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dc.contributor.authorPérez García, María Ángeles
dc.contributor.authorAlbertus, C.
dc.contributor.authorMasip, M.
dc.identifier.citationAlbetus, C., Masip, M., Pérez-García M.Á. (2015). Production of unstable heavy neutrinos in proto-neutron stars. Physics letters B, 751. Retrieved from Web of Science database.es_ES
dc.description.abstract[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.es_ES
dc.publisherElsevier Science Publishers (Amsterdam, Países Bajos)es_ES
dc.rightsAttribution-NonCommercial-NoDerivs 4.0 International
dc.subjectSupernova explosionses_ES
dc.titleProduction of unstable heavy neutrinos in photo-neutron starses_ES

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