Asymmetric WIMP dark matter

By M. Graesser, I. Shoemaker, L. Vecchi. 2011

185 citations recorded by the source corpus.

In existing dark matter models with global symmetries the relic abundance of dark matter is either equal to that of anti-dark matter (thermal WIMP), or vastly larger, with essentially no remaining anti-dark matter (asymmetric dark matter). By exploring the consequences of a primordial asymmetry on the coupled dark matter and anti-dark matter Boltzmann equations we find large regions of parameter space that interpolate between these two extremes. Interestingly, this new asymmetric WIMP framework can accommodate a wide range of dark matter masses and annihilation cross sections. The present-day dark matter population is typically asymmetric, but only weakly so, such that indirect signals of dark matter annihilation are not completely suppressed. We apply our results to existing models, noting that upcoming direct detection experiments will constrain a large region of the relevant parameter space.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8dd895a2f3dce0add4bf1a945a2d8a751bce9030

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Alexander Pukhov
2. G. B'elanger
3. Fawzi Boudjema
4. A. Semenov
5. Tongyan Lin
6. P. Schuster
7. Matthew McCullough
8. A. Pochinsky

In Atomic and Molecular Physics, and Optics

1. Alexander Pukhov
2. G. B'elanger
3. William Detmold
4. Tongyan Lin

In Nuclear and High Energy Physics

1. Alexander Pukhov
2. G. B'elanger
3. Fawzi Boudjema
4. A. Semenov
5. Tongyan Lin
6. G. Krnjaic
7. N. Toro
8. P. Schuster

Citations in the corpus

• WIMP dark matter candidates and searches—current status and future prospects (2017, background): “n absence of any mass degeneracy. In this case the nal DM relic density can be increased with respect to the non-degenerate scenario. On the other hand in the (partially) asymmetric DM (ADM) scenario [86,87] one can accommodate an otherwise too low ˜h2 by assuming that one component of the DM relic ”
• Dark matter, millicharges, axion and scalar particles, gauge bosons, and other new physics with LDMX (2018, background): “See also [132, 133] for a discussion.”
• Dark matter models and direct detection (2019, background): “The relic density then depends on both the annihilation rate and the asymmetry [49, 50].”
• Dark nuclei. I. Cosmology and indirect detection (2014, background): “is strongly coupled, seems plausible. In this case, the relic abundance of the symmetric component is suppressed by a factor ˘exp(˙ Ann=˙ Th) where the latter is the standard thermal DM cross section [80]. This is a result of continued annihilations with the asymmetric component. With the symmetric ”
• An Introduction to Particle Dark Matter (2019, unknown): “[43].”
• micrOMEGAs_3: A program for calculating dark matter observables (2013, background): “The Boltzmann equations for the abundance of a DM particle –defined as the number density divided by the entropy density - have to be generalized [38, 39, 40].”