2026-09-15T14:23:56Zhttps://gredos.usal.es/oai/requestoai:gredos.usal.es:10366/1375442026-01-12T16:17:23Zcom_10366_4092com_10366_4055com_10366_3946com_10366_3823col_10366_4093
Gestión del Repositorio Documental de la Universidad de Salamanca
author
Pérez García, María Ángeles
author
Albertus, C.
author
Masip, M.
2018-05-25T14:11:17Z
2018-05-25T14:11:17Z
2015-12-17
C. Albertus, M. Masip, M.A. Pérez-García,
Production of unstable heavy neutrinos in proto-neutron stars,
Physics Letters B,
Volume 751,
2015,
Pages 209-214,
ISSN 0370-2693,
https://doi.org/10.1016/j.physletb.2015.10.026.
(https://www.sciencedirect.com/science/article/pii/S0370269315007777)
0370-2693
http://hdl.handle.net/10366/137544
10.1016/j.physletb.2015.10.026
[EN] We discuss the production of a class of heavy sterile neutrinos nu(h) in proto-neutron stars. The neutrinos, of mass around 50 MeV, have a negligible mixing with the active species but relatively large dimension-5 electromagnetic couplings. In particular, a magnetic dipole moment mu approximate to 10(-6) GeV-1 implies that they are thermally produced through e(+)e(-) -> (nu) over bar (h)nu(h) in the early phase of the core collapse, whereas a heavy-light transition moment mu(tr) approximate to 10(-8) GeV-1 allows their decay nu(h) -> nu i gamma with a lifetime around 10(-3) s. This type of electromagnetic couplings has been recently proposed to explain the excess of electron-like events in baseline experiments. We show that the production and decay of these heavy neutrinos would transport energy from the central regions of the star to distances d approximate to 400 km, providing a very efficient mechanism to enhance the supernova shock front and heat the material behind it. (C) 2015 The Authors. Published by Elsevier B.V.
eng
Attribution-NonCommercial-NoDerivs 4.0 International
Dark-Matter
Physics
Supernova explosions
Production of unstable heavy neutrinos in photo-neutron stars
info:eu-repo/semantics/article
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