! $Id: 5414,v 10.1 1994/09/13 19:10:46 pepsa Exp $ coverpage: title_1: DAYGLOW EMISSION LINE PROFILES FROM THE OUTER PLANETS title_2: CYCLE4-MED sci_cat: SOLAR SYSTEM sci_subcat: GIANT PLANETS proposal_for: GO pi_fname: JOHN pi_mi: T. pi_lname: CLARKE pi_inst: UNIVERSITY OF MICHIGAN pi_country: USA pi_phone: 313-747-3540 hours_pri: 7.70 num_pri: 6 hrs: Y realtime: Y time_crit: Y off_fname: NEIL off_lname: GERL off_title: PROJECT REP., DRDA off_inst: 2660 off_addr_1: 475 E. JEFFERSON off_city: ANN ARBOR off_state: MI off_zip: 48109 off_country: USA off_phone: 313-763-6438 ! end of coverpage abstract: line_1: Recent IUE observations of the H Ly alpha emission line profile line_2: from Jupiter's dayglow and aurora reveal a substantial line broadening, line_3: implying that the observed high brightness is due to resonant line_4: scattering of solar emission with a broad line rather than charged line_5: particle excitation. This may reflect highly energetic processes line_6: producing a 5-10 km/sec suprathermal population of H atoms in Jupiter's line_7: upper atmosphere, which in turn may be related to the unresolved question line_8: of the high exospheric temperatures of 400-1200 K detected on all 4 giant line_9: planets during the Voyager encounters. It is clear that if the bright H line_10: Ly alpha emissions from the outer planets are due mainly to resonant line_11: scattering of solar and interplanetary emissions, as observed line_12: on Jupiter and Saturn from long term correlations with the solar line_13: Ly alpha flux, then the lines from all 4 planets must be broad to line_14: explain the observed high albedos. The H Ly alpha lineshapes provide line_15: a discriminant between the processes of resonant scattering and line_16: charged particle excitation. We propose to obtain high signal to noise line_17: H Ly alpha line profile measurements from Saturn, Uranus, and Neptune line_18: to resolve the questions about the excitation processes for the bright line_19: airglow emissions. line_20: ALL SATURN OBSERVATIONS HAVE BEEN MOVED TO A NEW PROPOSAL. ! ! end of abstract general_form_proposers: lname: CLARKE fname: JOHN mi: T. inst: 2660 country: USA ! lname: BEN JAFFEL fname: LOTFI inst: 5436 country: FRANCE esa: Y ! lname: GLADSTONE fname: RANDALL inst: 3440 country: USA ! lname: PRANGE fname: RENEE inst: 5448 country: FRANCE esa: Y ! lname: VIDAL-MADJAR fname: ALFRED inst: 5436 country: FRANCE esa: Y ! lname: WAITE fname: HUNTER inst: 3440 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We request 6 dark orbit spectra, with two spectra each for Saturn and line_2: Uranus and one for Neptune. The Saturn observations will consist of center line_3: to limb scans with the GHRS LSA (echelle A at 1215.7 A), with scans E/W and line_4: N/S from the planet center to the limb. The scan across the north pole will line_5: be important to reveal any line broadening associated with the polar aurora, line_6: as has been observed on Jupiter, and the E/W scan will show the changing line line_7: shape with the increased slant column near the limb. The 2 arc sec LSA is line_8: somewhat smaller than Uranus (3.8 arc sec diameter) and Neptune (2.4 line_9: arc sec diameter), although it is filled by both planets, and planet- line_10: center spectra will be taken of each. In addition, one spectrum will be line_11: obtained near the limb of Uranus where the magnetic pole is presently line_12: rotating in and out of the field of view from the Earth. Since the line_13: rotational ephemeris for Uranus is insufficiently accurate to determine line_14: the longitude system today, we will have to take our chances on the line_15: location of any auroral emission near the pole. Since the emissions from line_16: Neptune are closer to the background brightness, planet and sky background