Cooling in a Dissipative Dark Sector
arXiv:1705.10341 · doi:10.1103/PhysRevD.96.123001
Abstract
The possibility of a subdominant component of dark matter dissipating energy could lead to dramatic new phenomenology such as the formation of a dark disk. One rigorous way to assess this possibility and settle the debate on its feasibility is to include the dissipative dark component in a numerical hydrodynamical simulation. A necessary input to such a simulation is a prescription including energy dissipation rates of different processes and rates of processes that change the number densities of dark ions and atoms. In this article, we study the simplest dissipative dark sector which consists of a dark electron and proton, both charged under a dark gauged U(1). We present approximate analytic formulas for energy loss rates due to Compton scattering, bremsstrahlung, recombination, collisional ionization and collisional excitation as well as the rates of number density change. We also include the heating rate due to photoionization. The work serves as the first step to realize a numerical simulation including a dissipative dark sector, which hopefully can shed more light on the formation and properties of a dark disk originating from dark matter self-interactions.
25 pages, 5 figures
References in corpus (6)
- The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
- Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
- Properties of galaxies reproduced by a hydrodynamic simulation
- Hidden Sector Hydrogen as Dark Matter: Small-scale Structure Formation Predictions and the Importance of Hyperfine Interactions
- Dark Matter as a Trigger for Periodic Comet Impacts
- Supersymmetric Partially Interacting Dark Matter