dc.contributor.author | Camalich, Jorge Martin | |
dc.contributor.author | Terol-Calvo, Jorge | |
dc.contributor.author | Tolos Rigueiro, Laura | |
dc.contributor.author | Ziegler, Robert | |
dc.date.accessioned | 2022-03-11T10:02:50Z | |
dc.date.available | 2022-03-11T10:02:50Z | |
dc.date.created | 2022-02-14T15:08:59Z | |
dc.date.issued | 2021-06 | |
dc.identifier.citation | Camalich, J.M., Terol-Calvo, J., Tolos Riguiero, L., Ziegler, R. (2021) Supernova constraints on dark flavored sectors. Physical Review D, 103 (12), 1-7. | en_US |
dc.identifier.issn | 2470-0010 | |
dc.identifier.uri | https://hdl.handle.net/11250/2984557 | |
dc.description.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. | en_US |
dc.language.iso | eng | en_US |
dc.publisher | American Physical Society | en_US |
dc.rights | Navngivelse 4.0 Internasjonal | * |
dc.rights.uri | http://creativecommons.org/licenses/by/4.0/deed.no | * |
dc.subject | fysikk | en_US |
dc.title | Supernova constraints on dark flavored sectors | en_US |
dc.type | Peer reviewed | en_US |
dc.type | Journal article | en_US |
dc.description.version | publishedVersion | en_US |
dc.subject.nsi | VDP::Matematikk og Naturvitenskap: 400::Fysikk: 430::Astrofysikk, astronomi: 438 | en_US |
dc.source.pagenumber | 1-7 | en_US |
dc.source.volume | 103 | en_US |
dc.source.journal | Physical Review D | en_US |
dc.source.issue | 12 | en_US |
dc.identifier.doi | 10.1103/PhysRevD.103.L121301 | |
dc.identifier.cristin | 2001435 | |
cristin.ispublished | true | |
cristin.fulltext | original | |
cristin.qualitycode | 1 | |