!  File:  3948C.PROP
!  Database:  PEPDB
!  Date:  20-FEB-1994:01:14:08

coverpage:

  title_1:         DOPPLER IMAGING OF THE CHROMOSPHERES AND TRANSITION REGIONS
    title_2:       OF COOL STARS: AB DORADUS.  LATER CYCLE CONTINUATION
    sci_cat:       STELLAR ASTROPHYSICS
    sci_subcat:    COOL STARS
    proposal_for:  GTO/HRS
    cont_id:       1208
    pi_fname:      FREDERICK
    pi_mi:         M.
    pi_lname:      WALTER
    pi_inst:       STATE UNIVERSITY OF NEW YORK AT STONY BROOK
    pi_country:    USA
    pi_phone:      (516)632-8232
    keywords_1:    STELLAR CHROMOSPHERES, STELLAR TRANSITION REGIONS,
    keywords_2:    DOPPLER IMAGING, STELLAR ACTIVITY
    hours_pri:     14.46
    num_pri:       1
    pi_position:   ASSISTANT PROFESSOR
! end of coverpage

abstract:

    line_1:        AB Dor (HD 36705) is one the most active single early K
    line_2:        dwarfs known. It is very rapidly-rotating with a period of
    line_3:        0.514 days and vsini=100 km/s. It has been suggested that
    line_4:        AB Dor is still contracting to the main sequence, on the
    line_5:        basis of a strong Li I absorption line and Pleiades space
    line_6:        motions. The phenomena exhibited by this star include
    line_7:        flares, a large starspot, saturated emission line fluxes,
    line_8:        bright nonthermal radio emission, and a co-rotating disk
    line_9:        (or ring) located at two stellar radii that is identified
    line_10:       from H-alpha emission. We propose to monitor AB Dor, which
    line_11:       is in the continuous viewing zone, continuously for one
    line_12:       rotation period to produce Doppler images of the lower
    line_13:       chromosphere and the transition region in the light of
    line_14:       Mg II, C IV, Si IV, O IV, C II, N V, Si III], and C III],
    line_15:       with phase resolution of 0.05 at Mg II and 0.08 in the
    line_16:       transition region. We will use these data to produce a 3-D
    line_17:       model of the outer atmosphere of this star, using the
    line_18:       density-sensitive line ratios and the measured emission line
    line_19:       fluxes to infer the total nonradiative heating rate. We will
    line_20:       obtain coordinated x-ray, radio, and optical observations.

!
! end of abstract

general_form_proposers:

  lname:           BRANDT
    fname:         JOHN
    inst:          COLORADO, UNIVERSITY OF
    country:       USA

!

  lname:           BROWN
    fname:         ALEXANDER
    inst:          COLORADO, UNIVERSITY OF
    country:       USA

!

  lname:           CARPENTER
    fname:         KEN
    inst:          GODDARD SPACE FLIGHT CENTER
    country:       USA

!

  lname:           DUNCAN
    fname:         DOUGLAS
    inst:          STSCI
    country:       USA

!

  lname:           LINSKY
    fname:         JEFFREY
    mi:            L.
    inst:          COLORADO, UNIVERSITY OF
    country:       USA

!

  lname:           WALTER
    fname:         FREDERICK
    mi:            M
    inst:          SUNY-STONY BROOK
    country:       USA

!

  lname:           VILHU
    fname:         OSMI
    inst:          HELSINKI, UNIVERSITY OF
    country:       FINLAND

!
! end of general_form_proposers block

general_form_text:

