Publication:
Explaining pulsars high peculiar velocities - a viable particle physics solution

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dc.contributor.authorZuluaga Callejas, Jorge Iván
dc.contributor.otherNardi, Enrico
dc.date.accessioned2024-01-18T20:45:07Z
dc.date.available2024-01-18T20:45:07Z
dc.date.issued2001-03-01
dc.description1 documento
dc.description.abstractUna explicación convincente de las velocidades peculiares de los pulsares todavía nos es esquiva. Se presenta en este trabajo la hipótesis que cualquier solución de la física de partículas debe probablemente implicar la producción resonante de un neutrino no interactuante Vs de masa mvs rv 20-50 keV. Se propone aquí un modelo donde un campo magnético anisotrópico induce una asimetría en la conversion por resonant spin flavour precession de antineutrinos tauónicos en neutrinos esteriles Vs ' Para campos magnéticos internos de Bint 2: 1015 G un momento magnético de transición iJT-VS del orden de 10-12 magnetones de Bohr es requerido. La emisión asimétrica de Vs desde el núcleo de una su pernova (donde se forman los pulsares) puede producir un empuje apreciable sobre el núcleo y explicar velocidades de retroceso de algunos centenares de kilómetros por segundo.spa
dc.description.tableofcontents1 Introduction 7 1.1 Observational Evidences 8 1.2 Selection effects 14 1.3 Results ... 15 1.4 Correlations 16 2 Physics of Pulsar Kicks 19 2.1 The Collapse of Stellar Core 20 2.2 Astrophysical Mechanisms 25 2.2.1 Symmetric Explosion Scenario 26 2.2.2 Asymmetric Explosion Scenario 28 2.3 Partic1e Physics Mechanisms . . . . . . 31 2.4 Neutrino propagation in magnetized matter 32 2.5 Macroscopic parity violation in supernova 35 2.6 Neutrino oscillations . . .. 36 2.6.1 Vacuum oscillations . 36 2.6.2 Matter enhanced oscillations . 38 2.7 Resonant spin-flavor precession 44 2.8 Deformed neutrinospheres 46 3 Asymmetric emission of lis 49 3.1 The mechanism and its viability . . . . . . . . . . . . . . . . . 50 6 CONTENTS 3.2 Numerical Model and Simulation 3.2.1 The proto-neutron star model 3.2.2 The Algorithm . . . . . 3.2.3 The computational code 4 Results and Conclusions 4.1 Results . . . 4.2 Conclusions A The computational code A.1 Main routine . A.2 Other rout ines .spa
dc.format.mimetypeapplication/pdf
dc.identifier.urihttps://repositorio.minciencias.gov.co/handle/20.500.14143/50319
dc.language.isospa
dc.publisherUniversidad de Antioquia
dc.publisherColciencias
dc.publisher.placeMedellín
dc.rights.accessrightsinfo:eu-repo/semantics/openAccess
dc.rights.creativecommonsAtribución 4.0 Internacional (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subject.armarcInvestigación científica
dc.subject.lembProyectos de investigación
dc.subject.lembFísica de particulas
dc.titleExplaining pulsars high peculiar velocities - a viable particle physics solutionspa
dc.typeInforme de investigación
dc.type.coarhttp://purl.org/coar/resource_type/c_18ws
dc.type.contentText
dc.type.driverinfo:eu-repo/semantics/report
dc.type.redcolhttp://purl.org/redcol/resource_type/INF
dc.type.versioninfo:eu-repo/semantics/publishedVersion
dcterms.audienceEstudiantes, Profesores, Comunidad científica colombiana, etc.spa
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oaire.accessrightshttp://purl.org/coar/access_right/c_abf2
oaire.awardnumber22280509196
oaire.awardtitleExplaining pulsars high peculiar velocities - a viable particle physics solution
oaire.funderidentifier.colciencias222-96
oaire.fundernameDepartamento Administrativo de Ciencia, Tecnología e Innovación [CO] Colciencias
oaire.versionhttp://purl.org/coar/version/c_970fb48d4fbd8a85

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