Dark matter

All sensible cosmologies strive to understand and interpret the observable material universe. Observation documents the distribution of matter, classified according to perceived masses, distances and relative motion. Interpretation reduces observation to theoretical notions on the interaction between condensed and separated massive bodies. The end product is a catalogue of celestial bodies and the necessary interactions that dictate their relative equilibrium distribution in space. 

It is difficult to explain how a cosmology, which claims that only one percent of cosmic matter is observable by any means, can be considered a cosmology at all. But that is precisely the current status of the standard big-bang theory. What it means is that the theoretical model has no observational basis. If cosmology pretends to explain this dark matter it should do better than characterize it as WlMPs - Weakly Interacting Massive Particles. 

The notion of dark matter hrst emerged as a proposed resolution of Zwicky s paradox. Today, together with its cousin, dark energy, it is the panacea that cures all big-bang ailments (Turner, 2000). It even works where inflation fails and because it dehes detection can safely be assigned any desired attribute, without fear of contradiction. 

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Nomially the amplitude of the total incident field (or intensity of the incident light) is such that the light/matter coupling energies are sufficiently weak not to compete seriously with the dark matter Hamiltonian. As already noted, when this is tire case, tlie induced polarization, P is treated perturbatively in orders of the total electric field. Thus one writes... 

In addition to ordinai y matter, scientists have evidence for the existence in the universe of dark matter. Some of the dark matter is ordinai y matter, such as dust in outer space and planets going around other stars. Astronomers cannot see ordinai y dark matter because any light coming from such matter is too faint to be observed in telescopes. However, most of the dark matter in the universe is believed not to be ordinary matter. At the present time it is not known what this mysterious dark matter is, or what it is made of. Scientists know that this dark matter exists because it exerts a gravitational force on stars (which are made of ordinary matter), causing the stars to move faster than they otherwise would. According to present estimates, there is perhaps five times as much dark matter in the universe as ordinary matter. 

Or anyone for that matter, although these days there is a good deal of talk of dark matter which is not featured... 

Jorgensen CK, Kauffmann GB (1990) Crookes and Marignac - A Centennial of an Intuitive and Pragmatic Appraisal of Chemical Elements and the Present Astrophysical Status of Nucleosynthesis and Dark Matter . 73 227-254 Jorgensen CK, Reisfeld R (1982) Uranyl Photophysics. 50 121-171... 

Kerr, Philip. Dark matter. Random House. 

Neutrino Mass, Dark Matter, Gravitational Waves, Condensation of Atoms and Monopoles, Light Cone Quantization... 

James E. Peebles, professor emeritus at Princeton (2001), offers his own description. He states that at present the house of cosmological theories resembles scaffolding which is solidly assembled but still has large gaps. The open questions are those of dark matter , inflation and quintessence . We live in exciting times for cosmology. ... 

Galaxies consist mainly of dark matter built up from exotic particles. Satisfactory Much indirect evidence, but the particles still have to be discovered and alternative theories disproved. 

But we can t be too smug. We must avoid the mistake of the physicist who, as the twentieth century began, stated confidently that we knew all there was to know about physics, that science just needed to clean up a few dusty corners. Then came relativity, quantum theory, the Big Bang, and now dark matter, dark energy and string theory. Similarly in the life sciences, the more we learn, the better we understand how little we really know. There remains a vast landscape to explore, with great questions remaining. 

Heavy but diffuse halos of dark matter are considered, an initial mass of 108Mq is assumed (Mb/Mb = 10). 

The search for weakly interacting particle, which may constitute the dark matter in the universe. The elucidation of the nature of this dark matter is one of the most pressing problems in astrophysics and in cosmology. 

Dark matter searches with detector arrays up to several tens of kilograms. 

In a cryogenic experiment, one or several detectors are used for a definite goal for which they have been optimized. For example, in CUORE experiment described in Section 16.5, the sensors are the Ge thermistors, i.e. thermometers used in a small temperature range (around 10 mK). One detector is a bolometer made up of an absorber and a Ge sensor. The experiment is the array of 1000 bolometers arranged in anticoincidence circuits for the detection of the neutrinoless double-beta decay. Note that the sensors, if calibrated, could be used, as well, as very low-temperature thermometers. Also the array of bolometers can be considered a single large detector and used for different purposes as the detection of solar axions or dark matter. 

LTD-1 Low Temperature Detectors for Neutrinos and Dark Matter Proceedings of a Workshop, Field at Ringberg Castle, Tegernsee, May 12-13, 1987, ed. by K. Pretzl, N. Schmitz, L. Stodolsky, Springer-Verlag, Berlin, Heidelberg (December 1987)... 

LTD-2 Low Temperature Detectors for Neutrinos and Dark Matter II Proceedings of the Second European Workshop on Low Temperature Devices for the Detection of Low Energy Neutrinos and Dark Matter, Annecy-le-Vieux, France, May 2-6, 1988, ed. by L. Gonzales-Mestres and D. Perret-Gallix, Gif-sur-Yvette, France, Editions Frontieres (1988)... 

LTD-4 Proc. 4th Int. Conf. of Low Temperature Dark Matter and Neutrino Detectors, Oxford 1991, ed. by N.E. Booth and G.L. Salmon, Editions Frontieres, Gif-sur-Yvette, France (1992)... 

H. Wulandari et al. Neutron Background Studies for the CRESST Dark Matter Experiment, hep-... 

Update of the Proposal to LNGS for a Second Phase of the CRESST Dark Matter Search, MPI-PhE/ 2001-02... 

The other kind of dark matter must be non-baryonic (NDM) and is thought to consist of some kind of particles envisaged in extensions of the Standard Model ... 

The existence of dark matter (either baryonic or non-baryonic) is inferred from its gravitational effects on galactic rotation curves, the velocity dispersions and hydrostatic equilibrium of hot (X-ray) gas in clusters and groups of galaxies, gravitational lensing and departures from the smooth Hubble flow described by Eq. (4.1). This dark matter resides at least partly in the halos of galaxies such as our... 

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