Cross section calculations in theories of self-interacting dark matter

Girmohanta, Sudhakantha; Shrock, Robert

doi:10.1103/physrevd.106.063013

Cited by 14 publications

(29 citation statements)

References 88 publications

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“…We restrict to the case where α χ is small enough so that lowest-order perturbation theory provides a reliable description of the physics. As was shown in [82], the parameter choice used there satisfies this restriction while simultaneously yielding sufficient depletion of the χ number density in the early universe to produce the assumed number asymmetry in our ADM model. For further de-tails on our model, we refer the reader to [82].…”

Section: Cross Sectionsmentioning

confidence: 92%

“…First, we review the basic properties of the SIDM model with asymmetric dark matter that we used in [82]. In this model, the dark matter particle χ is a spin-1/2 Dirac fermion, and the mediator, ξ, is a real scalar, ξ = φ, or a vector, ξ = V .…”

Section: Cross Sectionsmentioning

confidence: 99%

“…(For an example of how this mixing can be suppressed in a DM model with specified ultraviolet physics, see, e.g., [83].) In [82] the illustrative set of values m χ = 5 GeV, m ξ = 5 MeV, and α χ = 3 × 10 −4 was used. Below we will show that this choice is consistent with the fit to astronomical data that we perform here.…”

Section: Cross Sectionsmentioning

confidence: 99%

“…For all the relevant data, the values of v rel are nonrelativistic (NR). In [82] we calculated the differential cross section in the center-of-mass (CM), dσ CM /dΩ, for the reaction (1.1) with both scalar and vector mediators in the regime where the Born approximation is valid. In the NR limit relevant to fitting data, the results for the scalar and vector mediators are equal and are [82]…”

Section: Cross Sectionsmentioning

confidence: 99%

“…However, a common practice in the literature was to include only the t-channel contribution, and fits to data were done with the resultant cross section. In [82], we presented differential and integrated cross sections for the reaction (1.1) with both the t-channel and u-channel terms properly included and discussed the differences with respect to previous calculations that included only the t-channel. (See also [81] for a related field-theoretic discussion and [73] for an analysis via solutions of the Schrödinger equation for potential scattering.)…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Fitting a Self-Interacting Dark Matter Model to Data Ranging From Satellite Galaxies to Galaxy Clusters

Girmohanta¹,

Shrock²

2022

Preprint

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We present a fit to observational data in an asymmetric self-interacting dark matter model using our recently calculated cross sections that incorporate both t-channel and u-channel exchanges in the scattering of identical particles. We find good fits to the data ranging from dwarf galaxies to galaxy clusters, and equivalent relative velocities from ∼ 20 km/sec to > ∼ 10 3 km/s. We compare our results with previous fits that used only t-channel exchange contributions to the scattering.

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Section: Cross Sectionsmentioning

confidence: 92%

Section: Cross Sectionsmentioning

confidence: 99%

Section: Cross Sectionsmentioning

confidence: 99%

Section: Cross Sectionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Fitting a Self-Interacting Dark Matter Model to Data Ranging From Satellite Galaxies to Galaxy Clusters

Girmohanta¹,

Shrock²

2022

Preprint

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Gravothermal evolution of dark matter halos with differential elastic scattering

Yang

2022

J. Cosmol. Astropart. Phys.

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We study gravothermal evolution of dark matter halos in the presence of differential self-scattering that has strong velocity and angular dependencies. We design controlled N-body simulations to model Rutherford and Møller scatterings in the halo, and follow its evolution in both core-expansion and -collapse phases. The simulations show the commonly-used transfer cross section underestimates the effects of dark matter self-interactions, but the viscosity cross section provides an accurate approximation for modeling angular-dependent dark matter scattering. We investigate thermodynamic properties of the halo, and find that the three moments of the Boltzmann equation under the fluid approximation are satisfied. We further propose a constant effective cross section, which integrates over the halo's characteristic velocity dispersion with weighting kernels motivated by kinetic theory of heat conduction. The effective cross section provides a good approximation to differential self-scattering for most of the halo evolution. It indicates that we can map astrophysical constraints on a constant self-interacting cross section to an SIDM model with velocity- and angular-dependent scatterings.

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A parametric model for self-interacting dark matter halos

Yang,

Nadler,

et al. 2024

J. Cosmol. Astropart. Phys.

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We propose a parametric model for studying self-interacting dark matter (SIDM) halos. The model uses an analytical density profile, calibrated using a controlled N-body SIDM simulation that covers the entire gravothermal evolution, including core-forming and -collapsing phases. By normalizing the calibrated density profile, we obtain a universal description for SIDM halos at any evolution phase. The model allows us to infer properties of SIDM halos based on their cold dark matter (CDM) counterparts. As a basic application, we only require two characteristic parameters of an isolated CDM halo at z = 0. We then extend the model to incorporate effects induced by halo mass changes, such as major mergers or tidal stripping, making it applicable to both isolated halos and subhalos. The parametric model is tested and validated using cosmological zoom-in SIDM simulations available in the literature.

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Cross section calculations in theories of self-interacting dark matter

Cited by 14 publications

References 88 publications

Fitting a Self-Interacting Dark Matter Model to Data Ranging From Satellite Galaxies to Galaxy Clusters

Fitting a Self-Interacting Dark Matter Model to Data Ranging From Satellite Galaxies to Galaxy Clusters

Gravothermal evolution of dark matter halos with differential elastic scattering

A parametric model for self-interacting dark matter halos

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