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  • Letter
  • Open Access

Supernova constraints on dark flavored sectors

Jorge Martin Camalich1,2, Jorge Terol-Calvo1,2,3, Laura Tolos4,5,6,7, and Robert Ziegler8

  • 1Instituto de Astrofísica de Canarias, C/ Vía Láctea, s/n E38205—La Laguna (Tenerife), Spain
  • 2Universidad de La Laguna, Departamento de Astrofísica, La Laguna, E-38206 Tenerife, Spain
  • 3Instituto de Física Corpuscular (CSIC-Universitat de València), C/ Catedrático José Beltrán 2, E-46980 Paterna (València), Spain
  • 4Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, 08193 Barcelona, Spain
  • 5Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Spain
  • 6Frankfurt Institute for Advanced Studies, Ruth-Moufang-Str. 1, 60438 Frankfurt am Main, Germany
  • 7Faculty of Science and Technology, University of Stavanger, 4036 Stavanger, Norway
  • 8Institut für Theoretische Teilchenphysik, Karlsruhe Institute of Technology, 76131 Karlsruhe, Germany

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Phys. Rev. D 103, L121301 – Published 4 June, 2021

DOI: https://doi.org/10.1103/PhysRevD.103.L121301

Abstract

Proto-neutron stars forming a few seconds after core-collapse supernovae are hot and dense environments where hyperons can be efficiently produced by weak processes. By making use of various state-of-the-art supernova simulations combined with the proper extensions of the equations of state including Λ hyperons, we calculate the cooling of the star induced by the emission of dark particles X0 through the decay Λ→nX0. Comparing this novel energy-loss process to the neutrino cooling of SN 1987A allows us to set a stringent upper limit on the branching fraction, BR(Λ→nX0)≤8×10−9, that we apply to massless dark photons and axions with flavor-violating couplings to quarks. We find that the new supernova bound can be orders of magnitude stronger than other limits in dark-sector models.

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Phys. Rev. D 103, L121301– Published 4 June, 2021
  • Received 11 January 2021
  • Revised 24 March 2021
  • Accepted 3 May 2021
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