J/A+A/604/A17ivo://CDS.VizieR/J/A+A/604/A17doi:10.26093/cds/vizier.36040017CDSMarques M.S.Zarka P.Echer E.Ryabov V.B.Alves M.V.Denis L.,Coffre A.2017-09-04T07:57:19Z2017-07-27T08:52:58ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frsolar-systemsolar-system-planetsradio-astronomyJupiter is a complex and at the same time very powerful radio source in the decameter wavelength range. The emission is anisotropic, intrinsically variable at millisecond to hour timescales, and also modulated by various external processes at much longer periods, ranging from ~10h to months or years (including Jovian day and year, solar activity and solar wind variations, and for ground-based observations, terrestrial day and year). As a consequence, long-term observations and their statistical study have proved to be necessary for disentangling and understanding the observed phenomena. We have built a database from the available 26yr of systematic, daily observations conducted at the Nancay Decameter Array and recorded in digital format. This database contains all observed Jovian decametric emissions, classified with respect to the time-frequency morphology, their dominant circular polarization, and maximum frequency. We present the results of the first statistical analysis of this database. We confirm the earlier classification of Jovian decameter emissions in Io-A, -A', -B, -C, -D and non-Io-A, -B, -C types, but we also introduce new emission types (Io-A'' and Io-B') and precise and characterize the non-Io-D type. We determine the contours of all emission types in the CML-{Phi}_Io_ plane (Central Meridian Longitude in Jupiter's System III coordinates versus Io Phase), provide representative examples of their typical time-frequency patterns, and the distribution of emission's maximum frequency as a function of {LAMBDA}_Io_ (Io's Longitude). Finally, we present a statistical analysis of the distributions of the occurrence rate, duration, intensity and polarization for each emission type. non-Io-DAM appears to be related to small-scale, possibly bursty auroral structures.2017A&A...604A..17Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/604/A17CatalogResearchIsServedByTAP VizieR generic servicerelated-tohttps://www.obs-nancay.fr : Nancay Obaervatory Home PAgehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/604/A17https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/604/A17http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/604/A17https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/604/A17https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/604/A17http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/604/A17GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapRadiodefaultJ/A+A/604/A17/obsLists of the parameters of observationrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRankObs[1/8163]meta.idintObs.dateObservation date (YYYY/MM/DD)time.epoch;obsnullableTimeTransJupiter's transit at Nancay meridiantime.epochnullableDEdegJupiter's declinationdegpos.eq.decHAsHour angle of start of observationminpos.eq.haintHAeHour angle of end of observationminpos.eq.haintFreqNDA optimisation frequencyMHzem.freqintFilt[1/4] Filter (1)meta.id;instr.filterintTimeTime of filter change 1->2 or 2->1time.epochnullableObs.timeSStart time of observationtime.epochnullableObs.timeEEnd time of observationtime.epochnullableFreqMinMinimum - maximum frequency of observationMHzem.freq;stat.min;stat.maxintFreqMaxMinimum - maximum frequency of observationMHzem.freq;stat.min;stat.maxintNem[0/17] Number of emissions catalogued for this observationmeta.id;instr.obstyintJ/A+A/604/A17/emLists of the numbers and parameters of emissionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRank[1/11463]meta.idintPol[0/1] Polarization (0=LH,1=RH)phys.polarizationintTimeSTime of emission starttime.epochnullableTimeETime of emission endtime.epochnullableFreqMinMinimum frequency of observationMHzem.freqfloatFreqMaxMaximum frequency of observationMHzem.freqfloatType[0/12] Source type (1)meta.code.classintAIPAverage intensity in emission polygon (units of 0.3125 dB)spect.line.intensityintAISAverage intensity in symmetrical emission polygon in opposite polarization (units of 0.3125 dB)spect.line.intensityintfracptFraction of points > background in dominant polarization%meta.numberintPolCCircular polarization ratio (LH>0, RH<0)%phys.polarization.circularintRankObs[4/8162] Rank of corresponding observationmeta.idintNptNumber of summits of emission polygonmeta.numberintFreq1Frequency value of emission polygon summits (x30./400+10 = MHz)em.freqintTime1Freq1 time value of emission polygon summits (2)time.epochintFreq2Frequency 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