Neutralinos, Big Bang Nucleosynthesis and 6Li in Low-Metallicity Stars

Details Neutralinos, Big Bang Nucleosynthesis and 6Li in Low-Metallicity Stars Neutralinos, Big Bang Nucleosynthesis and 6Li in Low-Metallicity Stars

2004-05-28

arxiv.org/abs/astro-ph/0405583v2

Phys.Rev. D70 (2004) 083510

Astronomy and Astrophysics

Astrophysics

5 pages, 3 figures, to match published version, note change of title

Scientific paper

10.1103/PhysRevD.70.083510

The synthesis of Li6 during the epoch of Big Bang nucleosynthesis (BBN) due to residual annihilation of dark matter particles is considered. By comparing the predicted Li6 to observations of this isotope in low-metallicity stars, generic constraints on s-wave dark matter annihilation rates into quarks, gauge bosons, and Higgs bosons are derived. It may be shown that, for example, wino dark matter in anomaly-mediated SUSY breaking scenarios with masses Mx < 250 GeV or light neutralinos with Mx < 20 GeV annihilating into light quarks are, taken face value, ruled out. These constraints may only be circumvented if significant Li6 depletion has occurred in all three low-metallicity stars in which this isotope has been observed to date. In general, scenarios invoking non-thermally generated neutralinos with enhanced annihilation rates for a putative explanation of cosmic ray positron or galactic center as well as diffuse background gamma-ray signals by present-day neutralino annihilation will have to face a stringent Li6 overproduction problem. On the other hand, it is possible that Li6 as observed in low-metallicity stars is entirely due to residual dark matter annihilation during BBN, even for neutralinos undergoing a standard thermal freeze-out.

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