! File: 4608C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:19:31:11 coverpage: title_1: MULTI TIMESCALE MULTISPECTRAL OBSERVATION OF THE JOVIAN AURORA title_2: CYCLE3 HIGH sci_cat: SOLAR SYSTEM sci_subcat: GIANT PLANETS proposal_for: GO pi_title: PROF pi_fname: JEAN-CLAUDE pi_mi: MC pi_lname: GERARD pi_inst: UNIVERSITE DE LIEGE pi_country: BELGIUM pi_phone: 32-41-529980 keywords_1: GIANT PLANETS, UV AURORA, H2, LYMAN-ALPHA hours_pri: 6.60 num_pri: 1 foc: Y time_crit: Y funds_amount: 51250 funds_length: 12 funds_date: JAN-93 pi_position: RESEARCH DIRECTOR off_fname: JAN off_mi: MJ off_lname: BERNARD off_title: CONSEILLER off_inst: SERVICE DE PROGRAMMATION DE LA POLITIQUE SCIENTIFIQUE off_addr_1: RUE DE LA SCIENCE, NB 8 off_city: BRUXELLES off_zip: 1040 off_country: BELGIUM off_phone: 32-2-2383583 ! end of coverpage abstract: line_1: Previous HST observations made with the FOC have demonstrated the ability of the line_2: HST to provide high spatial resolution images of the ultraviolet jovian aurora. line_3: They and other IUE and Voyager UVS observations suggest that wavelength line_4: dependence and time variations line_5: occur with different characteristic times. We propose to image the ultraviolet line_6: jovian aurora in several passbands to investigate its temporal variation on line_7: timescales ranging from ~10 min to hours. Exposures will be made when the line_8: 180 deg (Lambda III) longitude sector, where the aurora is best visible from line_9: Earth orbit, faces the Earth. Due to the expected loss of sensitivity in the line_10: far UV, this program should be preformed before the COSTAR correction. line_11: Coordinated IR measurements of emission connected to the UV aurora but line_12: originating from different altitude regions will be obtained in parallel with line_13: HST observations. Simultaneous radio observations of decametric jovian line_14: emissions and IUE UV spectra will also provide complementary data on energetic line_15: particle precipitation. The observed morphology, color ratio and characteristic line_16: time of the temporal variations will provide key information to discriminate line_17: between the various origins , identity and acceleration mechanisms of the line_18: precipitating particles. Theoretical models of particle interaction with the line_19: jovian magnetic field and atmosphere available from the proposing team will be line_20: used to derive quantitative information on these processes. ! ! end of abstract general_form_proposers: lname: GERARD fname: JEAN-CLAUDE title: PR mi: MC inst: 4330 country: BELGIUM esa: Y ! lname: BALLESTER fname: GILDA title: DR mi: . inst: 2380 country: USA ! lname: BENJAFFEL fname: LOTFI title: DR inst: 5436 country: FRANCE esa: Y ! lname: DOLS fname: VINCENT mi: J. inst: 4330 country: BELGIUM esa: Y ! lname: PARESCE fname: FRANCESCO title: DR inst: 3470 country: USA esa: Y ! lname: PRANGE fname: RENEE title: DR inst: 5448 country: FRANCE esa: Y ! lname: REGO fname: DANIEL inst: 5448 country: FRANCE esa: Y ! lname: WAITE fname: HUNTER title: DR mi: J. inst: 3440 country: USA ! lname: STORRS fname: ALEX title: DR mi: D. inst: 3470 country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: The jovian polar aurora in not only one of the most fascinating phenomena in line_2: the solar system, it has recently become, through the possibility of UV imaging line_3: with the HST and infrared observations from the ground, one of the key line_4: scientific fields where new, carefully planned observations will provide line_6: important insight. As with other planets , jovian aurorae are the visible line_7: signature of the coupling between the magnetosphere and the planets' line_8: atmospheres. For the outer planets which can rarely be visited, they provide a line_9: unique tool for the study of the magnetosphere, the effect of the solar wind line_10: and/or the planetary rotation on its dynamics and energetics, the satellites as line_11: plasma sources and energetic particle sinks and the global electrodynamical line_12: convection patterns coupling the magnetosphere and the ionosphere. Based on the line_13: terrestrial example and on specific studies of the Jovian magnetosphere (the few line_14: in-situ data from Pioneer, Voyager and Ulysses and theoretical work), several line_15: candidate processes have been identified for driving the Jovian aurorae and line_16: these can either dominate or coexist: line_17: - precipitation of magnetospheric particles (electrons, protons, and/or ions) line_18: pitch-angle diffused by e.m. waves in the Io plasma torus (diffuse aurora) line_19: - precipitation of particles, mainly electrons, accelerated by potential drops line_20: along magnetic field lines connected to various regions of the magnetosphere line_21: where intense field-aligned currents can flow (Io flux tube, plasma disc, outer line_22: magnetosphere field lines reconnecting to the solar wind (discrete aurorae) line_23: - precipitation of solar wind