! File: 4601C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:19:16:48 coverpage: title_1: JUPITER'S H LY ALPHA AURORAL/AIRGLOW LINE PROFILE: CYCLE 3 MEDIUM 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: 7.40 num_pri: 6 hrs: Y time_crit: Y funds_length: 12 off_fname: NEIL off_mi: D. off_lname: GERL off_title: PROJECT REP., 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: 313-763-6438 ! end of coverpage abstract: line_1: In a series of IUE observations with 0.14 Angstrom resolution we have line_2: resolved the width of the H Ly alpha emission line from Jupiter's aurora line_3: and dayglow. The initial motivation was to detect the signature of line_4: proton aurora in Jupiter's hydrogen atmosphere, i.e. highly Doppler- line_5: shifted Ly alpha emission from fast proton charge exchange. No proton line_6: aurora have been observed on Jupiter, with a tight upper limit, but the line_7: auroral Ly alpha line does appear broadened with an asymmetry toward line_8: the blue (upward moving) side. Although this was initially interpreted in line_9: terms of fast protons accelerated by auroral potentials, it is also possible line_10: that it represents a supersonic thermospheric wind. Equatorial data on line_11: Jupiter have shown that the observed brightening, or "bulge", is due to line_12: a symmetric broadening of the line rather than a bright core (as line_13: expected for electron collisional excitation). This appears more line_14: consistent with a superthermal population in the upper atmosphere than line_15: particle excitation, and suggests that the auroral broadening may be a line_16: related process. We can in principle identify an auroral thermospheric line_17: expansion away from the auroral oval by spatially resolved spectra at line_18: points on either side of the auroral oval, and we propose to do this in line_19: cycle 3. We will then relate the auroral observations to scheduled line_20: equatorial observations in cycle 2. ! ! end of abstract general_form_proposers: lname: CLARKE fname: JOHN title: PI mi: T. inst: 2660 country: USA ! lname: BEN JAFFEL fname: LOTFI inst: 5466 country: FRANCE esa: Y ! lname: GLADSTONE fname: RANDALL inst: 1506 country: USA ! lname: PRANGE fname: RENEE inst: 5436 country: FRANCE esa: Y ! lname: VIDAL-MADJAR fname: ALFRED inst: 5466 country: FRANCE esa: Y ! lname: WAITE fname: HUNTER inst: 3440 country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: We request 6 dark orbits for this program, with 5 orbits for 5 line_2: latitudes across the northern auroral oval on the central meridian line_3: and 1 orbit for sky background. Each dark orbit will include the line_4: observation of a specific latitude in Jupiter's northern auroral line_5: zone. All observations will be with GHRS G160M and the large line_6: aperture (LSA) for high spectral resolution and sensitivity. line_7: Pointing on Jupiter will be by blind offset, if this turns out to line_8: be accurate to a few tenths of an arc sec, otherwise we will peak line_9: up on one of the Galilean satellites and offset from there to the line_10: desired location on Jupiter. All observations may be performed line_11: with coarse track. The one orbit for a sky background measurement line_12: can be used for sky subtraction from all Jupiter spectra if the line_13: observations are scheduled close in time, and the observations line_14: should be scheduled near Jupiter opposition to minimize the line_15: geocoronal background. Scheduling restrictions will force these line_16: spectra to be taken over a period of several days, and we will line_17: therefore obtain a time-averaged view of the aurora. ! question: 4 section: 1 line_1: The atomic hydrogen line emission from Jupiter's aurora can only line_2: be observed in the far-UV. Ground-based observations have now revealed line_3: quadrupole emissions of H2 and thermal emissions of H3+, but these line_4: emission line shapes are not diagnostic of the dynamics of the upper line_5: atmosphere. We hope to learn about the dynamics of Jupiter's auroral line_6: atmosphere, specifically the very large energy input to the upper line_7: atmosphere and possibly also the interaction between Jupiter's line_8: magnetosphere and auroral upper