! File: 3683C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:16:09:57 coverpage: title_1: ACCRETION DISK MAPPING IN ECLIPSING CATACLYSMIC VARIABLES sci_cat: STELLAR ASTROPHYSICS sci_subcat: ERUPTIVE BINARIES proposal_for: GO targ_of_opp: Y pi_title: DR pi_fname: KEITH pi_mi: D pi_lname: HORNE pi_inst: STSCI pi_country: USA pi_phone: 301-338-4964 hours_pri: 10.32 num_pri: 2 fos: Y realtime: N time_crit: Y funds_amount: 176174 funds_length: 12 pi_position: DR off_fname: HERVEY off_mi: S. off_lname: STOCKMAN off_title: DEPUTY DIRECTOR off_inst: STSCI off_addr_1: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 301-338-4730 ! end of coverpage abstract: line_1: We will use the FOS in RAPID readout mode to obtain time-resolved ultraviolet line_2: spectrophotometry of accretion disk eclipses in two long-period cataclysmic line_3: variables, the nova-like variable UX UMa and the dwarf nova IP Peg in outburst line_4: and quiescence. From the eclipse data in the UV lines and continuum, we will line_5: map the structure of the hot inner accretion disk, boundary layer, and line_6: stream-disk interaction region using a combination of light-curve synthesis and line_7: maximum entropy mapping techniques. The principle goal of this experiment is to line_8: study the structure of accretion disks in order to test accretion disk models line_9: that are applied widely throughout astrophysics, e,g, in models of protostars line_10: and active galactic nuclei. The observations will also permit a study of the line_11: geometry of winds in these systems, and more accurate determinations of the line_12: masses, radii, and temperatures of the primary and secondary stars, which will line_13: contribute to our understanding of the evolution of close binary systems. line_14: NOTE: TAC has cut the UX UMa observations from this proposal. ! ! end of abstract general_form_proposers: lname: HORNE fname: KEITH title: PI mi: D inst: STSCI country: USA esa: N ! lname: BARWIG fname: HEINZ inst: UNIVERSITY OF MUNICH country: GERMANY esa: Y ! lname: LONG fname: KNOX inst: STSCI country: USA esa: N ! lname: MANTEL fname: KARL-HEINZ inst: UNIVERSITY OF MUNICH country: GERMANY esa: Y ! lname: MARSH fname: THOMAS mi: R inst: OXFORD UNIVERSITY country: UK esa: Y ! lname: POLIDAN fname: RONALD mi: S inst: NASA/GSFC country: USA esa: N ! lname: RAYMOND fname: JOHN mi: C inst: CENTER FOR ASTROPHYSICS country: USA esa: N ! lname: ROBINSON fname: EDWARD mi: L inst: UNIVERSITY OF TEXAS country: USA esa: N ! lname: RUTTEN fname: RENE inst: STERRENKUNDIG INSTITUUT "ANTON PANNEKOEK", AMSTERDAM country: NETHERLANDS esa: Y ! lname: SHAFTER fname: ALLEN mi: W inst: SAN DIEGO STATE UNIVERSITY country: USA esa: N ! lname: SZKODY fname: PAULA inst: UNIVERSITY OF WASHINGTON country: USA esa: N ! lname: WADE fname: RICHARD mi: A inst: PENN STATE UNIVERITY country: USA esa: N ! lname: WOOD fname: JANET mi: H inst: UNIVERSITY OF KEELE country: UNITED KINGDOM esa: Y ! lname: ZHANG fname: ER-HO inst: UNIVERSITY OF TEXAS AT AUSTIN country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will observe 3 eclipses of IP Peg in quiescence, and 4 eclipses of IP Peg line_2: near the peak and on the decline from an outburst. We will rely upon the AAVSO line_3: to inform us when an outburst of IP Peg begins, and the HST observations of IP line_4: Peg declining from outburst should begin within 2-4 days later. line_6: For each eclipse, binary phases -0.15 thru +0.15 should ideally be covered to line_7: include the eclipse of the disk with enough baseline on either side to line_8: establish the out-of-eclipse spectrum. This would require 68 minutes for IP line_9: Peg (Porbit=228m). We settle here for ~49min exposures covering phases -0.10 to line_10: +0.11. IP Peg 's binary period is approximately 2.38 HST orbit periods, line_11: thus an opportunity to observe an eclipse may occur every 5 HST orbits. line_13: Observing a minimum of three eclipses will help us to distinguish systematic line_14: eclipse features from random flickering variations that are characteristic of line_15: cataclysmic variables. The mean of the three eclipses will be used to study line_16: the disk structure, while the residuals after subtracting the mean eclipse line_17: will inform us about the variability properties of different parts of the line_18: disk. For IP Peg in