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| Home > Publications database > Cosmological and idealized simulations of dark matter haloes with velocity-dependent, rare and frequent self-interactions |
| Journal Article | PUBDB-2024-04952 |
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2024
Oxford Univ. Press
Oxford
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Please use a persistent id in citations: doi:10.1093/mnras/stae699 doi:10.3204/PUBDB-2024-04952
Report No.: DESY-23-154; arXiv:2310.07750
Abstract: Dark matter self-interactions may have the capability to solve or at least mitigate small-scale problems of the cosmological standard model, Lambda cold dark matter. There are a variety of self-interacting dark matter models that lead to distinguishable astrophysical predictions and hence varying success in explaining observations. Studies of dark matter (DM) density cores on various mass scales suggest a velocity-dependent scattering cross-section. In this work, we investigate how a velocity dependence alters the evolution of the DM distribution for frequent DM scatterings and compare to the velocity-independent case. We demonstrate that these cases are qualitatively different using a test problem. Moreover, we study the evolution of the density profile of idealized DM haloes and find that a velocity dependence can lead to larger core sizes and different time-scales of core formation and core collapse. In cosmological simulations, we investigate the effect of velocity-dependent self-interaction on haloes and satellites in the mass range of ≈10^11–|$10^{14} \, \mathrm{M_\odot }$|. We study the abundance of satellites, density, and shape profiles and try to infer qualitative differences between velocity-dependent and velocity-independent scatterings as well as between frequent and rare self-interactions. We find that a strongly velocity-dependent cross-section can significantly amplify the diversity of rotation curves, independent of the angular dependence of the differential cross-section. We further find that the abundance of satellites in general depends on both the velocity dependence and the scattering angle, although the latter is less important for strongly velocity-dependent cross-sections.
Keyword(s): dark matter: halo ; mass: scale ; dark matter: scattering ; differential cross section: angular dependence ; velocity dependence ; satellite ; dark matter: density ; collapse ; formation ; rotation ; cosmological model ; self-force ; dark matter: interaction ; galaxy: halo ; numerical calculations ; astroparticle physics ; methods: numerical ; galaxies: haloes ; dark matter
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