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GCR flux 9-day variations with LISA Pathfinder

dc.contributor.authorBenella, S.
dc.contributor.authorFabi, M.
dc.contributor.authorFinetti, N.
dc.contributor.authorTelloni, D.
dc.contributor.authorArmano, M.
dc.contributor.authorAudley, H.
dc.contributor.authorAuger, G.
dc.contributor.authorBaird, J.
dc.contributor.authorBassan, M.
dc.contributor.authorBinetruy, P.
dc.contributor.authorBorn, M.
dc.contributor.authorBortoluzzi, D.
dc.contributor.authorBrandt, N.
dc.contributor.authorCaleno, M.
dc.contributor.authorCavalleri, A.
dc.contributor.authorCesarini, A.
dc.contributor.authorCruise, M.
dc.contributor.authorDanzmann, K.
dc.contributor.authorde Deus Silva, M.
dc.contributor.authorDe Rosa, R.
dc.contributor.authorDi Fiore, L.
dc.contributor.authorDiepholz, I.
dc.contributor.authorDolesi, R.
dc.contributor.authorDunbar, N.
dc.contributor.authorFerraioli, Luigi
dc.contributor.authorFerroni, V.
dc.contributor.authorFitzsimons, E. D.
dc.contributor.authorFlatscher, R.
dc.contributor.authorFreschi, M.
dc.contributor.authorGarcía Marirrodriga, C.
dc.contributor.authorGerndt, R.
dc.contributor.authorGesa, L.
dc.contributor.authorGibert, F.
dc.contributor.authorGiardini, D.
dc.contributor.authorGiusteri, R.
dc.contributor.authorGrado, A.
dc.contributor.authorGrimani, C.
dc.contributor.authorGrzymisch, J.
dc.contributor.authorHarrison, I.
dc.contributor.authorHeinzel, G.
dc.contributor.authorHewitson, M.
dc.contributor.authorHollington, D.
dc.contributor.authorHoyland, D.
dc.contributor.authorHueller, M.
dc.contributor.authorInchauspé, H.
dc.contributor.authorJennrich, O.
dc.contributor.authorJetzer, P.
dc.contributor.authorJohlander, B.
dc.contributor.authorKarnesis, N.
dc.contributor.authorKaune, B.
dc.contributor.authorKorsakova, N.
dc.contributor.authorKillow, C. J.
dc.contributor.authorLobo, A.
dc.contributor.authorLloro, I.
dc.contributor.authorLiu, L.
dc.contributor.authorLópez Zaragoza, J. P.
dc.contributor.authorMaarschalkerweerd, R.
dc.contributor.authorMance, D.
dc.contributor.authorMartín, V.
dc.contributor.authorMartín Polo, L.
dc.contributor.authorMartino, J.
dc.contributor.authorMartín Porqueras, F.
dc.contributor.authorMadden, S.
dc.contributor.authorMateos, I.
dc.contributor.authorMcNamara, P. W.
dc.contributor.authorMendes, J.
dc.contributor.authorMendes, L.
dc.contributor.authorNofrarias, M.
dc.contributor.authorPaczkowski, S.
dc.contributor.authorPerreur Lloyd, M.
dc.contributor.authorPetiteau, A.
dc.contributor.authorPivato, P.
dc.contributor.authorPlagnol, E.
dc.contributor.authorPrat, P.
dc.contributor.authorRagnit, U.
dc.contributor.authorRamos Castro, J.
dc.contributor.authorReiche, J.
dc.contributor.authorRobertson, D. I.
dc.contributor.authorRozemeijer, H.
dc.contributor.authorRivas García, Francisco
dc.contributor.authorRussano, G.
dc.contributor.authorSarra, P.
dc.contributor.authorSchleicher, A.
dc.contributor.authorShaul, D.
dc.contributor.authorSlutsky, J.
dc.contributor.authorSopuerta, C. F.
dc.contributor.authorStanga, R.
dc.contributor.authorSumner, T.
dc.contributor.authorTexier, D.
dc.contributor.authorThorpe, J. I.
dc.contributor.authorTrenkel, C.
dc.contributor.authorTroebs, M.
dc.contributor.authorVetrugno, D.
dc.contributor.authorVitale, S.
dc.contributor.authorWanner, G.
dc.contributor.authorWard, H.
dc.contributor.authorWass, P. J.
dc.contributor.authorWealthy, D.
dc.contributor.authorWeber, W. J.
dc.contributor.authorWissel, L.
dc.contributor.authorWittchen, A.
dc.contributor.authorZambotti, A.
dc.contributor.authorZanoni, C.
dc.contributor.authorZiegler, T.
dc.contributor.authorZweifel, P.
dc.contributor.authorLISA Pathfinder Collaboration
dc.date.accessioned2023-11-20T12:52:40Z
dc.date.available2023-11-20T12:52:40Z
dc.date.issued2017
dc.identifier.citationC Grimani et al 2017 J. Phys.: Conf. Ser. 840 012037es
dc.identifier.issn1742-6596
dc.identifier.issn1742-6588
dc.identifier.urihttps://hdl.handle.net/20.500.12412/4679
dc.description.abstractGalactic cosmic-ray (GCR) energy spectra in the heliosphere vary on the basis of the level of solar activity, the status of solar polarity and interplanetary transient magnetic structures of solar origin. A high counting rate particle detector (PD) aboard LISA Pathfinder (LPF) allows for the measurement of galactic cosmic-ray and solar energetic particle (SEP) integral fluxes at energies > 70 MeV n−1 up to 6500 counts s−1. Data are gathered with a sampling time of 15 s. A study of GCR flux depressions associated with the third harmonic of the Sun rotation period (∼ 9 days) is presented here.es
dc.language.isoenges
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internacional*
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/4.0/*
dc.titleGCR flux 9-day variations with LISA Pathfinderes
dc.typearticlees
dc.identifier.doi10.1088/1742-6596/840/1/012037
dc.issue.number012037es
dc.journal.titleJournal of Physics: Conference Serieses
dc.rights.accessRightsopenAccesses
dc.volume.number840es


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Attribution-NonCommercial-NoDerivatives 4.0 Internacional
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