!  File:  1203C.PROP
!  Database:  PEPDB
!  Date:  16-FEB-1994:05:51:16

coverpage:

  title_1:         JOVIAN AURORAL LY-ALPHA PROFILE-CYCLE 3
    sci_cat:       SOLAR SYSTEM
    sci_subcat:    GIANT PLANETS
    proposal_for:  GTO/HRS
    cont_id:       1203
    pi_fname:      LAURENCE
    pi_mi:         M.
    pi_lname:      TRAFTON
    pi_inst:       TEXAS, UNIVERSITY OF
    pi_country:    USA
    pi_phone:      (512)471-1476
    keywords_1:    LY-ALPHA, AURORA, MAGNETOSPHERE, DEUTERIUM
    hours_par:     3.50
    num_par:       1
    hrs:           X
    pi_position:   RESEARCH SCIENTIST
! end of coverpage

abstract:

    line_1:        Observe the Ly-alpha profile for a bright auroral emission on Jupiter to study
    line_2:        excitation processes, proton precipitation along field lines, excitation
    line_3:        particle flux, and atmospheric properties. A determination of the D/H ratio
    line_4:        may result if the signal to noise is high enough.

!
! end of abstract

general_form_proposers:

  lname:           TRAFTON
    fname:         LAURENCE
    mi:            M.
    inst:          TEXAS, UNIVERSITY OF
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        Use FOC with Ly-alpha filter to locate brightest auroral emission in Jupiter's
    line_2:        north polar region when the foot of the Io flux tube is "visible" (i.e. Io
    line_3:        orbital phase angle between 135degrees - 225degrees) and central meridian is
    line_4:        lambdaIII (1965) = 160degrees - 220degrees. Point HRS aperture to brightest
    line_5:        location and track it (Jupiter is rotating) for exposure.
    line_8:        Observe +/- 1 month of pre-opposition quadrature to maximize wavelength
    line_9:        separation of H and D geocoronal and Jovian Ly-alpha emissions.
    line_11:       Obtain geocoronal calibration observation
    line_12:       with similar geocoronal - Sun - planet geometry, in parallel mode.

!

  question:        4
    section:       1
    line_1:        1216A required
    line_2:        spatial resolution required

!

  question:        5
    section:       1
    line_1:        The auroral emission of Jupiter is spatially isolated at several areas near the
    line_2:        poles but the precise location and extent are not known. It is believed that
    line_3:        the foot of the Io flux tube may be a hot spot for auroral emission. We need to
    line_4:        precisely locate the brightest emission using the FOC before observing it with
    line_5:        the HRS. Need maximum short-wavelength Doppler separation from geocoronal
    line_6:        Ly-alpha emission to minimize blending of H and D absorptions with
    line_7:        geocoronal H emission.

!

  question:        6
    section:       1
    line_1:        Darktime to reduce background Ly-alpha emission from geocorona.
    line_3:        Geocoronal spectrum needed to remove blended Ly-alpha background emission.
    line_5:        FOC image needed for locating auroral hot spots.

!

  question:        7
    section:       1
    line_1:        Preliminary reductions of STScI
    line_3:        Final reductions and analysis at U. TX using VAX 11/780 cluster

!

  question:        8
    section:       1
    line_1:        Request geocoronal observations to be parallel at no charge

!

  question:        10
    section:       1
    line_1:        VAX 11/780
    line_2:        Sun Sparcstation
    line_3:        R.A.'s

!

  question:        13
    section:       1
    line_1:        We will use the intermediate/high resolution modes of HRS to measure the
    line_2:        LY-alpha profile for the strong Jovian auroral emission from H2, H and D.

!
!end of general form text

general_form_address:

  lname:           TRAFTON
    fname:         LAURENCE
    mi:            M.
    category:      PI
    inst:          UNIVERSITY OF TEXAS AT AUSTIN
    addr_1:        RLM 16.326
    city:          AUSTIN
    state:         TX
    zip:           78712
    country:       USA
    phone:         (512)471-1476

!
! end of general_form_address records

! No fixed target records found

! No solar system records found

generic_targets:

  targnum_1:       1
    name_1:        GEOCORONA-1
    descr_1:       NIGHT GEOCORONAL LY-ALPHA PROFILE
    descr_2:       NEAR ECLIPTIC PLANE.
    criteria_1:    ABS_BETA < 30D
    comment_1:     NEED FOR INSTRUMENTAL PROFILE
    comment_2:     OF HRS TO SUBTRACT BACKGROUND
    comment_3:     LY-ALPHA FROM PLANETARY
    comment_4:     LY-ALPHA EMISSION. [THE ABS CALIB
    comment_5:     WILL BE DONE DURING COORD.
    comment_6:     PARALLEL HRS+FOS OBSERVATIONS].
    fluxnum_1:     1
    fluxval_1:     SURF(1216)=1.6E-6
    fluxnum_2:     2
    fluxval_2:     W-LINE(1216)=0.01

!
! end of generic targets

exposure_logsheet:

    linenum:       1.000
    targname:      GEOCORONA-1
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    num_exp:       1
    time_per_exp:  30M
    fluxnum_1:     1
    fluxnum_2:     2
    priority:      1
    param_1:       STEP-TIME=1.0
    req_1:         PAR;
    req_2:         DARK TIME;
    req_3:         CYCLE 3 / 1-2
    comment_1:     ALL PARALLEL GEOCORONA OBSERVATIONS
    comment_2:     REQUIRE LINE-OF-SIGHT DOPPLER
    comment_3:     CORRECTION FOR HST'S MOTION
    comment_4:     CALIBRATION FOR LINE 2 OF 1203AUG.

!

    linenum:       2.000
    targname:      GEOCORONA-1
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    num_exp:       1
    time_per_exp:  180M
    fluxnum_1:     1
    fluxnum_2:     2
    priority:      1
    param_1:       STEP-TIME=1.0
    req_1:         PAR;
    req_2:         DARK TIME
    comment_1:     OK TO COLLECT DATA IN SEGMENTS
    comment_2:     FROM DIFFERENT PRIME OBSERVATIONS.
    comment_3:     CALIBRATION FOR LINE 4 OF 1203AUG.

!
! end of exposure logsheet

! No scan data records found