atmosphere. The 5 latitudes observed line_9: will be +40, +50, +55, +60, and +70 degrees. These are chosen to be line_10: centered on the torus auroral zone with an extension well north and line_11: south of this. Between longitudes of 150-200 degrees we will cover line_12: both sides of the expected auroral oval. The 5 latitudes are needed line_13: to properly sample any variations with latitude. Using the GHRS G160M line_14: with LSA at 1216 A, we expect .096 counts/sec-diode-kR for diffuse line_15: emission compared with a background rate of .008 counts/sec-diode. line_16: The auroral emission is in the range 10-100 kR in brightness, depending line_17: on the level of auroral activity and extent of the emitting region, line_18: and the planetary airglow is ~10 kR. For a 10 kR brightness and a line_19: line 0.2 Angstroms full width at half maximum (FWHM), we would have line_20: ~ 2000 counts/diode on the central part of the line in a 40 min. line_21: integration, or a S/N = 40. ! question: 5 section: 1 line_1: We desire to minimize the sky background subtraction, which line_2: involves minimizing the geocoronal background Ly alpha emission line_3: by observing Jupiter near opposition. All Jupiter spectra will line_4: also be taken when the north auroral zone is tilted toward the line_5: Earth, i.e. when the central meridian longitude is 150-200 line_6: degrees. ! question: 6 section: 1 line_1: The only specific calibrations for this program that are not line_2: generally available will be a flat field at the same y-deflection line_3: as the observations, and an LSA G160M scattered light and line profile line_4: measurement using the on-board Pt-Ne calibration lamps. ! question: 7 section: 1 line_1: The GHRS data will be reduced using standard programs obtained line_2: from the ST ScI and GHRS team at the University of Michigan. The line_3: analysis of the data will involve shifting and co-adding the individual line_4: FP-split segments, applying any flat field, and measuring and line_5: subtracting the background geocoronal and IPM emissions. The IPM line_6: emissions will be largely Doppler-shifted off the planetary lines. line_7: We will then compare models for the line profiles convolved with the line_8: GHRS point spread function with the data from each planet: R. Gladstone line_9: and L. Ben Jaffel will take the lead in modeling the data, and both line_10: 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", J. line_2: 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. GO 3511 - "H Ly alpha Dayglow Emission Line Profiles from the Outer Planets", line_10: J. Clarke PI - related. line_11: 6. GO 3616 - "Upper Atmospheres of Uranus and Neptune", J. Clarke Co-I - may be line_12: related scientifically. line_13: 7. GO 3862 - "The Excitation of the Atmospheres of Planetary Satellites", J. line_14: Clarke PI - unrelated. line_15: 8. GTO 1269 - "Far UV Observations of the Giant Planets", A. Vidal-Madjar Co- line_16: I - related. line_17: 9. GO 2461 - "Interplanetary/interstellar gas connection: search for the local line_18: cloud" - A. Vidal-Madjar Co-I - unrelated. line_19: 10. GO 2536 - "Deuterium in the local interstellar gas" - A. Vidal-Madjar PI line_20: - unrelated. ! question: 10 section: 1 line_1: Complete computing facilities are in place and available within line_2: the Space Physics Research Laboratory at the University of Michigan line_3: for use on this project. Two VAX 750's and a VAX 8600 are accessible line_4: via a local area network, in addition to the Michigan network MERIT, line_5: SPAN, and NASA Internet. Two Sun Sparcstations with IDL are presently line_6: being used for IUE and HST data reductions. All Co-Investigators also line_7: have complete computer facilities available at their institutions for line_8: use on this project, and graduate students are available at all line_9: institutions for assistance with 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+40 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 2. lev2_1: TYPE=TORUS,POLE_LAT=90, lev2_2: RAD=69370.,LAT=+40,LONG=0 wind_1: OLG OF JUPITER BETWEEN -30 30, wind_2: CML OF JUPITER FROM EARTH wind_3: BETWEEN 150 200 comment_1: GHRS LSA WITH G160M ON comment_2: JUPITER CML AND +40 DEGREES comment_3: LATITUDE. OBSERVE H LY comment_4: ALPHA LINE PROFILE FROM comment_5: NEAR-AURORAL ATMOSPHERE comment_6: WHEN LIII = 150-200 DEG. 