Home › Core › Segment definitions

Select segment definition to view

Mnemonic
1
Description
2
Group
G_IS_4G4 Working Group 3
JM_PE35 Working Group 3
TOR_RS Working Group 3
JM_INCL Working Group 3
JM_PE_P4_noDL Working Group 3
JM_CB Working Group 3
JM_ENA Working Group 3
JM_GM Working Group 3
G_IS Working Group 3
E_IS Working Group 3
C_IS Working Group 3
CALLISTO_FLYBY_RPWI_IONO_AJS Working Group 3
EUROPA_FLYBY_RPWI_IONO_AJS Working Group 3
GANYMEDE_FLYBY_RPWI_IONO_AJS Working 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
C_IS_OBSC_IS_OBSWorking Group 3
CALLISTO_IONOCALLISTO_IONO In situ Callisto ionosphere observationWorking Group 3
E_IS_OBSE_IS_OBSWorking Group 3
EUROPA_IONO_ISEUROPA_IONO_IS In situ Europa ionosphere observationWorking Group 3
CALLISTO_ENAFar approach energetic neutral atom imaging of CallistoWorking Group 3
EUROPA_ENAFar approach energetic neutral atom imaging of EuropaWorking Group 3
GANYMEDE_ENAFar approach energetic neutral atom imaging of GanymedeWorking Group 3
G_IS_OBSG_IS_OBSWorking Group 3
G_IS_3G3Ganymede in-situ observations around closest approachWorking Group 3
GANYMEDE_IONOGANYMEDE_IONO In situ Ganymede ionosphere observationWorking 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
CALLISTO_WAKEIn situ Callisto wake observationWorking Group 3
EUROPA_TOR_ISIn situ Europa torus observationWorking Group 3
EUROPA_WAKEIn situ Europa wake observationWorking Group 3
GANYMEDE_WAKEIn situ Ganymede wake 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
JUPITER_CPSIn situ Jupiter current/plasma sheet observationWorking Group 3
JUPITER_NULLIn situ Jupiter magnetic null searchWorking Group 3
JUPITER_PDTIn situ Jupiter particle distribution transition region observation. Maximize pitch angle coverage for PEP/JEI, JDC,JoEE, JENI (ion mode)Working Group 3
GANYMEDE_GMIn situ mapping of global configuration and monitoring dynamics of Ganymede's magnetospheric environmentWorking 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_TAILIn situ search for signatures of local magnetic reconnection in the Jovian magnetotailWorking Group 3
JM_PE_OBSJupiter Magnetosphere perijove segments containing link to observations databaseWorking 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_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

51 segment definitions