Speaker
Description
The WIMP indirect detection signal is enhanced by the square of the WIMP density, and celestial bodies can catalyze WIMP annihilation by accumulating WIMPs with their gravitational potential. In particular, WIMP annihilation can induce a GeV neutrino signal from the Sun, the increase of the total luminosity of White Dwarfs in nearby Globular Clusters, or a sizeable radio emission from the Dark Matter cusp in the Black Hole of low--mass X--ray binaries. I will discuss how such signals can be complementary to direct detection to probe the WIMP thermal decoupling scenario and, in particular, how they allow to obtain bounds that do not depend on the WIMP velocity distribution.
Due to new telescope technologies in the next few years it will become possible to search for WIMPs using a growing list of stars and planets. To make this task easier I introduce WimPyCapture, a new module of the WimPyDD code (wimpydd.hepforge.org ) that will soon be released for the calculation of the capture rate of WIMPS by generic celestial bodies in the single scatter or optically thin regime. The module will be fully integrated in WimPyDD and will allow to combine WIMP direct detection and capture in celestial bodies in virtually any scenario, including inelastic scattering, an arbitrary WIMP spin and a generic WIMP velocity distribution in the Galactic halo. WimPyCapture will include templates for the calculation of the WIMP capture rate in different celestial bodies such as the Earth, the Sun, Jupiter-like planets, main-sequence stars, brown and white dwarfs, allowing the user to extend the range of celestial targets in a straightforward way.
