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JUPITER_NULLIn situ Jupiter magnetic null searchWorking Group 3
JUPITER_GMIn situ mapping of global configuration and monitoring dynamics of the Jovian magnetospheric environment. corotation should be in the FoV of PEP/JDC or PEP/JEI. Conditions for coverage: ◦ Minimum angle less than about 11.25 deg (half-azimuthal sector size) of a JEI or JDC pixel from corotation ◦ Boresight angle of JDC or JEI less than ˜90 deg Conditions for ideal coverage: ◦ Minimum angle less than about 11.25 deg (half-azimuthal sector size) of a JEI or JDC pixel from corotation ◦ Boresight angle less than ˜75 deg (JEI) or 70 deg (JDC): corotation away from the FoV edge JDC is preferred for monitoring corotation, over JEI, when possible.Working Group 3
JUPITER_ENAImaging of Jupiter's magnetosphere in energetic neutral atoms (ENAs).Maximize pitch angle coverage with PEP JEI,JDC,JoEE, JENI (ion mode) a) JENI has a broad FoV and captures Jupiter and the Io/Europa torus and magnetosphere at most times. No special pointing design required for JENI besides requiring an approximate nadir pointing (considerable offsets can still be acceptable) b) JNA disk-shaped/slit FoV has a slight offset from the XZ spacecraft plane, meaning that during nadir pointing, it images preferentially the northern or southern extension of the Europa/Io torus, whereas Jupiter may be in the edge or outside of the FoV, especially at large distances. Scans (small rotations around Sc-X) or periods with stable, small offset of the SC-xz plane from Nadir can help to better image stronger emissions from the equatorial torusWorking Group 3
JUPITER_CPSIn situ Jupiter current/plasma sheet observationWorking Group 3
JUPITER_CPIn situ Jupiter corotation breakdown region and plasma transport observation. Maximize the intervals for which co-rotation is measured to build spatial and temporal coverage of corotation profiles across the magnetosphere and also in the local moon environments. CP stands for corotation profileWorking Group 3
JUPITER_CBIn situ Jupiter corotation breakdown region and plasma transport observation. Maximize the intervals for which co-rotation is measured to build spatial and temporal coverage of corotation profiles across the magnetosphere and also in the local moon environments.Working Group 3
JM_PE35 Working Group 3
JM_PE33share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE31share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE29share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE27share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE25share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE23share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE21share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE19share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE17share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE15share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE13share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE_P4_noDL Working Group 3
JM_PE_P4Perijoves with WG3 prime (--> 20/09/18: modified (discussion with OW). assuming ~2 times what is produced in G4-G5 scenario (~6.5-7 Gb). Corresponds roughly to 19kbps, copied from JA_INCL) RS rate assumes no D/L suspension (case 2)Working Group 3
JM_PE_OBSJupiter Magnetosphere perijove segments containing link to observations databaseWorking Group 3
JM_PEassuming: JMAG: 2.31 kbps RPWI: 1.7*2.167 kbps PEP: 2 kpbs (ball park number; discussion with Gabriella at WG3 F2F meeting in Sept 2018)Working Group 3
JM_INCL Working Group 3
JM_GM Working Group 3
JM_ENA Working Group 3
JM_CB Working Group 3
GANYMEDE_WAKEIn situ Ganymede wake observationWorking Group 3
GANYMEDE_IONOGANYMEDE_IONO In situ Ganymede ionosphere observationWorking Group 3
