Late-phase-transition-induced fluctuations in the cosmic neutrino distribution and the formation of structure in the Universe

Details Late-phase-transition-induced fluctuations in the cosmic neutrino distribution and the formation of structure in the Universe Late-phase-transition-induced fluctuations in the cosmic neutrino distribution and the formation of structure in the Universe

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992phrvd..45.2595f&link_type=abstract

Physical Review D (Particles, Fields, Gravitation, and Cosmology), Volume 45, Issue 8, 15 April 1992, pp.2595-2600

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Particle-Theory And Field-Theory Models Of The Early Universe, Applications Of Electroweak Models To Specific Processes

Scientific paper

We show that late-time (Tc<=1 eV) cosmic vacuum phase transitions which induce separation of phases and which involve a discontinuity in neutrino properties (e.g., mass) across phase boundaries could give rise to spatial inhomogeneities in the distribution of neutrinos. The nucleation physics of the phase transition would determine the spatial scale of the fluctuations. These density perturbations would be born in the nonlinear regime and could have masses in the range of 106Msolar-1013Msolar. If the fluctuations are shells, as expected, and there is gravitational modification of the original phase-transition nucleation scale then the upper limit on their masses could be considerably larger (~=1018Msolar), possibly encompassing the largest structures in the Universe. The motivation for this work stems, in part, from the possibility that future experiments (i.e., solar neutrino experiments) may suggest new, low-energy-scale weak-interaction phenomena, such as neutrino flavor mixing.

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