Prompt cusps delay core formation by a factor of ~2 in SIDM halos but later collapse tracks align after rescaling, with ~5% late-stage deviations depending on concentration and outer velocity dispersion.
A parametric model for self-interacting dark mat- ter halos
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Core-collapsed SIDM halos produce longer FRB image time delays than CDM halos, enabling future surveys to constrain self-interaction cross sections above roughly 18-40 cm²/g depending on collapse timing.
Two-component SIDM with velocity-dependent inter- and intra-species interactions produces mass segregation that forms dwarf cores and boosts small-scale strong lensing efficiency by a factor of a few.
MW-mass SIDM halos bypass core formation and enter immediate core collapse due to baryonic preconditioning, allowing the compact stellar disk and bulge to survive close pericenter passages while the diffuse halo is more easily disrupted.
1D hydrodynamic simulations find that SIDM heat transport competes with gravity to regulate black hole accretion, enabling rapid growth in SIS profiles up to 10,000 solar masses from a 100 solar mass seed in 2 Myr.
citing papers explorer
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Role of prompt cusps in driving the core collapse of SIDM halos
Prompt cusps delay core formation by a factor of ~2 in SIDM halos but later collapse tracks align after rescaling, with ~5% late-stage deviations depending on concentration and outer velocity dispersion.
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Self-Interacting Dark Matter with Mass Segregation: A Unified Explanation of Dwarf Cores and Small-Scale Lenses
Two-component SIDM with velocity-dependent inter- and intra-species interactions produces mass segregation that forms dwarf cores and boosts small-scale strong lensing efficiency by a factor of a few.