particles either directly into the cusp or soon ! question: 2 section: 2 line_1: after injection in the magnetosheath and/or the boundary layer (giving either line_2: diffuse or discrete aurorae). line_3: The characteristics of the resulting auroral emissions must be different and line_4: bear the signature of the precipitation processes. In particular: line_5: - they differ in their morphology (forming ovals or only arcs at different line_6: latitudes, connected to Io, to the Io plasma torus, to the middle or the outer line_7: magnetosphere, or even extending into the polar cap, and looking as diffuse or line_8: discrete emissions) and by the energy/penetration depth of the precipitating line_9: particles (up to 100 kev or about MeV/nucleon if electrons or ions diffused by line_10: e.m. waves, keVs to tens of keVs if accelerated by electric fields, 100eVs to line_11: keVs if coming from the solar wind or the boundary layers). line_12: - they differ in the timescale of their temporal variations (timescales of line_13: months for the plasma torus, of days or fractions of day for the pitch angle line_14: diffusion, of hour(s) for the solar wind control, and down to a few minutes for line_15: field aligned currents generating acceleration structures and discrete aurorae) line_16: - they differ in the associated emissions in various other wavelength ranges: line_17: radioemission is only excited by keV electrons in acceleration structures and line_18: the electron bremsstrahlung spectrum differs from heavy ion X ray lines (only line_19: observed for ion pitch angle diffusion), extremely intense IR emission can be line_20: expected to be due to Joule heating from field aligned currents. line_21: The morphology of the Jovian UV aurora is now the best documented aspect of this line_22: research field. The paradigm derived from the limited spatial resolution/ non line_23: imaging observations of Voyager and IUE was that of two emitting rings ! question: 2 section: 3 line_1: surrounding the north and south poles, confined within an oval close to the Io line_2: orbit footprint (north 'UVS oval', Broadfoot et al., 1981), or at slightly line_3: higher latitude (615 line_3: (Ladreiter and Leblanc, 1990?). Both sources are modulated in longitude with a line_4: maximum in the same region as the UV maximum. The non Io source is variable, line_5: and correlated with the solar wind activity. Correlations between the line_6: decametric emission (routinely observed from the ground) and the UV one is very line_7: difficult, due to the specific conditions of the radio propagation and the lack line_8: of spatial resolution. However, a correlated event was first detected in line_9: December 1990 (Prange et al., 1992b), providing new insights on the Jovian line_10: auroral mechanism(s). line_11: Consequently, we plan to take advantage of the high spatial resolution of the line_12: FOC which will allow meaningful localized comparison between the H-Ly alpha, the line_13: We and the Ly H2 emission and existing one dimensional models. The variability line_14: of the various spatial auroral features, already identified on various magnetic line_15: field lines by earlier mapping, will be investigated on several timescales line_16: representative of various magnetospheric processes from tens of min to weeks. line_17: In addition, correlated observations at a comparable spatial resolution will be line_18: performed in the near- and mid-IR for comparison of localized spatial structures line_19: and of their variability. Finally, the temporal variations of the decametric line_20: radioemission, routinely recorded from the ground will be compared to variations line_21: of the discrete auroral features. Time for a parallel campaign of Jovian line_22: auroral observation with IUE has also been requested. In summary, we propose a line_23: short,time-effective program to image the UV aurora simultaneously with coor- ! question: 2 section: 8 line_1: This set of observations will allow to identify the different components of the line_2: Jovian aurora, to characterize the magnetospheric processes and thereby to line_3: construct a global picture of this fascinating phenomenon . line_4: References line_5: ---------- line_6: Ballester, G.E., R. Prange, S. Kim, T. Livengood, H.W. Moos, and J. line_7: Caldwelbt 1991, . Sandel, and A.L. Broadfoot, 1987, J. Geophys. Res., 92, line_8: 3141 line_9: Horanyi, M., T.E. Cravens, and J.H. Waite, Jr., 1988, J. Geophys. Res., 93, line_10: 7251 line_11: Kim, S.J., J. Caldwell, and T.M. Herbst,1992, Icarus,96, 143 Kostiuk, T., P. line_12: Romani, F. Espenak, T. Livengood, and J Goldstein, "Variable Phenomena in line_13: Jovian Systems", Annapolis, 23-26 july 1992 line_14: Ladreiter, H.P., and Y. Leblanc, 1990, J. Geophys. Res., 95,6427 line_15: Livengood, T.A., D.F. Strobel, and H.W. Moos, 1990, J. Geophys. Res., 95, line_16: 10375 line_17: Livengood, T.A., R. Prange, G.E. Ballester and W.H. Moos, 1991, EOS, 72, 186 line_18: Livengood, T.A., H.W. Moos, G.E. Ballester, and R.M. Prange, 1992, Icarus, line_19: 97,26 line_20: Prange, R., 1991, Astron. Astroph., 251, L15 line_21: Prange, R. and M. Elkhamsi, 1991, J. Geophys. Res., 96, 21371 line_22: Prange, R., D. Rego, and J.C. Gerard, 1992, submitted for publication. line_23: Prange, R., V. Dols, J.C. Gerard, and F. Paresce, 1992a, in "Variable ! question: 2 section: 9 line_1: Phenomena in Jovian Systems", Annapolis, 23-26 july 1992. line_2: Prange, R., P. Zarka, G.E. Ballester, T.A. Livengood, H.W. Moos, and L. line_3: Denis, 1992b, "Variable Phenomena in Jovian Systems", Annapolis, July 1992, to line_4: be submitted to J. Geophys. Res. line_5: Rego, D., R. Prange, and J.C. Gerard, 1992, submitted for publication. line_6: Waite, J.H.,Jr., T.E. Cravens, J. Kozyra, A.F. Nagy, S.K. Atreya, and R.H. line_7: Chen, 1983, J. Geophys. Res., 88, 6143 line_8: Waite, H. Jr., 1992, paper presented at "Variable Phenomena in Jovian Systems", line_9: Annapolis, 23-26 july 1992 ! question: 3 section: 1 line_1: As described in the scientific justification, we plan to investigate the time line_2: variation of the jovian aurora at different timescales and wavelengths by taking line_3: advantage of the FOC filter combinations and coordinating with parallel IR and line_4: radio ground observations. line_5: As far as the HST observations are concerned, this objective will be realized by line_6: imaging the jovian northern auroral zone with the FOC using the F/96 relay using line_7: the zoomed pixel format (8-bit words, 22 x 22 arcsec) to increase the visibility line_8: of the the aurora. Previous experience has demonstrated that the count rate is line_9: low enough to prevent 8-bit word saturation.OOB line_10: The aurora will be imaged at Lyman alpha, and in the line_11: Werner and Lyman bands of H2 using combinations of filters which adequately line_12: isolate the desired wavelength ranges: F120M+F140W, F130M+F140W and F152M+F175W, line_13: respectively. These combinations were already successfully used line_14: in GTO program 1269 and DDP4005. Sequences of exposures will be repeated line_15: with various periodicities to check systematically the variability of the north line_16: aurora versus several magnetospheric time scales: 1-2 hours line_17: (from one orbit to the next), 10-15 hours (over one Jovian rotation), and days- line_18: weeks. The shortest timescales of minutes suggested by previous observations line_19: will be checked in a single wavelength range (H2 Lyman) by successive exposures line_20: taken on the same orbit (2 exposures within about 1/2 hour). line_21: Since the global morphology will be known at that time well enough to allow us line_22: to fully analyze the limb brightning effect and the possible contributions from line_23: the back side of the auroral oval, we will compare images of the same ! question: 3 section: 2 line_1: selected longitude sector of Jupiter where the aurora has proven to be most line_2: active. The CML will be fixed at 180 deg +/- 58 deg (Jupiter rotation during one line_3: HST period) for the central exposure of each sequence, the individual features line_4: in the images being easy to localize within about 60 deg. from the central line_5: meridian. line_6: Additional short exposures with a suitable set of filters will be line_7: made on the first two visits to locate accurately the limb of the planet and line_8: cross check the limb determination derived during each sequence from the H2 line_9: Lyman images. line_10: This program will be implemented as follows: line_11: 1. During 4 CONSECUTIVE HST orbits, line_12: a. A continuum image will be made using the F210M,F220W,F6ND filters line_13: SIII Central Meridian Longitude = 70 deg. line_14: b. A first 15-min. FOC exposure with the F152+F175W filters line_15: (H2 Lyman-bands) will be obtained when the SIII Central line_16: Meridian Longitude = 130 deg. line_17: c. During the next orbit, two consecutive 15-min. exposures will be line_18: made, through the same filter combination . SIII CML will be near line_19: 190 deg. and 200 deg. respectively. line_20: Data collected during the 3 HST orbits will reveal the importance and features ! question: 3 section: 3 line_1: of the time variation of the precipitation pattern and/or magnetospheric line_2: variation of the precipitation pattern and/or magnetospheric processes line_3: on the time scales of 15 min. and 1-2 hours. line_4: 2. The same sequence 1a-c is repeated during the following jovian rotation, line_5: that is ~10 hours later but with the filter combination F120M+F140W line_6: ( HI Ly-alpha) and CMLs as close as possible to those of sequence 1. line_7: 3. Sequence 1b-c is repeated during the next jovian rotation with filters line_8: F152M+F175W and for CMLs as close as possible to sequence 1 line_9: 4. Sequence 1b-c is repeated during the next jovian rotation with filters line_10: F130M+F140W (H2 Werner-bands) with CMLs as close as possible to sequence 