Abstract
The core-cusp problem remains a challenging discrepancy between observations and simulations in the standard CDM model for the formation of galaxies. The problem is that CDM simulations predict a steep power-law mass density profile at the center of galactic dark matter halos. However, observations of dwarf galaxies in the Local Group reveal a density profile consistent with a nearly flat distribution of dark matter near the center. A number of solutions to this dilemma have been proposed. Here, we summarize investigations into the possibility that the dark matter particles themselves self interact and scatter. Such self-interacting dark matter (SIDM) particles can smooth out the dark-matter profile in high-density regions. We also review the theoretical proposal that self-interacting dark matter may arise as an additional Higgs scalar in the 3-3-1 extension of the Standard Model (SM). We present new simulations of galaxy formation and evolution for this formulation of self-interacting dark matter. Current constraints on this self-interacting dark matter are then summarized.
Original language | English |
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Article number | 2130001 |
Journal | Modern Physics Letters A |
Volume | 36 |
Issue number | 3 |
DOIs | |
State | Published - Jan 30 2021 |
Externally published | Yes |
Funding
This work was supported by the U.S. Department of Energy under Nuclear Theory grant DEFG02-95-ER40934, and the Institute for Cosmic Ray Research (ICRR) International University Research Program G08. Lan Q. Nguyen gratefully acknowledges support from the Simons Center for Geometry and Physics, Stony Brook University at which some of the research for this paper was performed.
Keywords
- Dark matter
- galaxies, core-cusp problems