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+50 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 2. lev2_1: TYPE=TORUS,POLE_LAT=90, lev2_2: RAD=68570.,LAT=+50,LONG=0 wind_1: OLG OF JUPITER BETWEEN -30 30, wind_2: CML OF JUPITER FROM EARTH wind_3: BETWEEN 150 200 comment_1: GHRS LSA WITH G160M ON comment_2: JUPITER CML AND +50 DEGREES comment_3: LATITUDE. OBSERVE H LY comment_4: ALPHA LINE PROFILE FROM comment_5: NEAR-AURORAL ATMOSPHERE comment_6: WHEN LIII = 150-200 DEG. 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: 3 name_1: JUPITER+55 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 2. lev2_1: TYPE=TORUS,POLE_LAT=90, lev2_2: RAD=68190.,LAT=+55,LONG=0 wind_1: OLG OF JUPITER BETWEEN -30 30, wind_2: CML OF JUPITER FROM EARTH wind_3: BETWEEN 150 200 comment_1: GHRS LSA WITH G160M ON comment_2: JUPITER CML AND +55 DEGREES comment_3: LATITUDE. OBSERVE H LY comment_4: ALPHA LINE PROFILE FROM comment_5: NEAR-AURORAL ATMOSPHERE comment_6: WHEN LIII = 150-200 DEG. 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: 4 name_1: JUPITER+60 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 2. lev2_1: TYPE=TORUS,POLE_LAT=90, lev2_2: RAD=67840.,LAT=+60,LONG=0 wind_1: OLG OF JUPITER BETWEEN -30 30, wind_2: CML OF JUPITER FROM EARTH wind_3: BETWEEN 150 200 comment_1: GHRS LSA WITH G160M ON comment_2: JUPITER CML AND +60 DEGREES comment_3: LATITUDE. OBSERVE H LY comment_4: ALPHA LINE PROFILE FROM comment_5: NEAR-AURORAL ATMOSPHERE comment_6: WHEN LIII = 150-200 DEG. 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: 5 name_1: JUPITER+70 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 2. lev2_1: TYPE=TORUS,POLE_LAT=90, lev2_2: RAD=67270.,LAT=+70,LONG=0 wind_1: OLG OF JUPITER BETWEEN -30 30, wind_2: CML OF JUPITER FROM EARTH wind_3: BETWEEN 150 200 comment_1: GHRS LSA WITH G160M ON comment_2: JUPITER CML AND +70 DEGREES comment_3: LATITUDE. OBSERVE H LY comment_4: ALPHA LINE PROFILE FROM comment_5: NEAR-AURORAL ATMOSPHERE comment_6: WHEN LIII = 150-200 DEG. 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: 6 name_1: SKY-BACKGROUND descr_1: OFFSET JUPITER lev1_1: STD = JUPITER, ACQ = 30. lev2_1: TYPE=POS_ANGLE,RAD=180., lev2_2: ANG=0.,REF=NORTH wind_1: OLG OF JUPITER BETWEEN -30 30 comment_1: GHRS LSA WITH G160M ON comment_2: SKY ROUGHLY 3 ARC MIN comment_3: FROM JUPITER. OBSERVE H LY comment_4: ALPHA LINE PROFILE FROM comment_5: SKY BACKGROUND GEO AND IPM comment_6: EMISSIONS. fluxnum_1: 1 fluxval_1: SURF-LINE(1216) = 1. +/- 1. E-11 fluxnum_2: 2 fluxval_2: W-LINE(1216) = 0.10 +/- 0.1 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 targname: JUPITER+40 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 4 time_per_exp: 660S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = DEF, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON req_1: CYCLE 3 / 1-6; req_2: PCS MODE C / 1-6; req_3: DARK TIME /1-6; ! linenum: 2.000 targname: JUPITER+50 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 4 time_per_exp: 660S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = DEF, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON ! linenum: 3.000 targname: JUPITER+55 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 4 time_per_exp: 660S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = DEF, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON ! linenum: 4.000 targname: JUPITER+60 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 4 time_per_exp: 660S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = DEF, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON ! linenum: 5.000 targname: JUPITER+70 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 4 time_per_exp: 660S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = DEF, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON ! linenum: 6.000 targname: SKY-BACKGROUND config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223.0 num_exp: 4 time_per_exp: 660S fluxnum_1: 2 priority: 1 param_1: FP-SPLIT = STD, param_2: STEP-PATT = DEF, param_3: STEP-TIME=1.0, param_4: DOPPLER = ON ! ! end of exposure logsheet ! No scan data records found