line_17: spectra will be taken. Saturn can be acquired by blind offset from guide line_18: stars, and GHRS autonomous acquisitions of satellites will be used for line_19: offsets to Uranus and Neptune. ! question: 4 section: 1 line_1: As described above, we are also pursuing this program with IUE observa- line_2: tions of Jupiter, Saturn, and Uranus: Neptune is too faint for IUE at high line_3: resolution. The observations are limited by much lower sensitivity, and line_4: roughly a factor of two lower spectral resolution, of IUE compared with the line_5: GHRS echelle A and LSA. The existing IUE data with the SWP camera and small line_6: aperture at high dispersion are shown by Clarke et al. (1991). Longer line_7: exposures are possible with IUE, but Jupiter's rotation of 36 degrees/hour line_8: limits observations of specific longitude regions to 2-3 hours. The GHRS line_9: spectral capabilities will allow us to obtain high quality H Ly alpha line_10: line profiles of regions on Saturn, and determine the full line shapes line_11: (including the important wings). With the 2 arc sec GHRS LSA we will also line_12: obtain sub-solar + auroral latitude spectra of Uranus with good sensitivity line_13: in the wings, and we expect to get a basic line width measurement of the line_14: fainter emission from Neptune. From our experience with IUE spectra at low line_15: signal to noise, we have determined that the H Ly alpha profile of Jupiter line_16: is very broad, and the high Ly alpha albedos of Saturn and Uranus require line_17: similarly broad lines if the dominant emission process is RS of solar and line_18: IPM Ly alpha. Neptune is the one case where the emission is sufficiently line_19: faint that the line may be narrow, and we wish to make this observation for line_20: comparison with the other 3 planets. ! question: 5 section: 1 line_1: We need to minimize the sky background subtraction, which involves line_2: minimizing the geocoronal background Ly alpha emission by observing line_3: near opposition. We also need some minimum Doppler shift between line_4: the planetary and geocoronal emissions from observing near roughly line_5: 30-60 degrees from the anti-solar point, so that the combined Earth and HST line_6: orbital motions of 38 km/sec have large components along the line of sight line_7: during the dark portion of the HST orbit when the background is minimal. line_8: This will allow us to separate spectrally the geoc. and planetary emissions. line_9: PLEASE NOTE: several parameters in the exposure list will need to be line_10: adjusted depending on the dates of observations, for Saturn and Uranus. line_11: PLEASE CONTACT THE PI WHEN THE WEEK OF OBSERVING IS SET to check this. line_12: The observation requires that the grating tilt should be kept same line_13: for the WAVE calibration as one of the scientific exposures in each group, line_14: for the targets, Saturn, Uranus, and Neptune. This means NO SPYBAL line_15: OPERATIONS SHOULD TAKE PLACE IN BETWEEN THE SCIENTIFIC EXPOSURES AND THE line_16: WAVE CALIBRATION. ! question: 6 section: 1 line_1: None. ! ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: There are a total of 21 programs in cycles 1-3, resulting in line_2: (to date) nine publications. Several more publications are in line_3: the process of being submitted and/or reviewed. ! question: 10 section: 1 line_1: Complete computing facilities are in place and available within the Space line_2: Physics Research Laboratory at the University of Michigan for use on this line_3: project. Two VAX 750's and a VAX 8600 are accessible via a local area line_4: network, in addition to the Michigan network MERIT, SPAN, and Internet. line_5: Three Sun Sparcstations with IDL are presently being used for IUE and line_6: HST data reductions. All Co-Investigators