quiescence, the 3 eclipses should be obtained as close line_19: together in time as possible in order to minimize the effect of secular line_20: variations in the disk structure. For IP Peg in outburst we wish to obtain 4 line_21: eclipses spaced by about 1 day in order to follow the propogation of cooling line_22: fronts as the disk declines from outburst. line_23: We will use the Blue Digicon with G160L disperser, which gives spectral ! question: 3 section: 2 line_1: coverage at 6.5A/pixel from 1150 to 2300A, and the Red Digicon with PRISM line_2: disperser, which covers 1700 to 9000A with variable resolution. These low line_3: dispersions provide the broadest possible wavelength coverage with sufficient line_4: resolution to isolate the strong but widely-spaced emission lines from the line_5: continuum. Our interest lies primarily in eclipses of continuum and emission line_6: line fluxes rather than in velocity profiles of the lines. The zero-order line_7: spectrum available with the G160L grating will provide a simultaneous optical line_8: light curve. line_10: For IP Peg in quiescence we will observe the first and third eclipses with line_11: FOS,BLUE,G160L and the second with FOS,RED,PRISM. The red spectra covering the line_12: MgII emission line and the Balmer continuum and line emission will help to line_13: constrain optically-thin regions such as the disk chromosphere. Both the red line_14: and blue configurations cover the 1700-2300A region, from which we will line_15: construct the best mean UV continuum light curve. For IP Peg in outburst we use line_16: FOS,BLUE,G160L for all 4 eclipses. ! question: 4 section: 1 line_1: The following capabilities unique to HST are needed: line_2: (1) sensitivity at space-ultraviolet wavelengths. line_3: (2) large aperture and efficient instruments. line_4: Other space instruments (IUE, Astro, Voyager, etc.) have collecting areas too line_5: small to achieve the necessary signal-to-noise ratios during the rapid line_6: eclipses, or cannot provide adequate time-resolution of the eclipses. line_8: Our team has extensive experience in observations and theoretical modelling of line_9: the spectra and eclipses of cataclysmic variables. We have observed eclipses line_10: with ground-based telescopes and have published analyses for a half-dozen line_11: systems. We have analyzed ultraviolet spectrophotometry of cataclysmic line_12: variables with IUE, Voyager and HUT and have published results for several line_13: dozen systems. We have measured radial velocity curves for about two dozen line_14: cataclysmic variables. We have studied the theoretical and observational line_15: properties of boundary layers between accretion disks and white dwarfs. These line_16: efforts have established the framework for interpreting the HST observations of line_17: eclipses in the ultraviolet, which provide crucial information about the the line_18: white dwarf, the inner regions of the disk and the boundary layer between them. ! question: 5 section: 1 line_1: We request time-critical observations for two reasons. First, the observations line_2: must cover specific orbital phases centered on eclipse. Second, we must observe line_3: three eclipses of each star so we can identify features in the light curves line_4: caused by flickering variations as opposed to eclipses. The cataclysmic line_5: variables vary secularly, and as the time interval between the eclipses line_6: increases, the size of secular changes in the systems will increase. All line_7: observations of a given target should, if possible, be obtained within a period line_8: of one or two weeks to minimize the effect of these secular variations. The line_9: secular variations also make it difficult to construct eclipse light curves by line_10: joining parts of many different eclipses. Whole eclipses must be observed line_11: whenever possible. To observe whole eclipse light curves, it is necessary to line_12: have uninterrupted long exposures. line_14: We request target of opportunity status for part of the observations intended line_15: to catch eclipses of IP Peg in outburst. The recurrence time for IP Peg is line_16: about 60-100 days; the probability of occurrence is high, but our understanding line_17: of the outbursts is too primitive to predict in advance when outbursts will line_18: occur. We will arrange for the AAVSO to monitor IP Peg and alert us when an line_19: outburst occurs. The decline from outburst generally begins 3-5 days after the line_20: rise, so a 2-3-d response should make it possible for the eclipses to occur line_21: near the peak or early decline of the outburst. ! question: 6 section: 1 line_1: Instrument Mode Special Calibration Requirement line_2: __________ _______ ________________________________ line_3: FOS/BL G160L Observe a flux standard that does line_4: not saturate the zero-order spec ! question: 7 section: 1 line_1: Initial data reduction and calibration will use the standard pipelined software line_2: at STScI. We will display the data as trailed spectrograms, and probably do line_3: some hand editing to eliminate noise bursts and other special problems. line_4: Calibrated data will then be distributed to co-investigators for analysis at line_5: their home institutions. line_7: We will extract eclipse light curves in selected continuum passbands and the line_8: emission lines. The three eclipses will be averaged together to form mean light line_9: curves, and the mean will be subtracted from the individual eclipses to examine line_10: the residuals due to flickering variations. Power-spectrum analysis will be line_11: performed to search for coherent or quasiperiodic oscillations which are line_12: sometimes seen in the optical light from cataclysmic variables. Some immediate line_13: qualitative interpretations will be made by direct inspection of the light line_14: curves. Ground-based and/or Voyager data obtained around the times of the HST line_15: observations will be brought together for interpretation along with the HST line_16: results. line_18: We will then proceed to fit detailed models to the data, using the light-curve line_19: synthesis and eclipse mapping techniques we have developed for ground-based line_20: data (see Horne 1985, Zhang, Robinson and Nather 1986). These analyses will line_21: yield geometries of the components, temperature and luminosity distributions line_22: for the disk, and the properties of the boundary layers. For the IP Peg line_23: observations in outburst a time-dependent disk model will be compared with the ! question: 7 section: 2 line_1: data to derive disk instability parameters. Improvements in the disk model line_2: codes will probably be needed to fit the high-quality HST observations. Results line_3: of these investigations will be presented at meetings and written up for line_4: publication in major refereed journals. ! question: 8 section: 1 line_1: The proposed HST observations form a self contained experiment: the eclipse line_2: analyses will yield new and significant information even if no other data are line_3: available. We feel strongly, however, that the scientific results of the line_4: eclipse analyses will be enhanced if the spectrophotometry from HST is line_5: complemented by photometry or spectrophotometry at other wavelengths. We will line_6: therefore attempt to obtain contemporaneous or even simultaneous observations line_7: at other wavelengths. For this purpose we have access to ground-based line_8: telescopes at the McDonald, La Palma, Mt. Laguna, Mt. Wendelstein, Manastash line_9: Ridge, Mount Hopkins, and Kitt Peak observatories, and we will request line_10: observing time on these telescopes for supporting eclipse observations at line_11: visual and near-infrared wavelengths. We also have access to the Voyager line_12: spacecraft with which we will attempt to obtain far-UV coverage of UX UMa line_13: eclipses. Our team has experience from several previous experiments line_14: involving simultaneous ground- and satellite-based observations. line_15: (NOTE: TAC has cut the UX UMa observations from this proposal.) ! question: 9 section: 1 line_1: GO-2243 "The Shock-Wave Structure of Herbig Haro Objects" line_2: Schwartz, Bohm, Cohen, Dopita, Hartman, Jones, Mundt, Raymond. line_3: GO-2356 "Identification of SNRs in M83 and other Spiral Galaxies" line_4: Long, Blari, Winkler, Kirshner, Raymond. line_5: GO-2380 "Instabilities in Accretion Disks and the Outbursts of Dwarf Novae" line_6: Horne and Marsh. line_7: GO-2334 "Ultraviolet Spectroscopy of the Black Hole A0620-00" line_8: McClintock, Remillard, and Horne. line_9: GO-3232 "Observations of X-Ray Nova Muscae 