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The impact of baryonic potentials on the gravothermal evolution of self-interacting dark matter haloes
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The presence of a central baryonic potential can have a significant impact on the gravothermal evolution of self-interacting dark matter (SIDM) haloes. We extend a semi-analytical fluid model to incorporate the influence of a static baryonic potential and calibrate it using controlled N-body simulations. We construct benchmark scenarios with varying baryon concentrations and different SIDM models, including constant and velocity-dependent self-interacting cross sections. The presence of the baryonic potential induces changes in SIDM halo properties, including central density, core size, and velocity dispersion, and it accelerates the halo's evolution in both expansion and collapse phases. Furthermore, we observe a quasi-universality in the gravothermal evolution of SIDM haloes with the baryonic potential, resembling a previously known feature in the absence of the baryons. By appropriately rescaling the physical quantities that characterize the SIDM haloes, the evolution of all our benchmark cases exhibits remarkable similarity. Our findings offer a framework for testing SIDM predictions using observations of galactic systems where baryons play a significant dynamical role.
Forward citations
Cited by 5 Pith papers
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Cold Dark Matter and Self-Interacting Dark Matter Interpretations of Cloud-9
Cloud-9's gas profile can be fit by both cuspy CDM and cored SIDM halos, but matching cosmological halo concentrations favors SIDM with σ/m ≈ 200 cm²/g at about 3σ tension versus 7σ for CDM.
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MARVELously Dark: the density profile evolution of dwarf halos in velocity-dependent SIDM
In a new SIDM simulation of isolated dwarf halos, nine low-mass halos are core-collapsed, and inner density slope—rather than central density—best tracks collapse onset and matches analytic collapse-time predictions.
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Strong-lensing Perturber Signatures in Self-interacting Dark Matter Simulations
Core-collapsed self-interacting dark matter halos in the Concerto simulations reach high enough central densities to match the perturbing masses inferred in J0946, B1938, SDP.81, and SPT2147-50.
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Dark Bondi Accretion Aided by Baryons and the Origin of JWST Little Red Dots
Gravothermal collapse in self-interacting dark matter halos, aided by brief baryonic Eddington accretion, can grow solar-mass seeds to 10^7 solar-mass black holes within about 500 million years, explaining JWST little...
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Constraints on dark matter self-interaction from velocity distribution function in isolated halos
N-body simulations and rotation-curve data constrain the dark matter self-interaction cross-section to σ/m ≤ 2.7 cm²/g at 95% C.L. for Milky Way-scale halos.
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