WHAT'S NEW WITH G2?

Additions made 9 March 1995

• Noted anticipated reductions due to decreased downlink capability

Additions made 30 January 1995

• Replaced sequence timeline graphics with new versions from the G02AHA SEF

Additions made 20 January 1995

• Updated MPP record times currently being planned for the Perijove and Plasma Sheet observations.

Additions made 17 January 1995

• Linked gifs for all of the MWG recorded observations except for the plasma sheet crossing using G02ADA.SEF which is the first official SEF for this orbit. It does not extend long enough in time to reach our plasma sheet crossing. Also note that many of the recent detailed changes in the PWS observations as described in this page HAVE NOT yet been implemented, hence, the observations in the gifs do not correspond to those currently planned. The next version of the SEF should fix this.

Additions/changes made 12 January 1995

• 1. Added gif for Ganymede Closest Approach observation to highlight region where UVS quiet is expected. No MWG commands are in this version of the G2 RSSG SEF.
• 2. Shortened the duration of the Plasma Sheet Crossing observation by 7.5 minutes on each end as a result of the resource trade with the AWG. This observation is now about 60 minutes long.

Changes made 11 January 1995

• 1. Updated the MPP recording time for the perijove crossing to be centered on the magnetic equator crossing
• 2. Updated the MPP recording time for the plasma sheet crossing to reflect a shorter, but more realistic duration based on known tape availability/allocation.

Changes requested 10 January 1995

• 1. Moved MPP recording period out of Ganymede closest approach observation and into Perijove observation. This was done because a following buffer-dump-to-tape would preclude us from reviewing the RTS in time to select any MPP data for playback.
• 2. Added MPP recording to the center of the Perijove observation from the tape saved in #1 above.
• 3. Changed wideband mode in the Perijove observation from 2 (80 kHz) to 3 (1 kHz) to take advantage of the continuous waveform samples afforded by MPP in the 1-kHz mode. This observation requires additional tape for the higher record rate of MPP, hence, it is a good observation for a tape-rich orbit of which G2 is a good example. We will do the 80-kHz observation again in a later orbit when we can only afford the LPW record rate.