  question:        2
    section:       1
    line_1:        Because most stars have very small apparent angular diameters, it is
    line_2:        difficult to resolve them spatially. Consequently, line surface fluxes are
    line_3:        necessarily an average over the entire visible hemisphere of the star.
    line_4:        From our knowledge of the solar surface, we know that such averages are
    line_5:        not only misleading, but that they convey little physical information.
    line_6:        Nonetheless, most stellar model atmospheres are based on such data.
    line_7:        What is needed to generate realistic model atmospheres are filling factors
    line_8:        of the plage regions, and densities in the active and quiet regions. The
    line_9:        technique of Doppler imaging can be used to map regions of contrasting
    line_10:       surface flux in a rotating star. Such information directly yields estimates
    line_11:       of the plage filling factors. Using these, the true surface fluxes and electron
    line_12:       densities of the various stellar surface structures can be measured.
    line_13:       This is a GHRS team project to map the chromosphere and transition
    line_14:       region of the rapidly rotating, active K dwarf AB Doradus (HD36705).
    line_15:       AB Dor rotates once every 12.5 hours. The projected equatorial rotational
    line_16:       velocity is 100 km/s. The star is known to have a very active chromosphere.,
    line_17:       with bright plages and dark spots. Our goal is to observe this star
    line_18:       continuously for one rotation period, mapping out the structure of
    line_19:       the lower chromosphere in the light of Mg II with a phase resolution
    line_20:       of 0.05, and mapping out the structure of the transition region in
    line_21:       the light of N V, C IV, Si IV, O IV, C II, C III], and Si III] with a
    line_22:       phase resolution of 0.08. Using 2 density sensitive line ratios, we will
    line_23:       be able to determine electron densities in the active regions directly.

!

  question:        3
    section:       1
    line_1:        AB Dor is in the continuous viewing zone. We will observe
    line_2:        during an uninterrupted window of 13.8 hours. During that
    line_3:        time we will cycle through observations with G160M, G200M,
    line_4:        and ECH-B. Medium resolution observations of the transition
    line_5:        region lines suffices to obtain about 12 resolution elements
    line_6:        over the rotationally broadened line profile.
    line_7:        All data will be obtained through the LSA.
    line_9:        We will observe the star for about 1.1 rotational cycles.
    line_10:       The overlap is necessary to begin to separate true
    line_11:       rotational modulation from secular variability.  This is
    line_12:       the bare minimum needed to provide some confidence in the
    line_13:       repeatability of the surface features: 2 full rotation would
    line_14:       be preferable, but are unfeasible on both operational and
    line_15:       time-requirement grounds.

!

  question:        4
    section:       1
    line_1:        Stellar transition regions can only be observed in the
    line_2:        ultraviolet.

!

  question:        5
    section:       1
    line_1:

!

  question:        6
    section:       1
    line_1:        This is a time critical observation. We require 13.77 hours
    line_2:        of uninterrupted time. The target is in the continuous
    line_3:        viewing zone, and this time can be scheduled between SAA
    line_4:        passages. We need uninterrupted coverage to study the
    line_5:        changes in line profile over the 12.5 hour stellar rotation
    line_6:        period. Earth occultations and reacquisitions would cut our
    line_7:        observing efficiency down to about 30%, which is unacceptable
    line_8:        for such a rapidly rotating star.
    line_9:        The length of the observation is dictated by the 12.5 hour
    line_10:       stellar rotation period. during that time we will obtain
    line_11:       about 0.05 phase resolution at Mg II, and somewhat lower
    line_12:       in the transition region lines.

!

  question:        7
    section:       1
    line_1:        We have developed extensive computer programs to analyze these spectra
    line_2:        using emission measure and model atmosphere techniques.
    line_3:        We know how to reduce GHRS spectra.

!

  question:        8
    section:       1
    line_1:        We need advance notice of the scheduling in order to arrange
    line_2:        for ground-based supporting photometry and spectroscopy. We
    line_3:        will request radio observations, and expect to
    line_4:        request contemporaneous ROSAT observations.

!

  question:        9
    section:       1
    line_1:        GTO programs 1208,1210. Data are being analyzed. The
    line_2:        preliminary analysis of the 1210 observations was presented
    line_3:        at the 7th Cambridge Cool Stars Workshop (October 1991);
    line_4:        premininary interpretation of the spectra from program 1208
    line_5:        were presented in February 1992 at the 10th International
    line_6:        Colloquium on X-Ray and Ultraviolet Observations of
    line_7:        Laboratory and Astrophysical Plasmas.

!

  question:        10
    section:       1
    line_1:        SUNY will supply an office and electricity. I have computing
    line_2:        capabilities here, and at GSFC.

