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Solar neutrinos before and after KamLAND

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Solar neutrinos before and after KamLAND

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dc.contributor.author Bahcall, John N.
dc.contributor.author González García, Mª Concepción
dc.contributor.author Peña Garay, Carlos
dc.date.accessioned 2014-11-03T12:31:13Z
dc.date.available 2014-11-03T12:31:13Z
dc.date.issued 2003
dc.identifier.citation Bahcall, John N. González García, Mª Concepción Peña Garay, Carlos 2003 Solar neutrinos before and after KamLAND Journal of High Energy Physics 03 2 009
dc.identifier.uri http://hdl.handle.net/10550/39540
dc.description.abstract We use the recently reported KamLAND measurements on oscillations of reactor anti-neutrinos, together with the data of previously reported solar neutrino experiments, to show that: (1) the total B-8 neutrino flux emitted by the Sun is 1.00 (1 +/- 0.06) (1sigma) of the standard solar model (BP00) predicted flux, (2) the KamLAND measurements reduce the area of the globally allowed oscillation regions that must be explored in model fitting by six orders of magnitude in the Deltam(2-)tan(2) theta plane, (3) LMA is now the unique oscillation solution to a CL of 4.7sigma, (4) maximal mixing is disfavored at 3.1sigma, (5) active-sterile admixtures are constrained to sin(2) eta less than or equal to 0.13 at 1sigma, (6) the observed B-8 flux that is in the form of sterile neutrinos is 0.00(-0.00)(+0.09) (1sigma), of the standard solar model (BP00) predicted flux, and (7) non-standard solar models that were invented to avoid completely solar neutrino oscillations are excluded by KamLAND plus solar data at 7.9sigma. We also refine quantitative predictions for future Be-7 and p - p solar neutrino experiments.
dc.language.iso eng
dc.relation.ispartof Journal of High Energy Physics, 2003, vol. 03, num. 2, p. 009
dc.subject Astronomia
dc.title Solar neutrinos before and after KamLAND
dc.type journal article es_ES
dc.date.updated 2014-11-03T12:31:13Z
dc.identifier.doi 10.1088/1126-6708/2003/02/009
dc.identifier.idgrec 097452
dc.rights.accessRights open access es_ES

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