Review of Asymmetric Dark Matter

Petraki, Kalliopi; Volkas, Raymond R.

doi:10.1142/s0217751x13300287

Cited by 524 publications

(537 citation statements)

References 353 publications

Supporting

Mentioning

536

Contrasting

Order By: Relevance

“…DM masses below the weak scale are also allowed provided the ratio α X /m X remains fixed [23]. Alternately, DM may be asymmetric, such that X andX are populated unequally in the early Universe due to a primordial X-number asymmetry [63][64][65]. In this case, annihilation still plays a crucial role for depleting the symmetric density of X andX, leaving behind the residual asymmetric component composed of X only.…”

Section: Particle Physics Of Self-interacting Dark Mattermentioning

confidence: 99%

Direct detection portals for self-interacting dark matter

Kaplinghat

Tulin²,

Yu³

2014

Phys. Rev. D

165

229

View full text Add to dashboard Cite

Dark matter self-interactions can affect the small scale structure of the Universe, reducing the central densities of dwarfs and low surface brightness galaxies in accord with observations. From a particle physics point of view, this points toward the existence of a 1 − 100 MeV particle in the dark sector that mediates self-interactions. Since mediator particles will generically couple to the Standard Model, direct detection experiments provide sensitive probes of self-interacting dark matter. We consider three minimal mechanisms for coupling the dark and visible sectors: photon kinetic mixing, Z boson mass mixing, and the Higgs portal. Self-interacting dark matter motivates a new benchmark paradigm for direct detection via momentum-dependent interactions, and ton-scale experiments will cover astrophysically motivated parameter regimes that are unconstrained by current limits. Direct detection is a complementary avenue to constrain velocity-dependent self-interactions that evade astrophysical bounds from larger scales, such as those from the Bullet Cluster.

show abstract

Section: Particle Physics Of Self-interacting Dark Mattermentioning

confidence: 99%

Direct detection portals for self-interacting dark matter

Kaplinghat

Tulin²,

Yu³

2014

Phys. Rev. D

165

229

View full text Add to dashboard Cite

show abstract

“…Other promising DM candidates such as the sterile neutrino or the gravitino have higher primordial velocities, pushing the regime of power suppression to larger scales where it becomes relevant for galaxy surveys such as in the case of warm or mixed DM. More exotic scenarios like interacting DM (Boehm & Schaeffer 2005), self-interacting DM (Spergel & Steinhardt 2000), asymmetric DM (Petraki & Volkas 2013), or ultra-light axion DM (Marsh & Silk 2013) can also lead to suppressed power at rather large scales either because they interact with the cosmic plasma, with dark radiation or because they undergo scalar field oscillations on astrophysical scales. Since the power suppression of different DM scenarios happens at different scales and is of varying shape, it is crucial to properly quantify the nonlinear clustering in this regime in order to distinguish between different DM species and to contribute towards a solution of one of the outstanding puzzles in modern physics.…”

Section: Introductionmentioning

confidence: 99%

Structure formation with suppressed small-scale perturbations

Schneider

2015

Monthly Notices of the Royal Astronomical Society

143

215

View full text Add to dashboard Cite

All commonly considered dark matter scenarios are based on hypothetical particles with small but non-zero thermal velocities and tiny interaction cross-sections. A generic consequence of these attributes is the suppression of small-scale matter perturbations either due to free-streaming or due to interactions with the primordial plasma. The suppression scale can vary over many orders of magnitude depending on particle candidate and production mechanism in the early Universe.While nonlinear structure formation has been explored in great detail well above the suppression scale, the range around suppressed perturbations is still poorly understood. In this paper we study structure formation in the regime of suppressed perturbations using both analytical techniques and numerical simulations. We develop simple and theoretically motivated recipes for the halo mass function, the expected number of satellites, and the halo concentrations, which are designed to work for power spectra with suppression at arbitrary scale and of arbitrary shape. As case studies, we explore warm and mixed dark matter scenarios where effects are most distinctive. Additionally, we examine the standard dark matter scenario based on weakly interacting massive particles (WIMP) and compare it to pure cold dark matter with zero primordial temperature. We find that our analytically motivated recipes are in good agreement with simulations for all investigated dark matter scenarios, and we therefore conclude that they can be used for generic cases with arbitrarily suppressed small-scale perturbations.

show abstract

“…These collider limits can be circumvented if the model features a 'light' mediator state [1][2][3]22] (relative to collider energies i.e. 100 GeV for LHC searches).…”

Section: Direct and Indirect Detectionmentioning

confidence: 99%

“…In such models the DM, which we denote here B , has an (approximately) conserved quantum number (which we also call B ). The relic density is determined by a particle-antiparticle asymmetry between B and B , in direct analogy to baryons [1][2][3]. If the DM has a similar mass to the proton m B ∼ m p and the hidden and visible sectors are connected via portal operators which violate B, L and B , but conserve some linear combination, then this can explain the cosmological coincidence Ω DM ∼ 5Ω B .…”

Section: Introductionmentioning

confidence: 99%

Annihilation signals from asymmetric dark matter

Hardy

Lasenby

Unwin

2014

J. High Energ. Phys.

View full text Add to dashboard Cite

Abstract:In the simplest models of asymmetric dark matter (ADM) annihilation signals are not expected, since the DM is non-self-conjugate and the relic density of anti-DM is negligible. We investigate a new class of models in which a symmetric DM component, in the 'low-mass' 1-10 GeV regime favoured for linking the DM and baryon asymmetries, is repopulated through decays. We find that, in models without significant velocity dependence of the annihilation cross section, observational constraints generally force these decays to be (cosmologically) slow. These late decays can give rise to gamma-ray signal morphologies differing from usual annihilation profiles. A distinctive feature of such models is that signals may be absent from dwarf spheroidal galaxies.

show abstract

Review of Asymmetric Dark Matter

Cited by 524 publications

References 353 publications

Direct detection portals for self-interacting dark matter

Direct detection portals for self-interacting dark matter

Structure formation with suppressed small-scale perturbations

Annihilation signals from asymmetric dark matter

Contact Info

Product

Resources

About