also have complete computer line_7: facilities available at their institutions for use on this project, and line_8: graduate students are available at all institutions for assistance with line_9: this project. ! !end of general form text general_form_address: lname: Clarke fname: John mi: T. category: PI inst: 2660 addr_1: AOSS Department addr_2: 2455 Hayward city: Ann Arbor state: MI zip: 481092143 country: USA phone: 313-747-3540 ! ! end of general_form_address records ! No fixed target records found solar_system_targets: ! targnum: 3 name_1: TITANIA-ACQ descr_1: SATELLITE TITANIA lev1_1: STD = URANUS, ACQ = 0.25 lev2_1: STD = TITANIA wind_1: OLG OF URANUS BETWEEN 300 330, wind_2: SEP OF OBERON TITANIA FROM EARTH wind_3: GT 10", SEP OF UMBRIEL TITANIA FROM wind_4: EARTH GT 10", SEP OF ARIEL TITANIA wind_5: FROM EARTH GT 10" comment_1: ON-BOARD ACQUISITION OF TITANIA comment_2: FOR OFFSET TO URANUS. fluxnum_1: 1 fluxval_1: V = 13.7 ! targnum: 4 name_1: URANUS-CENTER descr_1: PLANET URANUS lev1_1: STD = URANUS, ACQ = 0.25 wind_1: OLG OF URANUS BETWEEN 300 330 comment_1: OBSERVE URANUS AT PLANET CENTER. comment_2: GHRS ECH-A SPECTRUM OF H LY ALPHA comment_3: LINE WHEN URANUS OLG = 300-330 comment_4: DEGREES. fluxnum_1: 1 fluxval_1: SURF(V) = 8.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1216) = 3. +/- 1. E-12 fluxnum_3: 3 fluxval_3: W-LINE(1216) = 0.2 +/- 0.15 ! targnum: 5 name_1: URANUS-AUR descr_1: OFFSET URANUS lev1_1: STD = URANUS, ACQ = 0.25 lev2_1: TYPE=POS_ANGLE, REF=NORTH, lev2_2: ANG = 275., RAD=1.4 wind_1: OLG OF URANUS BETWEEN 300 330 comment_1: OBSERVE URANUS NEAR LIMB WHERE comment_2: AURORAL EMISSION IS EXPECTED. comment_3: GHRS ECH-A SPECTRUM OF H LY ALPHA comment_4: LINE WHEN URANUS OLG = 300-330 comment_5: DEGREES. NOTE: RAD DEPENDS ON comment_6: DAY OF OBSERVATION. fluxnum_1: 1 fluxval_1: SURF(V) = 8.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1216) = 3. +/- 1. E-12 fluxnum_3: 3 fluxval_3: W-LINE(1216) = 0.2 +/- 0.15 ! targnum: 6 name_1: TRITON-ACQ descr_1: SATELLITE TRITON lev1_1: STD = NEPTUNE, ACQ = 0.25 lev2_1: STD = TRITON wind_1: OLG OF NEPTUNE BETWEEN 300 330 wind_2: OLG OF NEPTUNE BETWEEN 30 60 comment_1: ON-BOARD ACQUISITION OF TRITON comment_2: FOR OFFSET TO NEPTUNE. fluxnum_1: 1 fluxval_1: V = 13.5 ! targnum: 7 name_1: NEPTUNE descr_1: PLANET NEPTUNE lev1_1: STD = NEPTUNE, ACQ = 0.25 wind_1: OLG OF NEPTUNE BETWEEN 300 330 wind_2: OLG OF NEPTUNE BETWEEN 30 60 comment_1: OBSERVE NEPTUNE AT PLANET CENTER. comment_2: GHRS ECH-A SPECTRUM OF H LY ALPHA comment_3: LINE. NEPTUNE OLG = 300-330 OR 30- comment_4: 60 DEGREES. fluxnum_1: 1 fluxval_1: SURF(V) = 9.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1216) = 0.6 +/- 0.6 E-12 fluxnum_3: 3 fluxval_3: W-LINE(1216) = 0.1 +/- 0.05 ! targnum: 8 name_1: NEPTUNE-OFFSET-SKY descr_1: OFFSET NEPTUNE lev1_1: STD = NEPTUNE lev2_1: TYPE=POS_ANGLE, REF=NORTH, lev2_2: ANG = 0, RAD=60 wind_1: OLG OF NEPTUNE BETWEEN 300 330 wind_2: OLG OF NEPTUNE BETWEEN 30 60 comment_1: OBSERVE SKY BACKGROUND GEO AND IPM comment_2: LY ALPHA EMISSIONS NEAR NEPTUNE. comment_3: OFFSET NORTH BY 1 ARC MINUTE. comment_4: ALSO GIVES SKY BACKGROUND FOR comment_5: SATURN AND URANUS, SO PLEASE comment_6: SCHEDULE #1-8 CLOSE IN TIME. fluxnum_1: 1 fluxval_1: SURF(V) = 8.