Home > Publications database > Cosmological and idealized simulations of dark matter haloes with velocity-dependent, rare and frequent self-interactions > print

001     611515
005     20250715170717.0
024 7 _ |a 10.1093/mnras/stae699
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024 7 _ |a 0035-8711
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024 7 _ |a 1365-2966
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024 7 _ |a arXiv:2310.07750
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100 1 _ |a Fischer, Moritz S.
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245 _ _ |a Cosmological and idealized simulations of dark matter haloes with velocity-dependent, rare and frequent self-interactions
260 _ _ |a Oxford
|c 2024
|b Oxford Univ. Press
336 7 _ |a article
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336 7 _ |a Journal Article
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500 _ _ |a 17 pages, 15 figures + appendices, accepted for publication in MNRAS
520 _ _ |a 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.
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650 _ 7 |a dark matter: halo
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650 _ 7 |a mass: scale
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650 _ 7 |a dark matter: scattering
|2 INSPIRE
650 _ 7 |a differential cross section: angular dependence
|2 INSPIRE
650 _ 7 |a velocity dependence
|2 INSPIRE
650 _ 7 |a satellite
|2 INSPIRE
650 _ 7 |a dark matter: density
|2 INSPIRE
650 _ 7 |a collapse
|2 INSPIRE
650 _ 7 |a formation
|2 INSPIRE
650 _ 7 |a rotation
|2 INSPIRE
650 _ 7 |a cosmological model
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650 _ 7 |a self-force
|2 INSPIRE
650 _ 7 |a dark matter: interaction
|2 INSPIRE
650 _ 7 |a galaxy: halo
|2 INSPIRE
650 _ 7 |a numerical calculations
|2 INSPIRE
650 _ 7 |a astroparticle physics
|2 autogen
650 _ 7 |a methods: numerical
|2 autogen
650 _ 7 |a galaxies: haloes
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650 _ 7 |a dark matter
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700 1 _ |a Kasselmann, Lenard
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700 1 _ |a Ragagnin, Antonio
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700 1 _ |a Robertson, Andrew
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700 1 _ |a Schmidt-Hoberg, Kai
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773 _ _ |a 10.1093/mnras/stae699
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787 0 _ |a Fischer, Moritz S. et.al.
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|r DESY-23-154 ; arXiv:2310.07750
|t Cosmological and idealised simulations of dark matter haloes with velocity-dependent, rare and frequent self-interactions
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