REVIEW 3 cited by
The Structure of Dissipative Dark Matter Halos
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
read the original abstract
Dissipative dark matter self-interactions can affect halo evolution and change its structure. We perform a series of controlled N-body simulations to study impacts of the dissipative interactions on halo properties. The interplay between gravitational contraction and collisional dissipation can significantly speed up the onset of gravothermal collapse, resulting in a steep inner density profile. For reasonable choices of model parameters controlling the dissipation, the collapse timescale can be a factor of 10-100 shorter than that predicted in purely elastic self-interacting dark matter. The effect is maximized when energy loss per collision is comparable to characteristic kinetic energy of dark matter particles in the halo. Our simulations provide guidance for testing the dissipative nature of dark matter with astrophysical observations.
Forward citations
Cited by 3 Pith papers
-
Dark Matter and Baryon Asymmetry from Monopole-Axion Interactions
A rotating QCD axion dissipates kinetic energy via dark monopole dyon transitions, explaining dark matter and baryon asymmetry with a predicted axion decay constant below 10^9 GeV.
-
Extended Color Twin Higgs
A Twin Higgs model with visible-only SU(4) color breaking predicts new Z', charge-1/6 vectors and charge-1/2 fermions, with reduced tuning, lower ΔNeff, and bosonic twin baryon dark matter.
-
Dynamical Evolutions in Globular Clusters and Dwarf Galaxies: Conduction Fluid Simulations
A two-fluid conduction model of stars plus collisionless dark matter predicts that most globular clusters have undergone mass segregation and core collapse on a Hubble time, whereas most dwarf galaxies have not.
Discussion (0). Continue with ORCID to comment.