Lumped-element axion dark matter detection beyond the magnetoquasistatic limit

Tensor Detection Severely Constrains Axion Dark Matter

Axion BEC Dark Matter

Cold dark matter axions thermalize through gravitational self-interactions and form a BoseEinstein condensate when the photon temperature reaches approximately 500 eV. Axion Bose-Einstein condensation provides an opportunity to distinguish axions from the other dark matter candidates on the basis of observation. The rethermalization of axions that are about to fall in a galactic potential well ...

Mixed axion-wino dark matter

A variety of supersymmetric models give rise to a split mass spectrum characterized by very heavy scalars but sub-TeV gauginos, usually with a wino-like LSP. Such models predict a thermally-produced underabundance of wino-like WIMP dark matter so that non-thermal DM production mechanisms are necessary. We examine the case where theories with a wino-like LSP are augmented by a Peccei-Quinn secto...

Wimp and Axion Dark Matter

There is almost universal agreement among cosmologists that most of the matter in the Universe is dark, and there are very good reasons to believe that most of this dark matter must be nonbaryonic. The two leading candidates for this dark matter are axions and weakly-interacting massive particles (WIMPs), such as the neutralino in supersymmetric extensions of the standard model. I discuss the a...

Axion hot dark matter bounds

The masses of the lightest particles are best constrained by the largest cosmic structures. The well-established method of using cosmological precision data to constrain the cosmic hot dark matter fraction [1, 2] has been extended to hypothetical low-mass particles, notably to axions, in several papers [3, 4, 5, 6, 7]. If axions thermalize after the QCD phase transition, their number density is...