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UVS_JUP_AP_AIRGLOW_STAREMonitoring auroral and airglow emissions in stare mode using the Airglow Port (AP). Slit held along Jupiter’s North/South and on the central meridian, while Jupiter rotates below S/C creating a map. Histogram mode.UVS
UVS_GCO_HPN/AUVS
UVS_GCO_HISTOGRAM_002N/AUVS
UVS_GCO_HISTOGRAM_001N/AUVS
OBSOLETE_RPWI_MAGN_In-situ_BurstN/ARPWI
OBSOLETE_RPWI_MAGN_In-situ_NormalN/ARPWI
OBSOLETE_RPWI_GAN_Radio_BurstUsed for radio occultation of Jovian radio emissions to infer the ionospheric spatial structure. RPWI
OBSOLETE_RPWI_GAN_In-situ_LowTMN/ARPWI
OBSOLETE_RPWI_GAN_In-situ_NormalMakes continuous detailed RPWI observations that satisfy most SciRD requirements below 1.6 MHz. Main science targets here are the ionospheric/magnetospheric electric currents and electrodynamics, including sub-surface ocean characteristics. RPWI
OBSOLETE_RPWI_GAN_Radio_PassiveRadarThere are several ways of doing passive radar under investigation. We have chosen the most resource hungry mode for this table. One of the RWI antenna nulls (X, Y or Z) should point towards Jupiter with +/-1 deg accuracy. Monitoring HOM and DAM Jupiter radiation with reflections from ionosphere, surface and sub-surface layers (ocean/bedrock) to determine ionosphere and ice sheet thickness. Due to lower frequency (below 3 MHz), RPWI will reach deeper than RIME.RPWI
OBSOLETE_RPWI_GAN_Radio_FullMake more detailed radio emissions from Jupiter as well as Ganymede. Will also support RIME measurements, giving the background natural radio emissions. Monitor the radio emission spectrum as well as polarization.RPWI
OBSOLETE_RPWI_GAN_Radio_SlowMake survey of radio emissions from Jupiter as well as Ganymede. Will also support RIME observations, giving the background natural radio emissions. Monitor the radio emission spectrum.RPWI
OBSOLETE_RPWI_GAN_In-situ_BurstMakes full plasma wave measurements and high-time resolution monitoring up to 1.6MHz as well as cover the low frequency and DC electric field and density measurements.RPWI

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