1. line_11: The sequences 1,2,3 and 4 will provide the multispectral imaging together with line_12: information concerning the 15-min, 1-2 and 10 hour variability of the jovian line_13: aurora. line_15: Revised 4 Feb. 1993 to include FOC bright object observation safety procedures. line_16: Contact Alex Storrs (STScI, storrs@stsci.edu, 410-338-4903) with questions. ! question: 4 section: 1 line_1: The IMAGING CAPABILITY of the FOC/HST in the ultraviolet is unique and essential line_2: to reach our scientific objectives. No other spacecraft or ground equipment can line_3: provide images of the UV jovian aurora. In fact, the ability of HST to provide line_4: images of the aurora of Jupiter may be considered as one of the major line_5: accomplishments of the HST in planetary sciences so far. Voyager UVS, IUE and line_6: HST observations have provided important information on the morphology of the UV line_7: jovian aurora, thereby opening a new era of scientific study of Jupiter's magne line_8: tospheric environment and physical processes. Previous FOC/HST observations line_9: in the GTO ULYSSES encounter program have demonstrated the ability of HST to line_10: monitor the spatial distribution of auroral phenomena from Earth orbit. line_11: However, no systematic information has ever been gathered concerning the time line_12: variation of the jovian aurora and the time constants involved in the physical line_13: processes controling particle precipitation. Only hints that such variations line_14: exist were provided by IUE and Voyager UVS spectrometer observations with very line_15: crude spatial resolution. Ground-based infrared observations also suggest the line_16: existence of time variations but they could not have been related to the UV line_17: aurora until HST UV imaging became possible. line_18: This program provides a unique opportunity to accomplish a major step towards line_19: the understanding of the jovian magnetospheric physics using an approach whose line_20: feasibility has now been clearly demonstrated. The parallel ground-based IR line_21: and radio observations will provide key information extremely useful in line_22: understanding future IR observations and their relation to the UV aurora. line_23: As shown by previous HST imaging of the same target, the aberration problem of ! question: 4 section: 2 line_1: the HST does not prevent obtaining good quality auroral observations. line_2: The amount of exposures requested in this program is the best possible line_3: compromise between the need to obtain as many images of the same auroral sector line_4: as possible and the limits on the spacecraft time available. Only one object line_5: (the northern polar region of Jupiter) is requested and use is made of the line_6: planet's rotation and HST orbit to obtain time sequences of the auroral line_7: phenomenon. The exposure times are based on observational experience with the line_8: same filters combinations obtained during our and other previous observations of line_9: the same object (GTO program 1269, DDP 4005). They are limited on one side by line_10: the need to obtain a sufficient S/N ratio and, on the other side, on the limits line_11: to spatial resolution set by the planet's rotation during the exposures. line_12: Pictures shown before demonstrate that good quality data may be collected with line_13: this observational and instrumental configurations. line_14: For example, previous 20 min Ly-alpha exposures (F120M + F140W) provide a S/N line_15: ratio of about 4. Previous H2 Ly-bands 15 min exposures (F152M + F175W) were line_16: obtained with a S/N of nearly 10. ! question: 5 section: 1 line_1: line_8: A coordinated campaign involving simultaneous observations with IUE has line_9: been planned for 1993. If possible, this program should be line_10: scheduled within one of the IUE windows, preferably before 17 July 1993. ! question: 7 section: 1 line_1: The set of co-investigators of this program covers all fields of expertise line_2: needed to collect and process the data, analyze the images and make a thorough, line_3: in-depth study of their significance and implications in the field of Jupiter' line_4: magnetospheric and atmospheric sciences. The PI and most Co-Is have a wide line_5: scientific experience in the fields of planetary atmospheres and magnetospheres line_6: and image processing. They have published a large number of scientific papers line_7: in international refereed journals. More specifically, the plans for data line_8: reduction and analysis are as follows. line_10: 1) The observations will be obtained and processed under the lead of the PI with line_11: active participation by Dols, Paresce, Storrs who have experience with line_12: the FOC and auroral UV observations and the STScI data pipeline and support line_13: and have already successfully analyzed FOC images of Io and of the Jovian line_14: aurora from GTO 1269 program (see list of publications). In addition to the line_15: procedures develloped at the PI's institutions,various IDL procedures have been line_16: developed by G.E. Ballester and J.H. Waite's to analyze HST, IUE and IR line_17: (Protocam images) observations. Other ones will be developed as needed by the line_18: program. line_19: Since the discovery of the spherical aberration, we have been especially line_20: concerned with the numerical deconvolution methods. Several methods are line_21: currently implemented on our workstations and have successfuly been used for the line_22: restoration of Io images in the GTO 1269 program. line_23: 2) One of the major problem in comparing images taken at different time (i.e. ! question: 7 section: 2 line_1: with different guide stars) and in comparing UV images with IR images, will be line_2: the accuracy obtained in the location of the auroral features, which must line_3: reach a fraction of arcsec. This issue is addressed by the presence of the line_4: combination of filters 152M+175W which shows the limb of the planet as seen in line_5: previous GTO images at this wavelength). line_6: This will be improved by a few visible image during the line_7: observing sequence. In any case, the analysis needs experience in limb fitting line_8: G.E. Ballester has developed this expertise from the analysis of IR Protocam line_9: images. line_10: The retrieved images will then be analyzed for any effects such as limb line_11: darkening and/or limb brightning at the various wavelengths, including line_12: resonant scattering at Lyman alpha, with already developed codes (L. BenJaffel line_13: and D. Rego). The contribution of emission from the backside of the auroral line_14: oval at the limb or just behind the limb will be modeled using the global line_15: representation of the north aurora derived from our GTO program (mapping of line_16: the aurora over a whole jovianain rotation, to be scheduled). line_17: 3) Once processed and analyzed, the HST images will be compared at various line_18: wavelength and their characteristic spatial features, their differences if any, line_19: and their temporal variations will be theoretically interpreted. Several line_20: numerical models were developed by the PI and Co-Is to analyze and model line_21: planetary auroral observations: line_22: - a code for generating synthetic spectra of the H2 bands and continuum line_23: in the 1100-2000 A range and their calculating their transmission through the ! question: 7 section: 3 line_1: FOC UV filters has been developed at the P.I.'s institution. It will be used to line_2: convert the measured count rate into total H2 emission rates. line_3: - modeling of multiple wavelength emissions (R.Prange, D.Rego,J.H.Waite, line_4: J.C. Gerard), including altitude distribution of the excitation by energetic line_5: particle and absorption by hydrocarbons and color ratio calculations line_6: - calculations of energetic particle interaction with Jupiter's atmos line_7: phere and iterative modeling of the Jovian atmosphere (providing a reliable line_8: auroral atmospheric model to be used in the previous calculations) have been line_9: developed and are still being improved (H. Waite) line_10: - radiative transfer analysis of UV emissions in an optically line_11: thick atmosphere (L. Ben Jaffel, D. Rego) line_12: - model of the longitudinal distribution of the energy deposition rate line_13: which we expect to derive informations on the injection mechanism of the line_14: particles, their equatorial distribution, the ratio of the electrons/ion input line_15: flux and to put new constrains on the ground level magnetic field (R. Prange) line_16: 4) Parallel IR and radio DAM data will be obtained through Co-Is G.E. line_17: Ballester, R. Prange, and H.W. Waite. Two of them (Ballester and Prange) have line_18: already a several years experience in the organization and analysis of line_19: correlated IR/UV observing campaigns between IRTF(Hawaii) and IUE (see line_20: references in the scientific justification). They have also developed line_21: collaborations with IR observers from the major observatories. Prange has also line_22: developed expertise in the analysis of radio emission and their correlations line_23: with UV data from IUE (see scientific justification). Prange and Waite can ! question: 7 section: 4 line_1: bring collaborators in the field of radio observations and modeling from line_2: France, US, and Japan. line_4: 4) The PI will have the overall responsibility to obtain the data, analyse line_5: them, coordinate a fast and efficient analysis and publish them in the line_6: scientific literature. ! question: 8 section: 1 line_1: As briefly described in (2) and (14), ground based IR and radio observation will line_2: be made in parallel with the HST observations. The Workshop "Variable Phenomena line_3: in Jovian Systems" held in Annapolis (22-26 July 1992) has adopted, on behalf of line_4: the International Jupiter Watch, a recommendation to encourage and facilitate