Endothermic self-interacting dark matter in Milky Way-like dark matter haloes

Author:

O’Neil Stephanie1ORCID,Vogelsberger Mark12ORCID,Heeba Saniya3,Schutz Katelin3,Rose Jonah C4ORCID,Torrey Paul4ORCID,Borrow Josh1ORCID,Low Ryan5ORCID,Adhikari Rakshak5,Medvedev Mikhail V56,Slatyer Tracy R127,Zavala Jesús8

Affiliation:

1. Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139, USA

2. The NSF AI Institute for Artificial Intelligence and Fundamental Interactions, Massachusetts Institute of Technology , Cambridge, MA 02139, USA

3. Department of Physics & McGill Space Institute, McGill University , Montréal, QC H3A 2T8, Canada

4. Department of Astronomy, University of Florida , Gainesville, FL 32611, USA

5. Department of Physics and Astronomy, University of Kansas , Lawrence, KS 66045, USA

6. Laboratory for Nuclear Science, Massachusetts Institute of Technology , Cambridge, MA 02139, USA

7. Center for Theoretical Physics, Massachusetts Institute of Technology , Cambridge, MA 02139, USA

8. Centre for Astrophysics and Cosmology, Science Institute, University of Iceland , Dunhagi 5, 107 Reykjavik, Iceland

Abstract

ABSTRACT Self-interacting dark matter (SIDM) offers the potential to mitigate some of the discrepancies between simulated cold dark matter (CDM) and observed galactic properties. We introduce a physically motivated SIDM model to understand the effects of self interactions on the properties of Milky Way and dwarf galaxy sized haloes. This model consists of dark matter with a nearly degenerate excited state, which allows for both elastic and inelastic scattering. In particular, the model includes a significant probability for particles to up-scatter from the ground state to the excited state. We simulate a suite of zoom-in Milky Way-sized N-body haloes with six models with different scattering cross sections to study the effects of up-scattering in SIDM models. We find that the up-scattering reaction greatly increases the central densities of the main halo through the loss of kinetic energy. However, the physical model still results in significant coring due to the presence of elastic scattering and down-scattering. These effects are not as apparent in the subhalo population compared to the main halo, but the number of subhaloes is reduced compared to CDM.

Funder

NASA

National Science Foundation

NSERC

U.S. Department of Energy

Simons Foundation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 2 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

1. Inelastic freeze-in;Physical Review D;2023-11-08

2. The role of baryons in self-interacting dark matter mergers;Monthly Notices of the Royal Astronomical Society;2023-06-14

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