Non‐perturbative Effect on Thermal Relic Abundance of Dark Matter

By J. Hisano, S. Matsumoto, M. Nagai, Osamu Saito, Masato Senami. 2006

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We point out that thermal relic abundance of dark matter is strongly altered by a non‐perturbative effect called the Sommerfeld enhancement, when constituent particles of the dark matter are SU(2)L non‐singlet and much heavier than the weak gauge bosons. Typical candidates are the heavy wino and higgsino. We investigate the non‐perturbative effect on the relic abundance of dark matter for the wino as an example. We show that its thermal abundance is reduced by 50% compared to the perturbative result. The wino mass consistent with the observed dark matter abundance turns out to be 2.7 TeV

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9c0f36db4c14af96f4a91c2cd1ef47294ec9211d

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Citations in the corpus

Wino dark matter under siege (2013, methodology): “plus SE calculation of [4] that is used to compute the cross sections presented in all the above figures (referred to as “tree-level-SE”), and the O ( g(8) ) perturbative calculation without any SE contribution (referred to as “one-loop-perturbative”).”
Self-Interacting Dark Matter from a Non-Abelian Hidden Sector (2014, background): “[92] J.”
Direct detection of electroweak-interacting dark matter (2011, background): “annihilation cross section of EW-IMP [11, 12] should be included [ 10 ].”
Weak Corrections are Relevant for Dark Matter Indirect Detection (2010, background): “This generic situation is realized in the region of the MSSM parameter space where DM could be the neutral component of the fermionic wino weak triplet with a value of the mass M ∼ 3 TeV dictated by the cosmological DM relic density [26, 29].”
Naturalness and the Status of Supersymmetry (2013, background): “For example, for mixed Bino-Higgsino [35–37] and pure Wino-like [38] neutralino dark matter, the upper bounds are”
Cosmological implications of Dark Matter bound states (2017, background): “Anyhow, this channel is not attractive enough to form a bound state, so that the sign change has a minor impact, as shown by comparing figure 5a with [3, 4].”
Dark Matter's secret liaisons: phenomenology of a dark U(1) sector with bound states (2016, background): “On the other hand, for DM masses larger than ∼10 TeV the constraints quickly lose power because the maximal energy of the Ams-02 data and because the annihilation cross section decreases.”
Non-abelian dark sectors and their collider signatures (2009, unknown): “GeV introduces a Sommerfeld enhancement [13, 14, 15, 16], giving a boost factor of the right size to enhance the DM annihilation cross-section2.”
In wino veritas? Indirect searches shed light on neutralino dark matter (2013, methodology): “In the plot, we also plotted the wino thermal relic abundance calculated in [21, 22].”