line_5: the correlated multiwavelength observations of the Jovian aurorae. This will line_6: make the simultaneity of the HST observations with ground-based IR observations line_7: easier to schedule. However, a problems remains, due to the fact that IR line_8: observations are only possible at night. To increase the temporal coverage of line_9: the IR observations and get a good overlap with the HST observing sequences line_10: (about 13 hours each), observatories located at different longitudes must be line_11: involved in the program. This can be reached using the Hawaii telescopes CFHT, line_12: UKIRT and IRTF, with which G.E. Ballester and R. Prange have already line_13: collaborated (P. Drossart, T. Kostiuk, S. Miller, among others, are willing line_14: to collaborate on this new program on the various Hawaii instruments) and the line_15: Pic du Midi Observatory (France) where R. Prange has already been observing, line_16: and which will be equipped with a new near-IR camera at the time of the Cycle 3 line_17: observations. line_19: For the radio observations, the problem of correlated observations is much less line_20: critical, since several radio-observatories make routine observations of the DAM line_21: Jovian emissions. In order to get a 24 hours coverage, data from various line_22: observatories will be used. R. Prange can have access to the French Nancay DAM line_23: array database (in collaboration with Y. Leblanc, A. Lecacheux, P. Zarka), and ! question: 8 section: 2 line_1: has developed collaborations with the observatory of the University of Florida line_2: (T. Carr). H. Waite will have access to US and Japanese data. ! question: 9 section: 1 line_1: 1. GTO program 1269, Far UV imaging of the Giant Planets (F. Paresce, PI; line_2: J.C. Gerard, Co-I) is partly related to this project. GTO results on the line_3: mapping of the jovian Ly-alpha and H2 aurora will be used as a basis on which line_4: this program and its physical analysis will be built. However, the GTO line_5: observations are widespread in time and will NOT provide the time coverage line_6: needed to analyze time variations. It does not either provide the multispectral line_7: data. UV and visible images of Io's surface were also obtained in this program. line_9: 2. Discretionary time (ID 4005),"HST UV Imaging of Jupiter to Support the line_10: Interpretation of Ulysses X-Ray Measurements" line_11: was provided during the ULYSSES spacecraft encounter with Jupiter (Stern, PI; line_12: Waite, Co-I) to image the H2 aurora in the Werner bands and for comparison with line_13: in-situ particle and field measurements. line_15: 3. GTO/FOC 1253, High Resolution Observations of Cataclysmic Variables (F. line_16: Paresce, PI); Not Related line_18: 4. GO 3511, H Ly alpha dayglow emission line profiles for the outer planets, J. line_19: Clarke, PI; R. Prange, L. Benjaffel, Co-Is); Not Related line_21: 5. GO 2627, Io's atmosphere and its interaction with the plasma torus (H.W. line_22: Moos, PI, G. Ballester, Co-I); Not Related ! question: 9 section: 2 line_1: 1. Cycle 0 GTO 1269 images were taken in 1991 and 1992. Io was observed line_2: through several combinations of filters from F120M to F220M. These images line_3: show SO2 frost patches on the surface of Io and are currently beeing compared line_4: with Voyager images taken 12 years ago. Extended deconvolution has been applied line_5: to these images, which should be very useful for the image processing of the line_6: Jovian aurora images. line_7: 2. Auroral images obtained during GTO cycle 1 (1992) provided the first UV line_8: picture of the northern polar jovian aurora. Two Lyman-alpha images of the line_9: north polar region of Jupiter were obtained with the FOC in February 1992. The line_10: presence of high latitude regions of enhanced emission was clearly observed. A line_11: comparison with the location of the Voyager UVS oval, the Io (L = 6) and line_12: high-latitude field-lines footprints showed that a better agreement is obtained line_13: with the L > 15 footprint in the sector (30 deg. < lambdaIII < 210 deg.) These line_14: two families of L-shells correspond to two possible sources of precipitation: line_15: particles originating respectively from the plasma torus of Io or particles from line_16: the distant magnetosphere in a distorted magnetic field by analogy with the line_17: terrestrial aurora. These observations provided evidence that monitoring of the line_18: UV jovian aurora, its morphology and intensity variations can be performed from line_19: Earth orbit with the Hubble Space Telecope. line_20: The initial results indicate that the main auroral process is probably not line_21: located at the footprint of the theoretical Io footprint, in contrast to the line_22: view widely accepted so far. They suggest that the emission could take place on line_23: high latitude field lines and that the stucture of the brightest features is ! question: 9 section: 3 line_1: patchy, exhibiting large longitudinal inhomogeneities. line_3: An excellent set of H2 images, presently being analyzed, was also obtained in line_4: June 1992 at 160 nm (Paresce et al.) and, with a lower S/N, at 130 nm (Stern et line_5: al.). These images confirm the result indicated before: the auroral oval lies line_6: on the footprint of distant magnetic field lines originating from the middle line_7: and/or outer magnetosphere of Jupiter. line_9: 3. GO 3511: first observations will be made after cycle 3 submission deadline line_11: Io surface ultraviolet imaging with the HST Near UV imaging of Jupiter's line_12: satellite Io with HST, Astron. Astrophys, 1992, in press. line_14: Far ultraviolet imaging of the jovian aurora with the Hubble Space Telescope V. line_15: Dols, J.C. Gerard, F. Paresce, R. Prange and A. Vidal-Madjar, Geophys. Res. line_16: Lett., 1992, in press. line_18: Solar system observations with HST, F. Paresce and J.C. Gerard, in Proceedings line_19: of the International Space Year Conference Munich, 1992, in press. line_21: Far ultraviolet imaging of Jupiter's northern polar regions with the FOC J.C. line_22: Gerard, V. Dols, F. Paresce, R. Prange and A. Vidal-Madjar, Proceedings of line_23: the HST Workshop, Sardinia, 1992, in press. ! question: 9 section: 4 line_1: High resolution near UV observation of Jupiter's satellite Io with the HST, F. line_2: Paresce, P. Sartoretti, V. Dols, J.C. Gerard and M. McGrath, Proceedings of line_3: the HST Workshop, Sardinia, 1992, in press. line_5: First Results from the FOC: Imaging the Core of R Aqr, F. Paresce et al.,Ap. line_6: J. Lett., 369, L67, 1991 line_8: The Structure of the Inner Arcsecond of R Aqr observed with HST, D.Burgarella line_9: and F.Paresce, Ap. J. Lett., 389, L29, 1992 line_11: Blue Stragglers in the Core of the Globular Cluster 47 Tuc, F.Paresce et al., line_12: Nature, 232, 297, 1991 line_14: High resolution near UV observation of Jupiter's satellite Io with the Hubble line_15: Space Telescope, V. Dols, J.C. Gerard, P. Sartoretti, H.-M. Adorf and F. line_16: Paresce, Abstract of a paper presented at the EGS General Assembly, Edinburgh, line_17: Ann. Geophys. Suppl., 10, C498, 1992. line_19: First Ly-alpha images of the jovian aurora with the HST, J.C. Gerard et al., line_20: presented at the EGS General Assembly, Edingburgh, April 1992. line_22: Multispectral Observations of Jovian Aurora, H. Waite et al., paper presented line_23: at the UCLA conference, June 22-26 and at the Variable Phenomena in Jovian ! question: 9 section: 5 line_1: Planetary Systems, Annapolis July 13-16. line_3: Analysis of the first image of the the jovian aurora at Lyman alpha obtained line_4: with the HST, R. Prange, V. Dols, J.C. Gerard and F. Paresce, paper line_5: presented at the conference "Variable phenomena in jovian planetary systems", line_6: Annapolis, July 13-16. line_8: Observations of the H and H2 ultraviolet aurora with the HST Faint Object Camera line_9: , J.C. Gerard, V. Dols, F. Paresce and R. Prange, abstract, 1992 DPS line_10: meeting, Munich, 1992, in press. ! question: 10 section: 1 line_1: -workstations are available in several institutions for data reduction, line_2: fitting and comparison with models line_3: -university computer time is available in all institutions for numerical line_4: modeling and comparison with data line_5: -1 full time research assistant in atmospheric physics (PRODEX program) line_6: funded by the Belgian Government for HST data analysis line_7: -1 graduate student in plasma physics (France) line_8: -Funds are available for this project through various scientific line_9: agencies: SPPS(B), CNRS(F), NASA and ESA. Financial support is requested by line_10: the US Co-I (see budget in annex). ! !end of general form text general_form_address: lname: GERARD fname: JEAN-CLAUDE mi: M title: PROF category: PI inst: INSTITUT D ASTROPHYSIQUE addr_1: 5, AVENUE DE COINTE city: LIEGE zip: 4000 country: BELGIUM phone: 32-41-529980 from_date: 01-JAN-93 to_date: 01-JAN-93 ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: JUPITER-OFF descr_1: FEATURE JUPITER lev1_1: STD=JUPITER lev2_1: TYPE=POS_ANGLE,RAD=65,ANG=102, lev2_2: REF=NORTH comment_1: POSITION IS 63" V3 FROM DESIRED. ! targnum: 2 name_1: JUPITER-OFF1 descr_1: FEATURE JUPITER lev1_1: STD=JUPITER lev2_1: TYPE=POS_ANGLE,RAD=65,ANG=102, lev2_2: REF=NORTH wind_1: CML OF JUPITER FROM EARTH BETWEEN wind_2: 120 140 comment_1: THIS PROGRAM SHOULD PREFERABLY MADE comment_2: IN JUNE 1993 WHICH IS CLOSE TO comment_3: QUADRATURE AND WITHIN THE WINDOW OF comment_4: PLANNED COORDINATED CAMPAIGN WITH IUE. comment_5: POSITION IS 63" V3 FROM DESIRED. comment_6: CML NEAR 127D AT THE comment_7: BEGINNING OF EXPOSURE ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 9.000 targname: DARK config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W,F6ND num_exp: 1 time_per_exp: 17S priority: 1 param_1: PIXEL= 50X25 req_1: SEQ 9-12 NO GAP; req_2: SEQ 9-10 NON-INT; req_3: CYCLE 3; comment_1: