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Galaxy Formation with Hot Dark Matter and Cosmic Strings

Published online by Cambridge University Press:  03 August 2017

Robert H. Brandenberger
Robert H. Brandenberger*
Affiliation:
Department of Physics, Brown University, Providence, R.I. 02912, USA

Extract

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Hot dark matter particles have large thermal velocities at teg and hence cannot be gravitationally bound on small scales (free streaming). In models of formation of structure based on linear adiabatic perturbations all inhomogeneities on scales smaller than the maximal free streaming length λj are washed out. The mass λj inside a bail of radius exceeds the galaxy mass. Hence in the above models galaxies can only lorm by fragmentation of larger-scale objects. This is a severe problem.

Type
Appendix 1: Poster Papers
Information
Symposium - International Astronomical Union , Volume 130: Large Scale Structures of the Universe , 1988 , pp. 560 - 561
Copyright
Copyright © Reidel 1988 

References

1) Brandenberger, R., Kaiser, N. and Turok, N., ‘Dissipationless clustering of neutrino perturbations about a cosmic string loop’, Phys. Rev. D. in press (1987).Google Scholar
2) Brandenberger, R., Kaiser, N., Schramm, D. and Turok, N., ‘Galaxy and structure formation with hot dark matter and cosmic strings’. DAMTP preprint. July 1987.Google ScholarPubMed
3) Bond, J. and Szalay, A. Ap. J. 274, 443 (1984).Google Scholar
4) Bertschinger, E. and Watts, P., MIT preprint (1987).Google Scholar