----- Submission 1 (Fri May 13 08:13:24 GMT 2005) ----- Assigned ID: 161 ----- Submission 1 (Fri Jan 21 08:41:45 GMT 2005) ----- High resolution imaging of Jupiter's diffuse auroral emissions inside and outside the main oval during solar minimum. The analysis of HST-STIS FUV images has greatly and quickly advanced our knowledge of the magnetospheric mechanisms producing the auroral emissions on the giant planets. However, these studies were limited to the brightest emissions and very little has been said about the fainter emissions, mainly because of the lower S/N. We propose to image the faint auroral emissions on Jupiter which could not be observed with STIS. We will take full advantage of ACS/SBC's higher sensitivity to observe the diffuse auroral FUV emissions appearing poleward and directly equatorward of Jupiter's main auroral oval in the northern hemisphere. This proposal has the potential to reveal new magnetosphere-ionosphere coupling mechanisms especially those involving solar wind interactions with a giant planet.
We will take full advantage of ACS's higher sensitivity to observe the diffuse auroral FUV emissions appearing poleward and directly equatorward of Jupiter's main auroral oval in the northern hemisphere (Figure 3). Recent ACS/SBC imaging of Jupiter's aurora (GO-10140) demonstrates that the global count rate is well below the bright object limit. It also shows that sufficient S/N is reached with exposure times on the order of 100s. Past STIS observations demonstrate that the polar emissions (especially the diffuse swirl region) are best viewed when the central meridian longitude (CML) is close to 180? (S3). The present program consists of 4 independent HST orbits. They could be arranged in a way such that in each orbit, the auroral footprint of Io appears in a different sector, spanning approximately 45? of longitude. This footprint and its trailing tail may then be used as aids to map the equatorial boundary of the diffuse emission in different local time sectors. The 4 orbits should ideally be executed near Jupiter's opposition (6 May 2006), preferentially during the three-month period prior to opposition or during the second half of May, during which two-gyro observations are possible. Four targets were defined (one for each visit/orbit). They are all the same, the purpose of this redundancy is to ensure that the 4 orbits can be scheduled completely independently. The timing and geometric constraints may be adjusted in order to increase the schedulability. SOLAR SYSTEM 12 false 0.0 false false false false false SUPPORTED SOLAR SYSTEM Celestial North up (Jupiter North up) in ACS FOV. Final POS_ANGLE values may depend upon NOMINAL ORIENTATION PLANET Jupiter aurora ACS STD=JUPITER TYPE=POS_ANGLE,RAD=20.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 120.0 200.0 SOLAR SYSTEM Celestial North up (Jupiter North up) in ACS FOV PLANET Jupiter aurora ACS STD=JUPITER TYPE=POS_ANGLE,RAD=20.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 150.0 200.0, OLG OF IO BETWEEN 100.0 200.0 SOLAR SYSTEM Celestial North up (Jupiter North up) in ACS FOV PLANET Jupiter aurora ACS STD=JUPITER TYPE=POS_ANGLE,RAD=20.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 150.0 200.0, OLG OF IO BETWEEN 100.0 200.0 SOLAR SYSTEM Celestial North up (Jupiter North up) in ACS FOV PLANET Jupiter aurora ACS STD=JUPITER TYPE=POS_ANGLE,RAD=20.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 150.0 200.0, OLG OF IO BETWEEN 100.0 200.0 ACS/SBC Imaging No No F125LP The 4 orbits should ideally be executed near Jupiter?s opposition (6 May 2006), preferentially between 15 Feb 2006 and 31 May 2006, during which two-gyro observations are possible. (Tic-Visit :proposal-id 10507 :visit-id "01" :proposal-version -1 :trans-version "20050323" :date "13-May-2005 10:07:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 333248 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10507 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10507 :visit-id "01" :orbit-number 1 :pcs-time 367 :si-vis-utilization 2660 :al-overhead-at-end 0 :internal-dur-at-end 342 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) false 1 0 The 4 orbits should ideally be executed near Jupiter?s opposition (6 May 2006), preferentially during the three-month period prior to opposition or during the second half of May, during which two-gyro observations are possible. 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