!   $Id: 5347,v 5.1 1994/08/01 17:49:00 pepsa Exp $

coverpage:

  title_1:         ROTATION RATES OF WHITE DWARFS AND BOUNDARY LAYERS
    title_2:       IN CATACLYSMIC VARIABLES: CYCLE4 MEDIUM
    sci_cat:       HOT STARS
    sci_subcat:    ERUPTIVE BINARIES
    proposal_for:  GO
    pi_fname:      JANET
    pi_mi:         H
    pi_lname:      WOOD
    pi_inst:       UNIVERSITY OF KEELE
    pi_country:    UK
    pi_phone:      011-44-782-583341
    hours_pri:     5.00
    num_pri:       2
    hrs:           Y
    off_fname:     WATSON
    off_lname:     FULLER
    off_title:     DEPARTMENT HEAD
    off_inst:      8030
    off_addr_1:    DEPARTMENT OF PHYSICS
    off_addr_2:    KEELE UNIVERSITY
    off_city:      KEELE
    off_country:   UK
    off_phone:     011-44-782-583326
! end of coverpage

abstract:

    line_1:        A long standing problem in cataclysmic variables has been the lack
    line_2:        of observed flux from boundary layers in non-magnetic systems. This
    line_3:        is frequently explained as due to the rapid rotation of the white dwarf.
    line_4:        Accretion of only 0.1 solar masses is enough to spin up a white dwarf
    line_5:        almost to its breakup velocity. It then reaches an equilibrium rotation
    line_6:        rate where mass is accreted but does not add angular momentum to the
    line_7:        white dwarf. However, no observational confirmation of such rapid
    line_8:        rotation rates has yet been obtained. We propose to observe white
    line_9:        dwarf photospheric lines in the UV and use model atmospheres to
    line_10:       determine the rotational broadening. If we find that rapidly
    line_11:       rotating white dwarfs are present this explanation for the lack
    line_12:       of flux from boundary layers is very likely to be true.
    line_13:       We will observe 2 dwarf novae with HRS and G160M covering 1382-1415
    line_14:       Angstroms. We chose as our targets the brightest (in the UV) dwarf
    line_15:       novae which are not eclipsing, have infrequent outbursts,
    line_16:       and for which there is evidence of the presence of Si IV 1393, 1402
    line_17:       absorption in IUE spectra. As a bonus of these observations we will
    line_18:       make the first ever radial velocity measurements directly from the
    line_19:       white dwarfs in cataclysmic variables.

!
! end of abstract

general_form_proposers:

  lname:           WOOD
    fname:         JANET
    title:         PI
    mi:            H
    inst:          8030
    country:       UK
    esa:           Y

!

  lname:           MARSH
    fname:         THOMAS
    inst:          8058
    country:       UK
    esa:           Y

!

  lname:           ROBINSON
    fname:         EDWARD
    mi:            L
    inst:          3550
    country:       US

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        We will obtain high resolution spectroscopy of the dwarf novae
    line_2:        CM Del and AH Her with the HRS using the LSA. We will use the
    line_3:        G160M grating with central wavelength 1398.5 Angstroms to cover
    line_4:        a wavelength range from 1382 to 1415 Angstroms. This wavelength
    line_5:        range covers the Si IV resonance doublet at 1393, 1402 Angstroms.
    line_6:        These absorption lines are produced in the white dwarfs'
    line_7:        photospheres. We will use RAPID readout mode with integration
    line_8:        times of 12.75s. This will allow us to investigate any variability
    line_9:        in the objects and means we will not smear out the observed lines
    line_10:       due to the white dwarf's orbital motion. As a bonus this data
    line_11:       will also allow us to measure the radial velocity of each
    line_12:       white dwarf from the absorption line cores; the first time a
    line_13:       direct measurement has been made in a cataclysmic variable.
    line_15:       IUE observations of CM Del and AH Her have shown that they both have
    line_16:       flux densities of 3.2 x 10 ^-26 ergs/s/cm^2/Hz at 1400 Angstroms.
    line_17:       With the HRS and G160M grating we therefore expect count rates of
    line_18:       108 counts/diode in one hour from each object using the LSA.
    line_19:       The dark count rate is 28.8 counts/diode in one hour. The dispersion
    line_20:       of 0.07 Angstroms/diode will easily resolve the line
    line_21:       cores. If the white dwarfs are rotating rapidly we expect line
    line_22:       core widths of a few Angstroms. Thus, without rebinning with
    line_23:       a total integration time of 95mins on AH Her and 91.5mins on CM Del

!

  question:        3
    section:       2
    line_1:        we will obtain signal-to-noise ratios of 12 and 11, respectively.
    line_3:        The observations of each star can be obtained in one visit with
    line_4:        observations continuing between Earth occultations until the
    line_5:        required time on target has been reached. Our primary aim, to
    line_6:        measure v sini, is not affected by what part of the orbit is
    line_7:        observed. The orbital periods of CM Del and AH Her are 3.9hr
    line_8:        and 6.2hr respectively.