!

  question:        13
    section:       1
    line_1:        We propose to study the dynamics of stellar transition regions by
    line_2:        measuring the redshifts, indicative of downflows, in lines of C III, Si III, C
    line_3:        IV, Si IV, and O IV. The energy balance and heating rates in stellar
    line_4:        chromospheres and transition regions will be derived from an emission measure
    line_5:        analysis of emission line fluxes and densities inferred from density sensitive
    line_6:        line ratio.

!
!end of general form text

general_form_address:

  lname:           WALTER
    fname:         FREDERICK
    mi:            M.
    category:      PI
    inst:          STATE UNIVERSITY OF NEW YORK
    addr_1:        DEPARTMENT OF EARTH AND SPACE SCIENCES
    city:          STONY BROOK
    state:         NY
    zip:           11794
    country:       USA
    phone:         516-632-8232

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        HD36705
    name_2:        AB-DORADUS
    descr_1:       G0 V STAR
    pos_1:         RA=05H28M35.821S+/-.01S,
    pos_2:         DEC=-65D29'18.77"+/-0.1"
    equinox:       1950
    pm_or_par:     Y
    pos_epoch_bj:  B
    pos_epoch_yr:  1950.00
    ra_pm_val:     0.003467
    ra_pm_unct:    0.000600
    dec_pm_val:    0.1330
    dec_pm_unct:   0.0090
    an_prlx_val:   0.0333
    rv_or_z:       V=0
    fluxnum_1:     1
    fluxval_1:     V=6.80

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    sequence_1:    DEFINE
    sequence_2:    ABDOR-DI
    targname:      #
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  163.2S
    fluxnum_1:     1
    priority:      #
    req_1:         ONBOARD ACQ FOR 2-6.1;
    comment_1:     STEP-TIME=1.6SEC
    comment_2:     CENTER IN LSA AFTER NEW DEFCAL

!

    linenum:       2.000
    sequence_1:    DEFINE
    sequence_2:    ABDOR-DI
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    ECH-B
    wavelength:    2798
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=2
    req_1:         CALIB FOR 2.1 NO SLEW;
    req_2:         SEQ 2.0-2.1 NON-INT;

!

    linenum:       2.100
    sequence_1:    DEFINE
    sequence_2:    ABDOR-DI
    targname:      #
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-B
    wavelength:    2798
    num_exp:       1
    time_per_exp:  272S
    priority:      #
    param_1:       STEP-PATT=5

!

    linenum:       3.100
    sequence_1:    DEFINE
    sequence_2:    ABDOR-DI
    targname:      #
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    wavelength:    1400
    num_exp:       4
    time_per_exp:  326.4S
    priority:      #
    param_1:       STEP-PATT=5

!

    linenum:       4.100
    sequence_1:    DEFINE
    sequence_2:    ABDOR-DI
    targname:      #
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-B
    wavelength:    2798
    num_exp:       1
    time_per_exp:  272S
    priority:      #
    param_1:       STEP-PATT=5

!

    linenum:       5.100
    sequence_1:    DEFINE
    sequence_2:    ABDOR-DI
    targname:      #
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    wavelength:    1550
    num_exp:       4
    time_per_exp:  326.4S
    priority:      1
    param_1:       STEP-PATT=5

!

    linenum:       6.100
    sequence_1:    DEFINE
    sequence_2:    ABDOR-DI
    targname:      #
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-B
    wavelength:    2798
    num_exp:       1
    time_per_exp:  272S
    priority:      #
    param_1:       STEP-PATT=5

!

    linenum:       20.000
    targname:      HD36705
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  1.8S
    priority:      1
    param_1:       SEARCH-SIZE=3
    param_2:       FAINT=1000
    param_3:       BRIGHT=RETURN
    req_1:         ONBOARD ACQ FOR 31;
    req_2:         CYCLE 9/ 20-38.1;
    req_3:         SEQ 20-38.1
    comment_1:     STEP TIME = 0.2 SEC

!

