! $Id: 5448,v 5.1 1994/07/27 18:07:00 pepsa Exp $ coverpage: title_1: SPECTRALLY RESOLVED MAPS OF OPTICALLY THICK ACCRETION DISKS: title_2: CYCLE4 HIGH sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO pi_fname: KNOX pi_mi: S. pi_lname: LONG pi_inst: 3470 pi_country: USA pi_phone: 410-338-4862 hours_pri: 5.04 num_pri: 1 fos: Y time_crit: Y off_fname: HERVEY S. off_lname: STOCKMAN off_title: DEPUTY DIRECTOR off_inst: 3470 off_addr_1: STSCI off_addr_2: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 410-338-4730 ! end of coverpage abstract: line_1: We will derive the structure of the steady state optically thick accretion disk line_2: in the novalike variable UX UMa by using the FOS in RAPID readout line_3: mode to monitor eclipses of its UV/optical spectra as the companion star line_4: progressively occults the accretion disk and the white dwarf. From the observed line_5: eclipse light curves at different wavelengths we will construct monochromatic line_6: maps of the disk and then extract the spectrum from any desired region of the line_7: disk surface, including annuli at different radii in the disk, the hot spot on line_8: the outer rim of the disk, and the white dwarf / boundary layer at the inner line_9: edge. Our maps from Earth-based optical spectroscopy are of sufficient quality line_10: to reveal not only changes in continuum intensity and slope but also Balmer line_11: lines transitioning from absorption in the inner disk to emission in the outer line_12: disk. Our HST experiment extends this analysis into the ultraviolet to pin down line_13: the hot parts of the disk. We will use our results to test our models of line_14: accretion disk atmospheres and chromospheres. By observing the spectrum at each line_15: radius rather than from the disk as a whole, the quality of the information is line_16: such that will constrain the radial dependences of the effective temperature, line_17: surface density, and microturbulent Mach number, and the vertical temperature line_18: structure. Observations of this type will drive fundamental new insights into line_19: the physics of accretion disks. ! ! end of abstract general_form_proposers: lname: LONG fname: KNOX mi: S. inst: 3470 country: USA ! lname: BAPTISTA fname: RAYMUNDO inst: 3470 country: USA ! lname: HORNE fname: KEITH inst: 6890 country: THE NETHERLANDS ! lname: HUBENY fname: IVAN inst: 2856 country: USA ! lname: MAUCHE fname: CHRISTOPHER mi: W. inst: 2460 country: USA ! lname: RUTTEN fname: RENE' inst: 7680 country: SPAIN esa: Y ! lname: WADE fname: RICHARD mi: A. inst: 3150 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will observe 4 eclipses of the novalike variable UX UMa. We are line_2: primarily interested in studying continuum and emission line time line_3: variability, and therefore we will use the FOS in "RAPID READOUT" mode line_4: with SUB-STEP=2 and READ-TIME=6 to obtain high temporal resolution. line_5: Ideally binary phases -0.15 thru 0.15 should be covered to include the line_6: eclipse of the disk with enough baseline on either side to establish line_7: the out-of-eclipse spectrum. This requires 85 m for UX UMa (Porbit = line_8: 283m). UX UMa is very near the continuous viewing zone (satisfying the line_9: night-time FGS limit of 12 deg) and therefore optimal or nearly optimal line_10: exposure times should be possible. line_11: Observing four eclipses will help us to distinguish systematic eclipse line_12: features from random flickering variations that are characteristic of line_13: cataclysmic variables. The mean of the four eclipses will be used to line_14: study the disk structure, while the residuals after subtracting the line_15: mean eclipse will inform us about the variability properties of line_16: different parts of the disk. The observations should be spaced as line_17: closely in time as possible in order to minimize the effect of secular line_18: variations in the disk structure. line_19: We will use the Blue Digicon with the G160L disperser, which gives line_20: spectral coverage at 6.5A/pixel from 1150 to 2400 A, and the Red line_21: Digicon with the PRISM disperser, which covers 1600 to 8000 A with line_22: variable resolution. These low dispersions provide the broadest line_23: possible wavelength coverge with sufficent resolution to isolate the ! question: 3 section: 2 line_1: strong, but widely spaced emission lines from the continuum. The line_2: zero-order spectrum available with the G160L grating will provide line_3: a simultaneous "optical" light curve with a bandpass of 1900A FWHM line_4: centered at 3400A. We will acess flickering effects on the mean eclipse line_5: light curve using the 4 independent eclipse light