!

  question:        4
    section:       1
    line_1:        HST is essential as its large mirror and efficient instruments mean it
    line_2:        is the only telescope capable of making these high resolution UV
    line_3:        observations, and the only one capable of achieving a high signal-to-noise.
    line_4:        This project cannot be done using optical data because the accretion disc
    line_5:        dominates the light in the optical even in quiescent dwarf novae. In the
    line_6:        UV quiescent accretion discs are very faint and the white dwarf's spectrum
    line_7:        can be observed.

!

  question:        5
    section:       1
    line_1:

!

  question:        6
    section:       1
    line_1:

!


!

  question:        8
    section:       1
    line_1:

!

  question:        9
    section:       1
    line_1:        Program GO-3836  "Spectroscopic Observations of the Exposed White Dwarfs
    line_2:        in the Dwarf Novae WZ Sagittae, U Geminorum and VW Hydri"
    line_3:        Sion, Szkody, Gilliland, Long, Pringle, Horne, Wood
    line_5:        This program is related to the current proposal.
    line_7:        Program GO-2380 "Instabilities in Accretion Disks and the Outbursts of
    line_8:        Dwarf Novae": Horne and Marsh.
    line_9:        Program GO-3683 "Accretion Disk Mapping in Cataclysmic Variables" Horne
    line_10:       et al.
    line_11:       Program GO-3600 "Oscillations, Flaring and Tomography of AE Aquarii":
    line_12:       Horne, Marsh, Robinson, Wood.
    line_13:       Program GO-3824 "A Search for Silicon and Carbon in GP Com":
    line_14:       Wood, Marsh, Lambert, Horne.
    line_15:       Program GO-3578  "Line Eclipse mapping of an Accretion Disk Wind"
    line_16:       Mason, Drew, Cordova, Mauche, Horne, Marsh
    line_17:       Program GO-4271  "Testing the Star-Disk Connection:
    line_18:       CIV and MGII Maps of Accretion Disks"
    line_19:       Horne, Marsh, Rutten, Saar
    line_21:       GTO time on the HSP for several projects. Bless, Dolan,
    line_22:       Elliot, Robinson, van Citters.

!

  question:        9
    section:       2
    line_1:        "HST Observations of the Dwarf Nova Z Cha through its Outburst Cycle"
    line_2:        Wood, Robinson, Dolan, Elliot, van Citters in "Annals of the Israel
    line_3:        Physical Society", Vol 10, ed. Regev, Shaviv, p19 (1993).
    line_5:        "HST Observations of the Eclipsing Dwarf Nova OY Carinae" Marsh in
    line_6:        Annals of the Israel Physical Society", Vol 10, ed. Regev, Shaviv, p7,
    line_7:        (1993).
    line_9:        "HST HRS Spectroscopy of U Gem in Quiescence: Rotation Rate of White
    line_10:       Dwarf" Sion, Huang, Long, Szkody, Horne 1993, BAAS, 25,909.
    line_12:       "HST High Speed Photometer Observations of the Crab Pulsar",
    line_13:       Biggs, Percival, Bless, Dolan, Elliot, Nelson, Robinson, Taylor,
    line_14:       van Citters, in Physics of Isolated Pulsars, ed. Riper, Epstein
    line_15:       and Ho, CUP, 1993, in press.
    line_17:       "The Crab Pulsar in the Visible and UV with 10microsec Time Resolution"
    line_18:       Percival, Biggs, Dolan, Robinson, Taylor, Bless, Elliot, Nelson,
    line_19:       Ramseyer, van Citters, Zhang, Ap.J., 407, 276. 1993.
    line_21:       "High Speed UV Photometry of HD 60435", Taylor, Nelson, Bless, Dolan,
    line_22:       Elliot, Percival, Robinson, van Citters, Ap.J. Lett. submitted, 1993.

!

  question:        10
    section:       1
    line_1:        Data analysis will be done using the STARLINK computing
    line_2:        facilities at Keele
    line_3:        and Oxford and on a Sparcstation II at the University
    line_4:        of Texas. The University
    line_5:        of Texas will provide facilities for a student.

!
!end of general form text

general_form_address:

  lname:           WOOD
    fname:         JANET
    mi:            H
    category:      PI
    inst:          8030
    addr_1:        DEPARTMENT OF PHYSICS
    addr_2:        KEELE UNIVERSITY
    city:          KEELE
    country:       UK
    phone:         011-44-782-583341
    telex:         36113 UNKLIB G/JHW%UK.AC.KEELE.PH.STARLINK@NSS.CS.UCL.AC.UK