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1216) = 3. +/- 2. E-12 fluxnum_3: 3 fluxval_3: W-LINE(1216) = .04 +/- .02 ! ! end of solar system targets ! No generic target records found exposure_logsheet: ! linenum: 4.100 targname: TITANIA-ACQ config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 2 param_1: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 5; req_2: GROUP 4.1-6.1 NO GAP; req_3: SEQ 4.1-6 NO GAP; req_4: CYCLE 4 / 4.1-9; comment_1: ON-BOARD ACQ OF TITANIA WITH N2. comment_2: WITH GHRS N2 - THEN OFFSET TO comment_3: URANUS FOR ECH-A SPECTRA. comment_4: I TAKE STEP-TIME = 10 SEC comment_5: FOR 2000 COUNTS/DWELL PT. ! linenum: 4.200 targname: TITANIA-ACQ config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 350S fluxnum_1: 1 priority: 3 comment_1: IMAGE OF TITANIA IN LSA comment_2: AFTER CENTERING. EXPECT comment_3: 250 COUNTS MAX. ! linenum: 5.000 targname: URANUS-CENTER config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-A wavelength: 1215.0 num_exp: 6 time_per_exp: 300S s_to_n: 10 s_to_n_time: 300S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 9, param_3: STEP-TIME = 1.0, param_4: DOPPLER = ON req_1: DARK TIME / 5-6 comment_1: OBSERVE URANUS AT PLANET CENTER. comment_2: GHRS ECH-A SPECTRUM OF H LY ALPHA comment_3: LINE WHEN URANUS OLG = 300-330 comment_4: DEGREES. ! linenum: 6.000 targname: URANUS-AUR config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-A wavelength: 1215.0 num_exp: 6 time_per_exp: 300S s_to_n: 10 s_to_n_time: 300S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 9, param_3: STEP-TIME = 1.0, param_4: DOPPLER = ON comment_1: OBSERVE URANUS NEAR LIMB WHERE comment_2: AURORAL EMISSION IS EXPECTED. comment_3: GHRS ECH-A SPECTRUM OF H LY ALPHA comment_4: LINE WHEN URANUS OLG = 300-330 comment_5: DEGREES. NOTE: RAD DEPENDS ON comment_6: DAY OF OBSERVATION. ! linenum: 6.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-A ! wavelength: 1215.5 wavelength: 1215.0 num_exp: 1 time_per_exp: 2M s_to_n: 50 s_to_n_time: 120S fluxnum_1: 1 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 9, param_3: STEP-TIME=1.0 req_1: CALIB FOR 6; req_2: PCS MODE G comment_1: WAVELENGTH CALIBRATION FOR 5-6. comment_2: NO SPYBAL SHOULD OCCURE BETWEEN comment_3: LINE 6-6.1. ! linenum: 7.100 targname: TRITON-ACQ config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 2 param_1: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 8; req_2: GROUP 7.1-9 NO GAP; req_3: SEQ 7.1-8 NO GAP comment_1: ON-BOARD ACQ OF TRITON WITH N2. comment_2: WITH GHRS N2 - THEN OFFSET TO comment_3: NEPTUNE FOR ECH-A SPECTRA. comment_4: I TAKE STEP-TIME = 10 SEC comment_5: FOR 2000 COUNTS/DWELL PT. ! linenum: 7.200 targname: TRITON-ACQ config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 350S fluxnum_1: 1 priority: 3 comment_1: IMAGE OF TRITON IN LSA comment_2: AFTER CENTERING. EXPECT comment_3: 250 COUNTS MAX. ! linenum: 8.000 targname: NEPTUNE config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-A wavelength: 1215.0 num_exp: 5 time_per_exp: 600S s_to_n: 8 s_to_n_time: 600S fluxnum_1: 2 priority: 2 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 9, param_3: STEP-TIME = 1.0, param_4: DOPPLER = ON req_1: DARK TIME comment_1: OBSERVE NEPTUNE AT PLANET CENTER. comment_2: GHRS ECH-A SPECTRUM OF H LY ALPHA comment_3: LINE. NEPTUNE OLG = 300-330 OR 30- comment_4: 60 DEGREES. comment_5: NO SPYBAL SHOULD OCCURE BETWEEN comment_6: LINE 8-8.1. ! linenum: 8.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-A ! wavelength: 1215.5 wavelength: 1215.0 num_exp: 1 time_per_exp: 2M s_to_n: 50 s_to_n_time: 120S fluxnum_1: 1 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 9, param_3: STEP-TIME=1.0 req_1: CALIB FOR 8; req_2: PCS MODE G comment_1: WAVELENGTH CALIBRATION FOR 8-9. ! linenum: 9.000 targname: NEPTUNE-OFFSET-SKY config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-A wavelength: 1215.0 num_exp: 6 time_per_exp: 300S s_to_n: 10 s_to_n_time: 300S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 9, param_3: STEP-TIME = 1.0, param_4: DOPPLER = ON req_1: DARK TIME comment_1: OBSERVE SKY BACKGROUND GEO AND IPM comment_2: LY ALPHA EMISSIONS NEAR NEPTUNE. comment_3: OFFSET NORTH BY 1 ARC MINUTE. comment_4: ALSO GIVES SKY BACKGROUND FOR comment_5: SATURN AND URANUS, SO PLEASE comment_6: SCHEDULE #1-9 CLOSE IN TIME. ! ! end of exposure logsheet