000890234 001__ 890234
000890234 005__ 20250512115731.0
000890234 0247_ $$2doi$$a10.1088/1742-6596/1342/1/012033
000890234 0247_ $$2ISSN$$a1742-6588
000890234 0247_ $$2ISSN$$a1742-6596
000890234 0247_ $$2Handle$$a2128/27068
000890234 0247_ $$2WOS$$aWOS:001432953400033
000890234 037__ $$aFZJ-2021-00821
000890234 082__ $$a530
000890234 1001_ $$0P:(DE-Juel1)168122$$aLudhova, Livia$$b0$$eCorresponding author$$ufzj
000890234 1112_ $$aTAUP 2017$$cSudbury$$d2017-07-24 - 2017-07-28$$wCanada
000890234 245__ $$aLimiting the effective magnetic moment of solar neutrinos with the Borexino detector
000890234 260__ $$aBristol$$bIOP Publ.87703$$c2020
000890234 264_1 $$2Crossref$$3print$$bIOP Publishing$$c2020-01-01
000890234 264_1 $$2Crossref$$3print$$bIOP Publishing$$c2020-01-01
000890234 300__ $$a5
000890234 3367_ $$2ORCID$$aCONFERENCE_PAPER
000890234 3367_ $$033$$2EndNote$$aConference Paper
000890234 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$mjournal
000890234 3367_ $$2BibTeX$$aINPROCEEDINGS
000890234 3367_ $$2DRIVER$$aconferenceObject
000890234 3367_ $$2DataCite$$aOutput Types/Conference Paper
000890234 3367_ $$0PUB:(DE-HGF)8$$2PUB:(DE-HGF)$$aContribution to a conference proceedings$$bcontrib$$mcontrib$$s1611672525_2352
000890234 520__ $$aBorexino has provided an updated upper limit on the effective neutrino magnetic moment of solar neutrinos μβα < 2.8 x 10−11 μऔ at 90% C.L. This result represents nearly a factor of two improvement with respect to the previous result based on 192 days of the Phase-I data. The current analysis has been performed using 1291.5 days exposure of the Phase-II data, characterized by a further improved level of radio-purity of liquid scintillator. Another key ingredient of the new analysis, lowering the threshold from 260 to 186 keV, was possible thanks to a better understanding of the detector-response function at low energies. The global spectral fit was preformed up to 2970 keV energy, using constraints on the sum of the solar neutrino fluxes implied by the radiochemical gallium experiments. From the limit for the effective neutrino magnetic moment, new limits for the magnetic moments of the neutrino flavour states were derived.
000890234 536__ $$0G:(DE-HGF)POF3-612$$a612 - Cosmic Matter in the Laboratory (POF3-612)$$cPOF3-612$$fPOF III$$x0
000890234 542__ $$2Crossref$$i2020-01-01$$uhttp://creativecommons.org/licenses/by/3.0/
000890234 542__ $$2Crossref$$i2020-01-01$$uhttps://iopscience.iop.org/info/page/text-and-data-mining
000890234 588__ $$aDataset connected to CrossRef
000890234 7001_ $$0P:(DE-HGF)0$$aBorexino collaboration$$b1
000890234 77318 $$2Crossref$$3journal-article$$a10.1088/1742-6596/1342/1/012033$$bIOP Publishing$$d2020-01-01$$n1$$p012033$$tJournal of Physics: Conference Series$$v1342$$x1742-6588$$y2020
000890234 773__ $$0PERI:(DE-600)2166409-2$$a10.1088/1742-6596/1342/1/012033$$gVol. 1342, p. 012033 -$$n1$$p012033$$tJournal of physics / Conference Series$$v1342$$x1742-6588$$y2020
000890234 8564_ $$uhttps://juser.fz-juelich.de/record/890234/files/Ludhova_2020_J._Phys.%20_Conf._Ser._1342_012033.pdf$$yOpenAccess
000890234 909CO $$ooai:juser.fz-juelich.de:890234$$pdnbdelivery$$pdriver$$pVDB$$popen_access$$popenaire
000890234 9101_ $$0I:(DE-588b)5008462-8$$6P:(DE-Juel1)168122$$aForschungszentrum Jülich$$b0$$kFZJ
000890234 9131_ $$0G:(DE-HGF)POF3-612$$1G:(DE-HGF)POF3-610$$2G:(DE-HGF)POF3-600$$3G:(DE-HGF)POF3$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMaterie und Universum$$vCosmic Matter in the Laboratory$$x0
000890234 9141_ $$y2020
000890234 915__ $$0LIC:(DE-HGF)CCBY3$$2HGFVOC$$aCreative Commons Attribution CC BY 3.0
000890234 915__ $$0StatID:(DE-HGF)0200$$2StatID$$aDBCoverage$$bSCOPUS
000890234 915__ $$0StatID:(DE-HGF)0300$$2StatID$$aDBCoverage$$bMedline
000890234 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000890234 9201_ $$0I:(DE-Juel1)IKP-2-20111104$$kIKP-2$$lExperimentelle Hadrondynamik$$x0
000890234 980__ $$acontrib
000890234 980__ $$aVDB
000890234 980__ $$aUNRESTRICTED
000890234 980__ $$ajournal
000890234 980__ $$aI:(DE-Juel1)IKP-2-20111104
000890234 9801_ $$aFullTexts
000890234 999C5 $$1Bellini$$2Crossref$$oBellini 2011$$y2011
000890234 999C5 $$1Bellini$$2Crossref$$9-- missing cx lookup --$$a10.1103/PhysRevLett.108.051302$$tPhys. Rev. Lett.$$v108$$y2012
000890234 999C5 $$1Bellini$$2Crossref$$9-- missing cx lookup --$$a10.1038/nature13702$$p383 -$$tNature$$v512$$y2014
000890234 999C5 $$1Bellini$$2Crossref$$9-- missing cx lookup --$$a10.1103/PhysRevD.82.033006$$tPhys. Rev. D$$v82$$y2010
000890234 999C5 $$1Agostini$$2Crossref$$oAgostini 2017$$y2017
000890234 999C5 $$1Bellini$$2Crossref$$9-- missing cx lookup --$$a10.1007/JHEP08(2013)038$$p038 -$$tJHEP$$v1308$$y2013
000890234 999C5 $$1Beda$$2Crossref$$9-- missing cx lookup --$$a10.1134/S1547477113020027$$p139 -$$tPhys.Part. and Nucl.Lett.$$v10$$y2013
000890234 999C5 $$1Wong$$2Crossref$$oWong 2007$$y2007
000890234 999C5 $$1Liu$$2Crossref$$oLiu 2004$$y2004
000890234 999C5 $$1Bellini$$2Crossref$$oBellini 2008$$y2008
000890234 999C5 $$1Agostini$$2Crossref$$oAgostini 2017$$y2017
000890234 999C5 $$1Raffelt$$2Crossref$$oRaffelt 1988$$y1988
000890234 999C5 $$1Arceo-Díaz$$2Crossref$$9-- missing cx lookup --$$a10.1016/j.astropartphys.2015.03.006$$p1 -$$tAstropart. Phys.$$v70$$y2015
000890234 999C5 $$1Bellini$$2Crossref$$9-- missing cx lookup --$$a10.1103/PhysRevD.89.112007$$tPhys. Rev. D$$v89$$y2014
000890234 999C5 $$1Abdurashitov$$2Crossref$$9-- missing cx lookup --$$a10.1103/PhysRevC.80.015807$$p1 -$$tPhys. Rev. C$$v80$$y2009
000890234 999C5 $$1Patrignani$$2Crossref$$oPatrignani 2016$$y2016