Dissipation in SIDM halos inverts heat conduction, suppresses isothermal cores, and explains an observed strong lens perturber with smaller cross sections or shorter times than the elastic case.
Uni- versal gravothermal evolution of isolated self-interacting dark matter halos for velocity-dependent cross-sections
7 Pith papers cite this work. Polarity classification is still indexing.
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Non-equilibrium relativistic SIDM halo collapse produces seed black holes of mass ~3e-8 of the halo mass at apparent horizon formation.
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.
SIDM core-collapse simulations produce a dense central core matching the lensing perturber, while CDM requires an IMBH with extreme tidal mass loss whose realism is left open.
N-body simulations with Arepo calibrate the β parameter in the SIDM gravothermal model, showing it is independent of cross-section, concentration, and mass for velocity-independent scattering, and introduce an effective β model for the long-mean-free-path regime.
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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Cooling, conduction, compact objects: Gravothermal evolution of dissipative self-interacting dark matter halos
Dissipation in SIDM halos inverts heat conduction, suppresses isothermal cores, and explains an observed strong lens perturber with smaller cross sections or shorter times than the elastic case.
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Non-Equilibrium Relativistic Core Collapse of Self-Interacting Dark Matter Halos -- Limits On Seed Black Hole Mass
Non-equilibrium relativistic SIDM halo collapse produces seed black holes of mass ~3e-8 of the halo mass at apparent horizon formation.
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Probing Collapsed Dark Matter Halos with Fast Radio Bursts
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.
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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.
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SIDM and CDM interpretations of the million-solar-mass lensing perturber JVAS B1938+666-$\mathcal{V}$
SIDM core-collapse simulations produce a dense central core matching the lensing perturber, while CDM requires an IMBH with extreme tidal mass loss whose realism is left open.
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Calibrating the SIDM Gravothermal Catastrophe with N-body Simulations
N-body simulations with Arepo calibrate the β parameter in the SIDM gravothermal model, showing it is independent of cross-section, concentration, and mass for velocity-independent scattering, and introduce an effective β model for the long-mean-free-path regime.
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Spherically Symmetric Fluid Simulations of Black Hole Accretion in Self-Interacting Dark Matter Halos
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.