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Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR,Astrophysics, Cosmology and Extragalactic Astrophysics, astro-ph.CO,High Energy Physics - Phenomenology, hep-ph
Abstract:
So far, direct detection searches have come empty handed in their quest for
Dark Matter (DM). Meanwhile, asteroseismology arises as a complementary tool to
study DM, as its accumulation in a star can enhance energy transport, by
providing a conduction mechanism, producing significant changes in the stellar
structure during the course of the star's evolution. The stellar core,
particularly affected by the presence of DM, can be investigated through
precise asteroseismic diagnostics. We modelled three stars including DM energy
transport: the Sun, a slightly less massive and much older star, KIC 7871531
($0.85 \, M_{\odot}$, $9.41 \, \text{Gyr}$), and a more massive and younger
one, KIC 8379927 ($1.12 \, M_{\odot}$, $1.82 \, \text{Gyr}$). We considered
both the case of Weakly Interactive Massive Particles, albeit with a low
annihilation, and the case of Asymmetric DM for which the number of trapped
particles in the star can be much greater. By analysing these models with
asteroseismic separation ratios weighted towards the core, we found indications
limiting the effective spin-dependent DM-proton coupling for masses of a few
GeV. This independent result is very close to the most recent and most
stringent direct detection DM constraints.
