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What does the Dynamical Analsis of Clusters of Galaxies Tell us About Massive Neutrinos?

  • G. Des Forêts (a1), D. Gerbal (a1), G. Mathez (a1), A. Mazure (a1) and E. Salvador-Solé (a1) (a2)...

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It is often claimed that massive neutrinos (v's) can solve the “missing mass” problem, but it is not so clear in the particular case of clusters of galaxies (C.O.G.). Let us assume that the unseen matter is composed by massive v's only. If they are cosmological, the v's should obey Fermi-Dirac statistics with a density of ∼ 100 v/cm3/species. But if “relic,” the v's would be so slow (1) that they cannot exist in this form (because of the previous Jeans instability or because they are trapped in wells generated by baryonic matter). Since the time when the v's decoupled from the primeval mixture (T ∼ 3–1 MeV), the v's can be considered as a “gravitational plasma,” so that violent relaxation occurs in inhomogeneous systems, leading to a Lynden-Bell distribution defined by three parameters: ην (numerical density), Vv (r.m.s. velocity) and the v-mass, mv, all unknown. All three of these parameters are, in fact, necessary to define a state of v-matter.

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References

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1. Doroshkevich, A.G., Khlopov, Y., Sunyaev, R.A., Szalay, A.S., and Zeldovich, Ya.B. 1981, Ann. N.Y. Acad. Sci., 375, 32.
2. Gerbal, D., Mathez, G., Mazure, A., and Salvadore-Solé, E. 1982, Moriond Second Astrophysics Meeting, p. 299, Edition Frontières, Paris. des Fôrets, G., Dominguez-Tenreiro, R., Gerbal, D., Mathez, G., Mazure, A., and Salvadore-Solé, E. 1982, submitted to Ap. J.
3. White, S.D.M. 1977, M.N.R.A.S., 179, 33.
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6. Capelato, H.V., Gerbal, D., Salvador-Solé, E., Mathez, D., Mazure, A., and Roland, J. 1979, Astron. Astrophys. Suppl., 38, 295.
7. Valtonen, M.J., and Byrd, G.G. 1979, Ap. J., 230, 655.

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