Terrestrial and martian heat flow limits on dark matter

Abstract

If dark matter is efficiently captured by a planet, energy released in its annihilation can exceed that planet's total heat output. Building on prior work, we treat Earth's composition and dark matter capture in detail and present improved limits on dark matter-nucleon scattering cross sections for dark matter masses ranging from 0.1 to 10 10 GeV. We also extend Earth limits by applying the same treatment to Mars. The scope of dark matter models considered is expanded to include spin-dependent nuclear interactions including isospin-independent, proton only, and neutron only interactions. We find that Earth and Mars heating bounds are alleviated for dark matter s-wave self-annihilation cross sections 10 −37 cm 2 .

Constraining the spin-independent elastic scattering cross section of dark matter using the Moon as a detection target and the background neutrino data

“…In particular, the upper limits for the µ + µ − , τ + τ − and bb channels are generally tighter than that obtained by considering the internal heat rate of the Moon (the Moon internal heat constraint) [9]. For a small range of the 'res- 14Al (10.3) MgO (9) Si(32.5) CaO (12) Ca (6.02) Fe (9.4) 1680-1737 2.9 same scaled by 0.097 onance dark matter mass' near 52 GeV (m χ ≈ 48 − 56 GeV), the upper limits can be constrained to σ SI p ∼ 10 −36 cm 2 , which are tighter than that obtained by considering the internal heat rate of the Earth (the Earth internal heat constraint) [20]. Furthermore, in Fig.…”

Phenomenology of magnetic black holes with electroweak-symmetric coronas

“…As discussed in [63,64], if a significant fraction of DM is captured as it passes through the Earth and then annihilates efficiently to SM particles other than neutrinos inside the Earth, the heat so generated would surpass measurements of the internal heat of the Earth. This…”

Electroweak-symmetric dark monopoles from preheating

“…5 We have not shown constraints from direct detection surface runs [56][57][58][59][60] and high-altitude detectors [61][62][63][64][65], which are generally in the gray excluded regions above the underground overburden line. Indirect detection, IceCube [66], and Earth heating via captured DM annihilations [65,67] would not provide constraints because dark monopoles annihilate primarily to the dark sector. 6 One cannot simply take the monopole coupling to be the Higgs coupling to the Φ particle, which has been done in ref.…”