On the evaporation of solar dark matter: spin-independent effective operators

TL;DR

This paper investigates how spin-independent dark matter interactions affect solar dark matter evaporation, using Monte Carlo simulations to improve accuracy and exploring implications for detection and the solar abundance problem.

Contribution

It introduces a non-thermal Monte Carlo approach to evaluate solar DM evaporation for SI operators, providing more reliable results than Maxwellian assumptions.

Findings

Determines minimum DM masses detectable via solar neutrinos.

Shows evaporation effects are significant for momentum-dependent asymmetric DM.

Provides parameter space for solar DM detection based on SI operators.

Abstract

As a part of the effort to investigate the implications of dark matter (DM)-nucleon effective interactions on the solar DM detection, in this paper we focus on the evaporation of the solar DM for a set of the DM-nucleon spin-independent (SI) effective operators. In order to put the evaluation of the evaporation rate on a more reliable ground, we calculate the non-thermal distribution of the solar DM using the Monte Carlo methods, rather than adopting the Maxwellian approximation. We then specify relevant signal parameter spaces for the solar DM detection for various SI effective operators. Based on the analysis, we determine the minimum DM masses for which the DM-nucleon coupling strengths can be probed from the solar neutrino observations. As an interesting application, our investigation also shows that evaporation effect can not be neglectd in a recent proposal aiming to solve the solar abundance problem by invoking the momentum-dependent asymmetric DM in the Sun.