Constraining Dissipative Dark Matter Self-Interactions

Research output: Journal Publications and ReviewsRGC 21 - Publication in refereed journalpeer-review

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Original languageEnglish
Article number121102
Journal / PublicationPhysical Review Letters
Volume123
Issue number12
Online published18 Sept 2019
Publication statusPublished - 20 Sept 2019
Externally publishedYes

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Abstract

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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Constraining Dissipative Dark Matter Self-Interactions. / Essig, Rouven; McDermott, Samuel D.; Yu, Hai-Bo et al.
In: Physical Review Letters, Vol. 123, No. 12, 121102, 20.09.2019.

Research output: Journal Publications and ReviewsRGC 21 - Publication in refereed journalpeer-review

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