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Title: Evaporation and scattering of momentum- and velocity-dependent dark matter in the Sun

Abstract

Dark matter with momentum- or velocity-dependent interactions with nuclei has shown significant promise for explaining the so-called Solar Abundance Problem, a longstanding discrepancy between solar spectroscopy and helioseismology. The best-fit models are all rather light, typically with masses in the range of 3–5 GeV. This is exactly the mass range where dark matter evaporation from the Sun can be important, but to date no detailed calculation of the evaporation of such models has been performed. Here we carry out this calculation, for the first time including arbitrary velocity- and momentum-dependent interactions, thermal effects, and a completely general treatment valid from the optically thin limit all the way through to the optically thick regime. We find that depending on the dark matter mass, interaction strength and type, the mass below which evaporation is relevant can vary from 1 to 4 GeV. This has the effect of weakening some of the better-fitting solutions to the Solar Abundance Problem, but also improving a number of others. As a by-product, we also provide an improved derivation of the capture rate that takes into account thermal and optical depth effects, allowing the standard result to be smoothly matched to the well-known saturation limit.

Authors:
 [1];  [2]; ;  [3]
  1. ARC Centre of Excellence for Particle Physics at the Terascale, School of Physics, The University of Melbourne, Swanston St and Tin Alley, Victoria 3010 (Australia)
  2. SISSA and INFN, Sezione di Trieste, Via Bonomea 265, 34136 Trieste (Italy)
  3. Department of Physics, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ (United Kingdom)
Publication Date:
OSTI Identifier:
22667632
Resource Type:
Journal Article
Resource Relation:
Journal Name: Journal of Cosmology and Astroparticle Physics; Journal Volume: 2017; Journal Issue: 10; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABUNDANCE; BY-PRODUCTS; CAPTURE; EVAPORATION; GEV RANGE; INTERACTIONS; MASS; NONLUMINOUS MATTER; NUCLEI; SATURATION; SCATTERING; SPECTROSCOPY; SUN; TEMPERATURE DEPENDENCE; VELOCITY; VISIBLE RADIATION

Citation Formats

Busoni, Giorgio, Simone, Andrea De, Scott, Pat, and Vincent, Aaron C., E-mail: giorgio.busoni@unimelb.edu.au, E-mail: andrea.desimone@sissa.it, E-mail: p.scott@imperial.ac.uk, E-mail: aaron.vincent@imperial.ac.uk. Evaporation and scattering of momentum- and velocity-dependent dark matter in the Sun. United States: N. p., 2017. Web. doi:10.1088/1475-7516/2017/10/037.
Busoni, Giorgio, Simone, Andrea De, Scott, Pat, & Vincent, Aaron C., E-mail: giorgio.busoni@unimelb.edu.au, E-mail: andrea.desimone@sissa.it, E-mail: p.scott@imperial.ac.uk, E-mail: aaron.vincent@imperial.ac.uk. Evaporation and scattering of momentum- and velocity-dependent dark matter in the Sun. United States. doi:10.1088/1475-7516/2017/10/037.
Busoni, Giorgio, Simone, Andrea De, Scott, Pat, and Vincent, Aaron C., E-mail: giorgio.busoni@unimelb.edu.au, E-mail: andrea.desimone@sissa.it, E-mail: p.scott@imperial.ac.uk, E-mail: aaron.vincent@imperial.ac.uk. Sun . "Evaporation and scattering of momentum- and velocity-dependent dark matter in the Sun". United States. doi:10.1088/1475-7516/2017/10/037.
@article{osti_22667632,
title = {Evaporation and scattering of momentum- and velocity-dependent dark matter in the Sun},
author = {Busoni, Giorgio and Simone, Andrea De and Scott, Pat and Vincent, Aaron C., E-mail: giorgio.busoni@unimelb.edu.au, E-mail: andrea.desimone@sissa.it, E-mail: p.scott@imperial.ac.uk, E-mail: aaron.vincent@imperial.ac.uk},
abstractNote = {Dark matter with momentum- or velocity-dependent interactions with nuclei has shown significant promise for explaining the so-called Solar Abundance Problem, a longstanding discrepancy between solar spectroscopy and helioseismology. The best-fit models are all rather light, typically with masses in the range of 3–5 GeV. This is exactly the mass range where dark matter evaporation from the Sun can be important, but to date no detailed calculation of the evaporation of such models has been performed. Here we carry out this calculation, for the first time including arbitrary velocity- and momentum-dependent interactions, thermal effects, and a completely general treatment valid from the optically thin limit all the way through to the optically thick regime. We find that depending on the dark matter mass, interaction strength and type, the mass below which evaporation is relevant can vary from 1 to 4 GeV. This has the effect of weakening some of the better-fitting solutions to the Solar Abundance Problem, but also improving a number of others. As a by-product, we also provide an improved derivation of the capture rate that takes into account thermal and optical depth effects, allowing the standard result to be smoothly matched to the well-known saturation limit.},
doi = {10.1088/1475-7516/2017/10/037},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 10,
volume = 2017,
place = {United States},
year = {Sun Oct 01 00:00:00 EDT 2017},
month = {Sun Oct 01 00:00:00 EDT 2017}
}