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        CM-DEL
    descr_1:       A,149,161,906
    pos_1:         PLATE-ID = 02UR,
    pos_2:         RA = 20H 24M 56.92S +/- 0.07S,
    pos_3:         DEC = +17D 17' 54.52" +/- 1.0"
    equinox:       2000.0
    comment_1:     ALL FLUXES ARE FOR QUIESCENCE.
    comment_2:     IN OUTBURST BRIGHTENS BY 2-3
    comment_3:     MAGNITUDES BUT ITS UNLIKELY TO
    comment_4:     BE IN OUTBURST.
    fluxnum_1:     1
    fluxval_1:     V=15.3+/-0.1
    fluxnum_2:     1
    fluxval_2:     B-V=0.10+/-0.01
    fluxnum_3:     2
    fluxval_3:     E(B-V)=0.08+/-0.01
    fluxnum_4:     3
    fluxval_4:     F-CONT(1400)=49+/-3E-15

!

    targnum:       2
    name_1:        AH-HER
    name_2:        GSC2049.01115
    descr_1:       A,149,161,906
    pos_1:         PLATE-ID = 02BA,
    pos_2:         RA = 16H 44M 09.99S +/- 0.07S,
    pos_3:         DEC = +25D 15' 01.9" +/- 0.8"
    equinox:       2000.0
    comment_1:     ALL FLUXES ARE FOR QUIESCENCE.
    comment_2:     IN OUTBURST BRIGHTENS BY 2-3
    comment_3:     MAGNITUDES BUT ITS UNLIKELY TO
    comment_4:     BE IN OUTBURST. COORDS FROM
    comment_5:     GUIDE STAR CATALOGUE.
    fluxnum_1:     1
    fluxval_1:     V=14.7+/-0.1
    fluxnum_2:     1
    fluxval_2:     B-V=0.10+/-0.01
    fluxnum_3:     2
    fluxval_3:     E(B-V)=0.03+/-0.01
    fluxnum_4:     3
    fluxval_4:     F-CONT(1400)=49+/-3E-15

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

  LINENUM:  1.0
  TARGNAME:CM-DEL
  CONFIG:HRS
  OPMODE:ACQ
  APERTURE:2.0
  SP_ELEMENT:MIRROR-N2
  WAVELENGTH:
  NUM_EXP:1
  TIME_PER_EXP:72S
  S_TO_N:
  S_TO_N_TIME:
  FLUXNUM_1:1
  PRIORITY:1
  REQ_1:CYCLE 4 / 1-3;
  REQ_2:ONBOARD ACQ FOR 2;
  REQ_3:GROUP 1-3 NO GAP;
  COMMENT_1:STEP-TIME=8S 1000 counts expected

!

  LINENUM:  2.0
  TARGNAME:CM-DEL
  CONFIG:HRS
  OPMODE:ACQ/PEAKUP
  APERTURE:2.0
  SP_ELEMENT:MIRROR-N2
  WAVELENGTH:
  NUM_EXP:1
  TIME_PER_EXP:714S
  S_TO_N:
  S_TO_N_TIME:
  FLUXNUM_1:1
  PRIORITY:1
  REQ_1:ONBOARD ACQ FOR 3
  COMMENT_1:STEP-TIME=7S

!

  LINENUM:  3.0
  TARGNAME:CM-DEL
  CONFIG:HRS
  OPMODE:ACCUM
  APERTURE:2.0
  SP_ELEMENT:G160M
  WAVELENGTH:1398.5
  NUM_EXP:12
  TIME_PER_EXP:410S
  S_TO_N:10
  S_TO_N_TIME:82M
  FLUXNUM_1:3
  PRIORITY:1

!

  LINENUM:  4.0
  TARGNAME:AH-HER
  CONFIG:HRS
  OPMODE:ACQ
  APERTURE:2.0
  SP_ELEMENT:MIRROR-N2
  WAVELENGTH:
  NUM_EXP:1
  TIME_PER_EXP:27S
  S_TO_N:
  S_TO_N_TIME:
  FLUXNUM_1:1
  PRIORITY:1
  REQ_1:CYCLE 4 / 4-6;
  REQ_2:ONBOARD ACQ FOR 5;
  REQ_3:GROUP 4-6 NO GAP;
  COMMENT_1:STEP-TIME=3S 1000 COUNTS EXPECTED

!

  LINENUM:  5.0
  TARGNAME:AH-HER
  CONFIG:HRS
  OPMODE:ACQ/PEAKUP
  APERTURE:2.0
  SP_ELEMENT:MIRROR-N2
  WAVELENGTH:
  NUM_EXP:1
  TIME_PER_EXP:306S
  S_TO_N:
  S_TO_N_TIME:
  FLUXNUM_1:1
  PRIORITY:1
  REQ_1:ONBOARD ACQ FOR 6
  COMMENT_1:STEP-TIME=3S

!

  LINENUM:  6.0
  TARGNAME:AH-HER
  CONFIG:HRS
  OPMODE:ACCUM
  APERTURE:2.0
  SP_ELEMENT:G160M
  WAVELENGTH:1398.5
  NUM_EXP:12
  TIME_PER_EXP:414S
  S_TO_N:11
  S_TO_N_TIME:82.8M
  FLUXNUM_1:3
  PRIORITY:1

!
! end of exposure logsheet

! No scan data records found