TEST EXPOSURE FOR comment_2: LINE 10. PERFORM SIP comment_3: ONLY IF FILTERS ARE IN comment_4: PLACE. comment_5: THE WHOLE PROGRAM SHOULD BE PREFERABLY comment_6: SCHEDULED WITHIN CYCLE2 ! linenum: 10.000 targname: JUPITER-OFF config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W,F6ND num_exp: 1 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: CYCLE 3/9-42; req_3: REQ UPLINK; comment_1: PUT CONT. OBS. IN ORBIT comment_2: BEFORE AURORAL OBS. ! linenum: 10.500 targname: DARK config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M,F175W num_exp: 1 time_per_exp: 17S priority: 1 param_1: PIXEL= 50X25 req_1: SEQ 10.5-11 NON-INT; comment_1: TEST EXPOSURE FOR comment_2: LINE 11. PERFORM SIP comment_3: ONLY IF FILTERS ARE IN comment_4: PLACE. ! linenum: 11.000 targname: JUPITER-OFF1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M,F175W num_exp: 1 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: REQ UPLINK; comment_1: THIS IMAGE DEFINES THE TIMING comment_2: OF THE WHOLE PROGRAM ! linenum: 12.000 targname: JUPITER-OFF config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M,F175W num_exp: 2 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: NON-INT; comment_1: SET OF 2 CONSECUTIVE IMAGES DURING comment_2: THE SAME HST UNOCCULTED ORBIT comment_3: FIRST IMAGE TAKEN 1 HST ORBIT AFTER comment_4: BEGINNING OF JUPVAR11 ! linenum: 19.000 targname: DARK config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W,F6ND num_exp: 1 time_per_exp: 17S priority: 1 param_1: PIXEL= 50X25 req_1: SEQ 19-22 NO GAP; req_2: SEQ 19-20 NON-INT; comment_1: TEST EXPOSURE FOR comment_2: LINE 20. PERFORM SIP comment_3: ONLY IF FILTERS ARE IN comment_4: PLACE. ! linenum: 20.000 targname: JUPITER-OFF config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W,F6ND num_exp: 1 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_2: REQ UPLINK; comment_1: IMAGE TAKEN 1 HST ORBIT comment_2: BEFORE 1ST LY A IMAGE ! linenum: 20.500 targname: DARK config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F120M,F140W num_exp: 1 time_per_exp: 17S priority: 1 param_1: PIXEL= 50X25 req_1: SEQ 20.5-21 NON-INT; comment_1: TEST EXPOSURE FOR comment_2: LINE 21. PERFORM SIP comment_3: ONLY IF FILTERS ARE IN comment_4: PLACE. ! linenum: 21.000 targname: JUPITER-OFF1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F120M,F140W num_exp: 1 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_2: AFTER 11 BY 596M +/- 30M; req_3: REQ UPLINK; comment_1: IMAGE TAKEN 1 JOVIAN ROTATION comment_2: AFTER 1ST H2 LY EXPOSURE ! linenum: 22.000 targname: JUPITER-OFF config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F120M,F140W num_exp: 2 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: NON-INT; comment_1: SET OF 2 CONSECUTIVE IMAGES DURING comment_2: THE SAME UNOCCULTED ORBIT comment_3: FIRST IMAGE TAKEN 1 HST ORBIT comment_4: AFTER BEGINNING OF JUPVAR21 comment_5: EXPOSURE ! linenum: 30.500 targname: DARK config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M,F175W num_exp: 1 time_per_exp: 17S priority: 1 param_1: PIXEL= 50X25 req_1: SEQ 30.5-31 NON-INT; req_2: SEQ 30.5-32 NO GAP; comment_1: TEST EXPOSURE FOR comment_2: LINE 31. PERFORM SIP comment_3: ONLY IF FILTERS ARE IN comment_4: PLACE. ! linenum: 31.000 targname: JUPITER-OFF1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M,F175W num_exp: 1 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: REQ UPLINK; req_2: NON-INT; req_3: AFTER 21 BY 596M +/- 30M; comment_1: IMAGE TAKEN JOVIAN ROTATION comment_2: AFTER 1ST LY A IMAGE comment_3: SHOULD OBEY CML WINDOWS ! linenum: 32.000 targname: JUPITER-OFF config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M,F175W num_exp: 2 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: NON-INT; comment_1: SET OF 2 CONSECUTIVE IMAGES DURING comment_2: THE SAME HST UNOCCULTED ORBIT comment_3: FIRST IMAGE TAKEN 1 HST ORBIT AFTER comment_4: BEGINNING OF LINE 31 ! linenum: 40.500 targname: DARK config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F130M,F140W num_exp: 1 time_per_exp: 17S priority: 1 param_1: PIXEL= 50X25 req_1: SEQ 40.5-41 NON-INT; req_2: SEQ 40.5-42 NO GAP; comment_1: TEST EXPOSURE FOR comment_2: LINE 41. PERFORM SIP comment_3: ONLY IF FILTERS ARE IN comment_4: PLACE. ! linenum: 41.000 targname: JUPITER-OFF1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F130M,F140W num_exp: 1 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: REQ UPLINK; req_2: AFTER 31 BY 596M +/- 30M; comment_1: IMAGE TAKEN 1 JOVIAN ROTATION comment_2: AFTER 1ST H2 LYA IMAGE OF 2ND comment_3: GROUP (I.E. LINE 31) ! linenum: 42.000 targname: JUPITER-OFF config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F130M,F140W num_exp: 2 time_per_exp: 900S priority: 1 param_1: PIXEL= 50X25 req_1: NON-INT; comment_1: SET OF 2 CONSECUTIVE IMAGES DURING comment_2: THE SAME HST UNOCCULTED ORBIT comment_3: FIRST IMAGE TAKEN 1 HST ORBIT AFTER comment_4: BEGINNING OF JUPVAR41 ! ! end of exposure logsheet ! No scan data records found