! File: 4792C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:03:40:31 coverpage: title_1: H LY ALPHA DAYGLOW EMISSION LINE PROFILES FROM THE OUTER title_2: PLANETS - PART TWO 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: 5.97 num_pri: 6 hrs: Y time_crit: Y funds_length: 12 off_fname: A. off_mi: W. off_lname: STEISS off_title: DIRECTOR, DRDA off_inst: UNIVERSITY OF MICHIGAN off_addr_1: 475 E. JEFFERSON off_city: ANN ARBOR off_state: MI off_zip: 48109 off_country: USA off_phone: 313-764-7230 ! end of coverpage abstract: line_1: One of the outstanding scientific questions about the outer planets line_2: following the Voyager tour is why the upper atmospheres have bright line_3: FUV airglow emissions and very high exospheric temperatures of 400 - line_4: 1200 K on the 4 planets. IUE observations of Jupiter's H Ly alpha line_5: emission line profile have shown that the equatorial lines are broad, line_6: and can be fit by the inclusion of a velocity distribution in addition line_7: to thermal motions (although the physical process leading to this line_8: additional component has not been identified). It is clear that if the line_9: bright H Ly alpha emissions from the outer planets are due mainly to line_10: resonant scattering of solar and interplanetary emissions, as observed line_11: on Jupiter and Saturn from long term correlations with the solar line_12: Ly alpha flux, then the lines from all 4 planets must be broad to line_13: explain the observed high albedos. The H Ly alpha lineshapes certainly line_14: provide a discriminant between processes of resonant scattering and line_15: charged particle excitation. We propose to obtain good signal H Ly line_16: alpha line profile measurements at the center and limb of Jupiter line_17: to resolve the questions about the excitation processes and to line_18: explore the possibility that the upper atmospheric line broadening line_19: process is also the source of the observed thermospheric heating. line_20: Note- this program was originally a part of 3511. ! ! end of abstract general_form_proposers: lname: CLARKE fname: JOHN title: PROF. mi: T. inst: UNIVERSITY OF MICHIGAN country: USA ! lname: GLADSTONE fname: RANDALL inst: UNIVERSITY OF CALIFORNIA, BERKELEY country: USA ! lname: BEN JAFFEL fname: LOTFI inst: UNIVERSITY OF ARIZONA country: USA ! lname: PRANGE fname: RENEE inst: INSTITUT D'ASTROPHYSIQUE SPATIALE country: FRANCE esa: Y ! lname: VIDAL-MADJAR fname: ALFRED inst: OBSERVATOIRE DE PARIS country: FRANCE esa: Y ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: We require 3 dark orbits for Jupiter line_2: (bulge center, bulge limb, and mid-latitudes). line_3: and one geocoronal/interplanetary H Ly alpha sky background. The Jupiter line_4: observations will consist of one dark orbit integration each pointing the GHRS line_5: SSA with G160M at 1) Jupiter's equatorial "Ly alpha bulge" region on the line_6: central meridian, 2) the bulge longitudes (equator) at 70 degrees from the line_7: central meridian toward the sunlit limb, and 3) midlatitudes on the central line_8: meridian. line_9: Jupiter can be acquired by blind pointing on coarse track, and GHRS line_10: autonomous acquisition will be used for Uranus, also on coarse track. ! question: 4 section: 1 line_1: We are also pursuing this program with IUE observations of Jupiter, and have line_2: applied to observe Saturn and Uranus: Neptune is too faint for IUE at high line_3: resolution. These observations are limited by the lower sensitivity, and line_4: roughly a factor of two lower spectral resolution, of IUE compared with the line_5: GHRS G160M and SSA. The existing IUE data with the SWP camera and small line_6: aperture at high dispersion have been published (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 should allow us to obtain high quality H Ly alpha emission line_10: line profiles of discrete regions on Jupiter, and determine the full line_11: line shapes (including the wings) on those planets. ! question: 5 section: 1 line_1: We desire to minimize the geocoronal background Ly alpha emission, and also line_2: to obtain the maximum Doppler shifts between the planetary and geocoronal line_3: emissions. This is accomplished by observing when the planet is roughly 30-60 line_4: degrees from the anti-solar point, so that the combined Earth and HST orbital line_5: motions of 38 km/sec have large components along the line of sight during the line_6: dark portion of the HST orbit when the background is minimal. A preferred line_7: Jupiter longitude range is desired for those observations, but there are no line_8: longitude requirements for the other planets. ! question: 6 section: 1 line_1: The only specific calibrations for this program that are not generally line_2: available will be a flat field at the same y-deflection as the observations, line_3: and an SSA G160M scattered light and line profile measurement using the on- line_4: board Pt-Ne calibration lamps. ! question: 7 section: 1 line_1: The GHRS data will be reduced at the University of Michigan using standard line_2: programs obtained from the ST ScI or GHRS team. The analysis of the data will line_3: involve shifting and co-adding the individual FP-split segments, applying any line_4: flat field, and measuring and subtracting the background geocoronal and IPM line_5: emissions. The IPM emissions will be largely Doppler-shifted off the planetary line_6: lines, and we will schedule the observations when the planetary lines have line_7: nearly the largest possible Doppler shift from the geocoronal emission (see line_8: above). We will then compare models for the line profiles convolved with the line_9: GHRS point spread function (as in Figure 2) with the data from each planet: R. line_10: Gladstone and L. Ben Jaffel will take the lead in modeling the data, and both line_11: have modeling codes ready for use. ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: 1. GO 2602 - "The Excitation of the Atmospheres of Planetary Satellites", line_2: J. Clarke PI - unrelated. line_3: 2. GO 2603 - "Parallel Observations of H Ly alpha Emission from the Local ISM", line_4: J. Clarke PI - related for sky background. line_5: 3. GO 2393 - "D/H Ratio of Venus and Mars from Lyman alpha Emission", J. Clarke line_6: Co-I - unrelated. line_7: 4. GO 2625 - "Excitation Processes for the Outer Planet UV Emissions", J. line_8: Clarke Co-I - possibly related scientifically. line_9: 5. GTO 1269 - "Far UV Observations of the Giant Planets", A. Vidal-Madjar line_10: Co-I - related. line_11: 6. GO 2727 - "Search for Exogenous Water in Saturn's Atmosphere: A Critical line_12: Test for Ring Erosion Theories", R. Prange PI - unrelated. ! 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 network, line_4: in addition to the Michigan network MERIT, SPAN, and NASA Internet. A SUN 4/110 line_5: workstation with IDL is presently being used for IUE and HST data reductions, line_6: and a Sparcstation IPX with IDL is being procured under cycle 1 GO funding. All line_7: Co-Investigators also have complete computer facilities available at their line_8: institutions for use on this project, and graduate students are available at line_9: all institutions for assistance on this project. ! !end of general form text general_form_address: lname: CLARKE fname: JOHN mi: T. title: PROF. category: PI inst: UNIVERSITY OF MICHIGAN addr_1: AOSS DEPT. city: ANN ARBOR state: MI zip: 481092143 country: USA ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: JUPITER-CML descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 2. lev2_1: TYPE=TORUS,POLE_LAT=90, lev2_2: RAD=66900,LAT=0,LONG=0 wind_1: OLG OF JUPITER BETWEEN 30 60, wind_2: CML OF JUPITER FROM EARTH wind_3: BETWEEN 50 150 comment_1: OBSERVE JUPITER "BULGE" REGION AT comment_2: 50-150 DEG. SYSTEM III LONGITUDE AND comment_3: MAGNETIC EQUATOR ON CENTRAL MERIDIAN. comment_4: GHRS G160M SPECTRUM OF LY ALPHA LINE comment_5: PROFILE WITH LSA. OLG = 30-60 FOR comment_6: TARGETS 1-3 MEANS ROUGHLY 28 FEB. comment_7: TO 27 MARCH 1993. fluxnum_1: 1 fluxval_1: SURF(V) = 5.3 fluxnum_2: 2 fluxval_2: SURF-LINE(1216) = 2. +/- 1. E-11 fluxnum_3: 3 fluxval_3: W-LINE(1216) = 0.15 +/- 0.1 ! targnum: 2 name_1: JUPITER-MIDLATITUDE descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 2. lev2_1: TYPE=TORUS,POLE_LAT=90, lev2_2: RAD=66900,LAT=+30,LONG=0 wind_1: OLG OF JUPITER BETWEEN 30 60, wind_2: CML OF JUPITER FROM EARTH wind_3: BETWEEN 150 50 comment_1: OBSERVE JUPITER MIDLATITUDES AT comment_2: 150-50 DEG. SYSTEM III LONGITUDE AT comment_3: +30 DEG. LATITUDE ON CENTRAL MERIDIAN. comment_4: GHRS G160M SPECTRUM OF LY ALPHA LINE comment_5: PROFILE WITH LSA. fluxnum_1: 1 fluxval_1: SURF(V) = 5.3 fluxnum_2: 2 fluxval_2: SURF-LINE(1216) = 2. +/- 1. E-11 fluxnum_3: 3 fluxval_3: W-LINE(1216) = 0.15 +/- 0.1 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 targname: JUPITER-CML config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 2 time_per_exp: 1350S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 5, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON req_1: CYCLE 2 / 1-3; req_2: PCS MODE C / 1-2; req_3: DARK TIME /1-2; ! linenum: 2.000 targname: JUPITER-MIDLATITUDE config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 2 time_per_exp: 1350S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 5, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON ! linenum: 3.000 targname: EARTH-CALIB config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 3 time_per_exp: 700S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = 5, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON req_1: PCS MODE G ! ! end of exposure logsheet ! No scan data records found