Author:
Banks Hannah,Ansari Siyam,Vincent Aaron C.,Scott Pat
Abstract
Abstract
Asymmetric dark matter (ADM) that is captured in stars can
act as an efficient conductor of heat. Small ADM-induced changes in
a star's temperature gradient are known to alter neutrino fluxes and
asteroseismological signatures, erase convective cores and modify a
star's main sequence lifetime. The Sun's proximity to us makes it an
ideal laboratory for studying these effects. However, the two
formalisms commonly used to parametrize such heat transport were
developed over 30 years ago, and calibrated with a single set of
simulations. What's more, both are based on assumptions that break
down at the Knudsen transition, where heat transport is
maximized. We construct a Monte Carlo simulation to exactly solve
the Boltzmann collision equation, determining the steady-state
distribution and luminosity carried in stars by ADM with cross
sections that depend on velocity and momentum. We find that,
although the established (Gould & Raffelt) formalism based on local
thermal equilibrium does well for constant cross sections, the
isothermal (Spergel & Press) method actually performs better across
all models with a simple, universal rescaling function. Based on
simulation results, we provide recommendations on the
parametrization of DM heat transport in stellar evolution models.
Subject
Astronomy and Astrophysics
Cited by
6 articles.
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