curves obtained from line_6: the 1600-2300A region in which the G160L and PRISM coverages overlap. line_7: We will observe the first and third eclipses with the G160L disperser line_8: and the second/fourth with the PRISM. The red spectra are needed to line_9: cover Mg II emission and the Balmer continuum and line emission region; line_10: the G160L observations are needed to study the hottest portions of the line_11: disk and the higher ionization state lines--N V and C IV. line_12: The above program assumes we are able to use ACQ/BINARY target line_13: acquisition. If we are forced to use ACQ/PEAK - which is much more line_14: time consuming - we will have to remove the last eclipse observation line_15: (with FOS/RD,PRISM). ! question: 4 section: 1 line_1: HST is the only experiment with sufficient sensitivity, spectral line_2: resolution, and temporal resolution in the UV to carry out this type line_3: of observation. We have studied this system previously in the UV. line_4: Other spacecraft (IUE, Voyager, etc.) have collecting areas that are line_5: too small to achieve the S/N and the time resolution we need. (In this line_6: regard, it is important to note that the WD in this system is eclipsed line_7: in a period of about 50 sec). line_8: Our team has extensive experience in observing and modeling the eclipses line_9: of cataclysmic variables. We have observed eclipses with Earth-based line_10: telescopes and have published analyses for a half-dozen systems. line_11: However, the inner region of the accretion disk, the boundary layer, line_12: and the WD should be most apparent in the UV and therefore high line_13: time-resolution UV observations are crucial to significant new line_14: advances in our understanding of CVs. ! question: 5 section: 1 line_1: These observations are time critical and must cover specific orbital line_2: phases. The orbital ephemeris of this system is well known so the line_3: conditions can be specified well in advance. We must observe four line_4: eclipses of the star so we can separate flickering variations from line_5: orbital variations. The target is a novalike variable and therefore it line_6: does not undergo the periodic outbursts associated with dwarf novae line_7: (Very occassionally it is found in a low state). The object do vary line_8: somewhat and therefore all four of the observations should be scheduled line_9: as close together as is possible to minimize the effects of any secular line_10: variations and the joining together of the light curves from the line_11: various eclipses. Whole eclipses must be observed whenever possible. line_12: To observe whole eclipse light curves, it is necessary to have line_13: uninterrupted long exposures; as discussed above the object is in or line_14: very near the continuous viewing zone. ! question: 6 section: 1 line_1: none ! ! ! question: 9 section: 1 line_1: GO-2380 "Instabilities in Accretion Disks and the Outbursts of Dwarf line_2: Novae" (HORNE, CO-I) - This program is related to our proposal. line_3: Data were obtained and are under analysis. A first paper is nearly line_4: ready for submission. Eclipses of the accretion disk were observed in line_5: quiescence and during a superoutburst. The white dwarf dominates the line_6: quiescent spectrum and has deep FeII absorption from intervening line_7: material in the upper atmosphere of the disk. Strange dips are seen line_8: during the superoutburst light curve, probably because outer disk line_9: material obscures the inner disk. The white dwarf is brighter after line_10: superoutburst than before. These data are not suitable for our study line_11: because the quiescent disk is optically thin, too faint, and not in a line_12: steady state, while the superoutbursting disk is also not in a steady line_13: state and suffers severe obscuration of the inner disk by intervening material. line_14: GO-3232 "Observations of X-Ray Nova Muscae 1991" (HORNE, CO-I) - line_15: This program is only periferally related to our proposal. By combining line_16: HST/FOS, IUE, optical and X-ray spectra of Nova Muscae on the decline line_17: from outburst we place limits on the mass of the putitive black hole line_18: in this system, and show that the cooling front predicted by disk line_19: instability model was not seen in this object. Results are published in Ap.J. line_20: GO-3578 "Line Eclipse Mapping of an Accretion Disk Wind" (HORNE, CO-I) line_21: The program is related to this proposal. HRS was used to investigate line_22: line profile changes during the eclipses of UX UMa. Deep eclipses were line_23: observed in the UV, showing that the UV light from UX UMa's disk is ! question: 9 section: 2 line_1: concentrated toward the disk center. The data are not suitable for our line_2: present study because the HRS data were taken at high resolution to line_3: focus on eclipse effects in line profiles. We are currently analyzing line_4: these data with our eclipse mapping programs, but they will cover only line_5: 40A regions near 1550 and 1640A. Our present proposal aims to observe line_6: the entire optical and ultraviolet. line_7: GO-3683 "Accretion Disk Mapping in Eclipsing Cataclysmic Variables" line_8: (HORNE, PI; RUTTEN, LONG, WADE, CO-I) - This program is related to our proposal. line_9: Data on the dwarf nova IP Peg were obtained and are under analysis. line_10: The bright spot dominates the ultraviolet light and it flickers line_11: strongly in quiescence. This data is not suitable for our present line_12: program because the IP Peg disk is not in a steady state. line_13: GO-3600 "Oscillations, Flares, and Tomography of AE Aquarii" (HORNE, PI) line_14: This program is only periferally related to our proposal. Data were line_15: obtained and are under analysis. Oscillations and flares have enormous line_16: amplitude in the ultraviolet. Emission lines flare but do not oscillate. line_17: GO-4271 "Testing the Star-Disk Connection: CIV and MgII Maps of Disks" line_18: (HORNE, PI; LONG, RUTTEN, COI) - This program is periferally related line_19: to our proposal. Data have been taken and are under analysis. The disk line_20: of dwarf nova T Leo will be mapped by Doppler tomography in CIV and line_21: MgII emission lines to study the accretion disk chromosphere. ! question: 10 section: 1 line_1: Salary and basic computer facilities are provided for Long, Horne, line_2: Rutten, Hubeny, and Wade. Support is needed for postdoc Baptista. ! !end of general form text general_form_address: lname: LONG fname: KNOX mi: S. category: PI inst: 3470 addr_1: 3700 San Martin Drive city: Baltimore state: MD zip: 21218 country: USA phone: 410-338-4862 telex: long@stsci.edu ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: UX-UMA descr_1: A,151,161,906 pos_1: RA = 204.1711D +/- 0.0001D, pos_2: DEC = +51.9137D +/- 0.0001D equinox: J2000 pm_or_par: N comment_1: ECLIPSING STAR, V=14.2 IN ECLIPSE comment_2: THIS IS A NEAR CVZ TARGET fluxnum_1: 1 fluxval_1: V = 12.8 +/- 0.2 fluxnum_2: 1 fluxval_2: B-V = 0.1 +/- 0.1 fluxnum_3: 2 fluxval_3: F-CONT(1500) = 2.0 +/- 0.5 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE B targname: UX-UMA config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 0.05S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 1.1; req_3: AT 10-MAY-94 +/- 90D comment_1: BRIGHT VARIABLE STAR. comment_2: TO PERMIT COORDINATED OBSERVATIONS. comment_3: PLEASE NOTIFY P.I. WHEN DATES ARE comment_4: SCHEDULED OR CHANGED. ! linenum: 1.100 sequence_1: DEFINE B targname: UX-UMA config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G160L num_exp: 1 time_per_exp: 0.18S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 1.2 ! linenum: 1.200 sequence_1: DEFINE B targname: UX-UMA config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: G160L num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=5 param_2: SEARCH-SIZE-Y=5 param_3: SCAN-STEP-X=.172 param_4: SCAN-STEP-Y=.172 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 2.0 ! linenum: 2.000 sequence_1: DEFINE B targname: UX-UMA config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L num_exp: 1 time_per_exp: 62M priority: 1 param_1: SUB-STEP=2 param_2: READ-TIME=6 req_1: CYCLE 4; req_2: NON-INT; req_3: ZERO-PHASE JD2443904.87872 +/- 0.00003D; req_4: PERIOD 0.196671278D +/- 0.00000002D; req_5: PHASE 0.89 +/- 0.01 ! linenum: 3.000 sequence_1: DEFINE R targname: UX-UMA config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 2.3S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 3.1 comment_1: BRIGHT VARIABLE STAR. ! linenum: 3.100 sequence_1: DEFINE R targname: UX-UMA config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: PRISM num_exp: 1 time_per_exp: 2.3S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 4.0 ! linenum: 4.000 sequence_1: DEFINE R targname: UX-UMA config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 78M priority: 1 param_1: SUB-STEP=2 param_2: READ-TIME=6 req_1: CYCLE 4; req_2: NON-INT; req_3: ZERO-PHASE JD2443904.87872 +/- 0.00003D; req_4: PERIOD 0.196671278D +/- 0.00000002D; req_5: PHASE 0.86 +/- 0.02; ! linenum: 5.000 sequence_1: USE B req_1: SEQ 5-6 WITHIN 5 D ! linenum: 6.000 sequence_1: USE B comment_1: AS SOON AS POSSIBLE AFTER 5 ! linenum: 7.000 sequence_1: USE R req_1: SEQ 7-8 WITHIN 5 D ! linenum: 8.000 sequence_1: USE R comment_1: AS SOON AS POSSIBLE AFTER 7 ! ! end of exposure logsheet ! No scan data records found