    linenum:       31.000
    sequence_1:    USE
    sequence_2:    ABDOR-DI
    targname:      HD36705
    priority:      1
    req_1:         SEQ 31-38.1 NON-INT
    comment_1:     THIS SEQUENCE REQUIRES 13.77 HOURS
    comment_2:     OF CONTINUOUS SPACECRAFT TIME.
    comment_3:     THIS OBSERVATION MUST BE SCHEDULED
    comment_4:     WHILE THE TARGET IS IN THE CVZ,
    comment_5:     AND CANNOT BE INTERRUPTED BY SAA
    comment_6:     PASSAGES. (CONTINUED LINE 31.100)

!

    linenum:       31.100
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    wavelength:    1240
    num_exp:       4
    time_per_exp:  326.4S
    priority:      1
    param_1:       STEP-PATT=5
    comment_1:     (CONTINUED FROM 31.000)
    comment_2:     TARGHET ACQUISITION (LINE 20) CAN
    comment_3:     BE SCHEDULED DURING SAA ORBITS.
    comment_4:     *PLEASE CONTACT THE PI IF 13.8 HOURS
    comment_5:     *OF CONTINUOUS VIEWING TIME CAN NOT
    comment_6:     *BE SCHEDULED IN CYCLE 9.

!

    linenum:       32.000
    sequence_1:    USE
    sequence_2:    ABDOR-DI
    targname:      HD36705
    priority:      1
    comment_1:     IT MAY BE NECESSARY TO UPDATE THE
    comment_2:     MEMORY DURING THIS OBSERVATION.
    comment_3:     I HAVE MADE NO PROVISION FOR
    comment_4:     BREAKING THE OBSERTVATION TO
    comment_5:     INCLUDE A SECOND TARGET ACQUISITION.

!

    linenum:       32.100
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    wavelength:    1335
    num_exp:       4
    time_per_exp:  326.4S
    priority:      1
    param_1:       STEP-PATT=5

!

    linenum:       33.000
    sequence_1:    USE
    sequence_2:    ABDOR-DI
    targname:      HD36705
    priority:      1

!

    linenum:       33.100
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G200M
    wavelength:    1900
    num_exp:       4
    time_per_exp:  326.4S
    priority:      1
    param_1:       STEP-PATT=5

!

    linenum:       34.000
    sequence_1:    USE
    sequence_2:    ABDOR-DI
    targname:      HD36705
    priority:      1

!

    linenum:       34.100
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    wavelength:    1240
    num_exp:       4
    time_per_exp:  326.4S
    priority:      1
    param_1:       STEP-PATT=5

!

    linenum:       35.000
    sequence_1:    USE
    sequence_2:    ABDOR-DI
    targname:      HD36705
    priority:      1

!

    linenum:       35.100
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    wavelength:    1335
    num_exp:       4
    time_per_exp:  326.4S
    priority:      1
    param_1:       STEP-PATT=5

!

    linenum:       36.000
    sequence_1:    USE
    sequence_2:    ABDOR-DI
    targname:      HD36705
    priority:      1

!

    linenum:       36.100
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G200M
    wavelength:    1900
    num_exp:       4
    time_per_exp:  326.4S
    priority:      1
    param_1:       STEP-PATT=5

!

    linenum:       37.100
    targname:      ^
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  163.2S
    fluxnum_1:     1
    priority:      ^
    req_1:         ONBOARD ACQ FOR 37.2;
    comment_1:     STEP-TIME=1.6SEC
    comment_2:     CENTER IN LSA AFTER NEW DEFCAL

!

    linenum:       37.200
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    ECH-B
    wavelength:    2798
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=2
    req_1:         CALIB FOR 37.3 NO SLEW;
    req_2:         SEQ 37.2-37.3 NON-INT;

!

    linenum:       37.300
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-B
    wavelength:    2798
    num_exp:       1
    time_per_exp:  272S
    priority:      ^
    param_1:       STEP-PATT=5

!

    linenum:       37.400
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G160M
    wavelength:    1400
    num_exp:       4
    time_per_exp:  326.4S
    priority:      ^
    param_1:       STEP-PATT=5

!

    linenum:       38.100
    targname:      HD36705
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-B
    wavelength:    2798
    num_exp:       1
    time_per_exp:  272S
    priority:      2
    param_1:       STEP-PATT=5

!
! end of exposure logsheet

! No scan data records found