculty Development Award
- U.S. Department of Energy (DOE) [DE-SC0015845, DE-SC0017938] Funding Source: U.S. Department of Energy (DOE)
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 semianalytical 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 18 dwarf galaxies that exhibit a corelike dark matter density profile, we derive constraints on the strength of the dissipative interactions and the energy loss per collision.
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