GANYMEDE_GMIn situ mapping of global configuration and monitoring dynamics of Ganymede's magnetospheric environmentWorking Group 3
GANYMEDE_FLYBY_RPWI_IONO_AJS Working Group 3
GANYMEDE_ENAFar approach energetic neutral atom imaging of GanymedeWorking Group 3
G_IS_OBSG_IS_OBSWorking Group 3
G_IS_4G4 Working Group 3
G_IS_3G3Ganymede in-situ observations around closest approachWorking Group 3
G_IS Working Group 3
EUROPA_WAKEIn situ Europa wake observationWorking Group 3
EUROPA_TOR_ISIn situ Europa torus observationWorking Group 3
EUROPA_IONO_ISEUROPA_IONO_IS In situ Europa ionosphere observationWorking Group 3
EUROPA_FLYBY_RPWI_IONO_AJS Working Group 3
EUROPA_ENAFar approach energetic neutral atom imaging of EuropaWorking Group 3
E_IS_OBSE_IS_OBSWorking Group 3
E_IS Working Group 3
CALLISTO_WAKEIn situ Callisto wake observationWorking Group 3
CALLISTO_IONOCALLISTO_IONO In situ Callisto ionosphere observationWorking Group 3
CALLISTO_FLYBY_RPWI_IONO_AJS Working Group 3
CALLISTO_ENAFar approach energetic neutral atom imaging of CallistoWorking Group 3
C_IS_OBSC_IS_OBSWorking Group 3
C_IS Working Group 3
SHADOWEDGErings SHADOWEDGE. Imaging of the ring region intersected by the planetary shadow at moderate elevation and very high phase. Especially for the very faint gossamer rings and the Thebe extensionWorking Group 2
ROI_INTERSECTIONROI_INTERSECTIONWorking Group 2
RINGSPIRAL_MPRINGSPIRAL_MP (medium phase: JANUS Def)Working Group 2
RINGSPIRAL_HPRINGSPIRAL_HP (high phase, Janus def)Working Group 2
RINGPHASE Working Group 2
RINGMOSAICRINGMOSAIC (Janus definition). impression of the extent of the whole ring systemWorking Group 2
RINGMATTERRINGMATTER. Observations of the main rings and the gossamer rings, imaging the ring ansae from moderately large elevation. The moderatly large elevation will reveal azimuthal structure in the rings and the presence of clumps at the resolution limit of the imaging.Working Group 2
RING_PHASECURV_90 Working Group 2
RING_PHASECURV_80 Working Group 2
RING_PHASECURV_70 Working Group 2
RING_PHASECURV_60 Working Group 2
RING_PHASECURV_50 Working Group 2
RING_PHASECURV_5Opportunity implementation in geopipeline SC distance to Jupiter larger than 8e5 km SC elevation above the rings lower than 0.5 deg Only one Ansae tested for phase conditions - value must be between 5 deg and 10 degWorking Group 2
RING_PHASECURV_40 Working Group 2
RING_PHASECURV_30 Working Group 2
RING_PHASECURV_20 Working Group 2
RING_PHASECURV_170 Working Group 2
RING_PHASECURV_160 Working Group 2
RING_PHASECURV_150 Working Group 2
RING_PHASECURV_140 Working Group 2
RING_PHASECURV_130 Working Group 2
RING_PHASECURV_120 Working Group 2
RING_PHASECURV_110 Working Group 2
RING_PHASECURV_100 Working Group 2
RING_PHASECURV_10Opportunity implementation in geopipeline SC distance to Jupiter larger than 8e5 km SC elevation above the rings lower than 0.5 deg Only one Ansae tested for phase conditions - value must be between 10 deg and 20 degWorking Group 2
RING_LPRing low phaseWorking Group 2
RING_HPRing high phaseWorking Group 2
J_SAT_VALETUDO Working Group 2
J_SAT_THYONE Working Group 2
J_SAT_THEMISTO Working Group 2
J_SAT_TAYGETE Working Group 2
J_SAT_SINOPE Working Group 2
J_SAT_S2017_J9 Working Group 2
J_SAT_S2017_J7 Working Group 2
J_SAT_S2017_J6 Working Group 2
J_SAT_S2017_J5 Working Group 2
J_SAT_S2017_J3 Working Group 2
J_SAT_S2017_J2 Working Group 2
J_SAT_S2016_J1 Working Group 2
J_SAT_S2011_J2 Working Group 2
J_SAT_S2010_J2 Working Group 2
J_SAT_S2010_J1 Working Group 2
J_SAT_S2003_J9 Working Group 2
J_SAT_S2003_J4 Working Group 2
J_SAT_S2003_J19 Working Group 2
J_SAT_S2003_J16 Working Group 2
J_SAT_S2003_J12 Working Group 2
J_SAT_S2003_J10 Working Group 2
J_SAT_PRAXIDIKE Working Group 2
J_SAT_PHILOPHROSYNE Working Group 2
J_SAT_PASITHEE Working Group 2
J_SAT_PASIPHAE Working Group 2

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