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Constraining Dissipative Dark Matter Self-Interactions.

Rouven Essig1, Samuel D McDermott2, Hai-Bo Yu3

  • 1C.N. Yang Institute for Theoretical Physics, Stony Brook University, Stony Brook, New York 11794, USA.

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|October 22, 2019
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Summary
This summary is machine-generated.

Dissipative dark matter self-interactions accelerate halo collapse. This study constrains these interactions using dwarf galaxy data, revealing how dark matter halo evolution is impacted by energy loss mechanisms.

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Area of Science:

  • Cosmology
  • Astrophysics
  • Particle Physics

Background:

  • Dark matter halos are fundamental structures in cosmic evolution.
  • Dissipative dark matter self-interactions are proposed in various particle physics models.
  • These interactions can influence halo structure and dynamics.

Purpose of the Study:

  • To investigate the gravothermal evolution of dark matter halos with dissipative self-interactions.
  • To quantify the impact of these interactions on halo collapse times and profiles.
  • To constrain the parameters of dissipative dark matter models using observational data.

Main Methods:

  • Utilizing a semianalytical fluid model.
  • Calibrating the model with isolated and cosmological N-body simulations.
  • Analyzing density and velocity dispersion profiles of simulated halos.
  • Comparing model predictions with observational data from dwarf galaxies.

Main Results:

  • Dissipative interactions significantly accelerate halo gravothermal collapse compared to elastic interactions.
  • The inner dark matter density profile becomes cuspy again at late times.
  • Constraints are derived for the strength of dissipative interactions and energy loss per collision.

Conclusions:

  • Dissipative dark matter self-interactions play a crucial role in dark matter halo evolution.
  • The observed core-like profiles in dwarf galaxies can be explained by these interactions.
  • This research provides a pathway to test particle physics models of dark matter.