Direct and Indirect Detection of Dark Matter

Details Direct and Indirect Detection of Dark Matter Direct and Indirect Detection of Dark Matter

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.4005c&link_type=abstract

American Astronomical Society, 182nd AAS Meeting, #40.05; Bulletin of the American Astronomical Society, Vol. 25, p.860

Astronomy and Astrophysics

Astronomy

Scientific paper

The gravitationally required dark matter may consist of three components: hadronic, hot, and cold, each requiring specific detection techniques. Since visible matter is <1% of the universe critical density, but 2--8% is allowed by nucleosynthesis, much of the missing hadronic matter is likely to be in the form of objects between 10(-7) and 10(-1) solar masses. These are being searched for by microlensing using ~ 10(7) stars in the LMC as sources. Hot dark matter has to be deduced from terrestrial non-accelerator and accelerator neutrino experiments. Cold dark matter (CDM) in the form of axions is being searched for via conversion to microwave photons in a magnetic field. If the CDM is made up of WIMPs, the massive particles may annihilate in the sun or earth and produce neutrinos which can be detected underground. Alternatively, these particles can hit detector nuclei underground and the recoil energy measured in the form of ionization and phonons. The status of all these experiments will be discussed.

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