1991" line_10: Panagia, Lund, Gilmozzi, Horne, Paresce, Valle, and Schrader. line_12: Robinson has GTO time on the HSP. The first science data from the HSP will not line_13: be obtained before August 1991 according to the present HST schedule. line_15: GO-2380 may obtain eclipse observations of the short-period dwarf nova OY Car line_16: to test the prediction of disk instability models that the disk's UV flux line_17: should increase during quiescence. The present proposal will observe two line_18: systems with Porbit near 4h, the nova-like variable UX UMa, and the dwarf nova line_19: IP Peg. This will begin to sample the dependence of disk structure over the line_20: (Porbit-Mdot) parameter space. ! question: 10 section: 1 line_1: Salary and basic computer facilities are being provided for the P.I line_2: and many of the Co-Is. ! !end of general form text general_form_address: lname: HORNE fname: KEITH category: PI inst: STSCI addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA phone: 410-338-4964 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: IP-PEG descr_1: A,149,161 pos_1: PLATE-ID = 02BB, pos_2: RA = 23H 23M 8.61S +/- 0.5", pos_3: DEC = +18D 24' 59.5" +/- 0.5" equinox: J2000 pm_or_par: N pos_epoch_bj: B pos_epoch_yr: 1982.81 comment_1: DWARF NOVA V=11 IN OUTBURST, comment_2: V=14-16 IN QUIESCENCE. comment_3: ECLIPSING STAR, V=18 IN ECLIPSE. fluxnum_1: 1 fluxval_1: V = 15 +/- 1 fluxnum_2: 1 fluxval_2: B-V = 0.2 fluxnum_3: 1 fluxval_3: F-CONT(1500) = 1 +/- 1 E-14 fluxnum_4: 2 fluxval_4: V = 11 +/- 1 fluxnum_5: 2 fluxval_5: B-V = 0.0 fluxnum_6: 2 fluxval_6: F-CONT(1500) = 1 +/- 1 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: IP-PEG config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 15S fluxnum_1: 1 priority: 1 req_1: GROUP 1-2 NO GAP; req_2: ONBOARD ACQ FOR 1.5; req_3: SPATIAL SCAN; ! linenum: 1.500 sequence_1: DEFINE B targname: IP-PEG config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G160L num_exp: 1 time_per_exp: 15S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 2; req_2: SPATIAL SCAN; ! linenum: 2.000 sequence_1: DEFINE B targname: IP-PEG config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L wavelength: 1500 num_exp: 1 time_per_exp: 40.75M priority: 1 param_1: READ-TIME=6.18 req_1: NON-INT ; req_2: PERIOD 0.15820613D +/- 0.00000004D ; req_3: ZERO-PHASE JD2445615.4224 +/- 0.001D ; req_4: PHASE 0.90 +/- 0.02 ; comment_1: TRY TO CENTER EXPOSURE ON PHASE 0.005, comment_2: MUST COVER PHASES -0.09 TO +0.10. comment_3: BINARY PERIOD IS NEAR 2.36 HST ORBITS, comment_4: THUS ECLIPSE WINDOW OCCURS EVERY 5TH comment_5: HST ORBIT. ! linenum: 4.000 sequence_1: DEFINE R targname: IP-PEG config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 15S fluxnum_1: 1 priority: 1 req_1: GROUP 4-5 NO GAP; req_2: ONBOARD ACQ FOR 4.5; req_3: SPATIAL SCAN; ! linenum: 4.500 sequence_1: DEFINE R targname: IP-PEG config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G160L num_exp: 1 time_per_exp: 15S fluxnum_1: 1 priority: 1 req_1: GROUP 4-5 NO GAP; req_2: ONBOARD ACQ FOR 5; req_3: SPATIAL SCAN; ! linenum: 5.000 sequence_1: DEFINE R targname: IP-PEG config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 39.5M priority: 1 param_1: READ-TIME=6.18 req_1: NON-INT; req_2: PHASE 0.90 +/- 0.02 OF REF 2; comment_1: TRY TO CENTER EXPOSURE ON PHASE 0.005, comment_2: MUST COVER PHASES -0.09 TO +0.10. comment_3: BINARY PERIOD IS NEAR 2.36 HST ORBITS, comment_4: THUS ECLIPSE WINDOW OCCURS EVERY 5TH comment_5: HST ORBIT. ! linenum: 7.000 sequence_1: USE B req_1: AT 30-SEP-92 +/- 90D ; req_2: SEQ 7-9 WITHIN 7 D ; comment_1: PI IS PLANNING COORDINATED comment_2: OBSERVATIONS. ! linenum: 8.000 sequence_1: USE R req_1: AFTER 7 ; comment_1: AS SOON AS POSSIBLE AFTER 7 ! linenum: 9.000 sequence_1: USE B req_1: AFTER 8 ; comment_1: AS SOON AS POSSIBLE AFTER 8 ! linenum: 10.000 sequence_1: USE B req_1: TARG OF OPP / 10-13 ; req_2: SEQ 10-13 WITHIN 7 D ; comment_1: EXECUTE AS SOON AS POSSIBLE AFTER PI comment_2: REQUEST TO ACTIVATE THESE TARG OF OPP comment_3: EXPOSURES. ! linenum: 11.000 sequence_1: USE B req_1: AFTER 10 BY 1D +/- 1 D ; comment_1: IDEALLY 15 HRS AFTER 10 ! linenum: 12.000 sequence_1: USE B req_1: AFTER 11 BY 1D +/- 1 D ; comment_1: IDEALLY 15 HRS AFTER 11 ! linenum: 13.000 sequence_1: USE B req_1: AFTER 12 BY 1D +/- 1 D ; req_2: CYCLE 2 / 1-13 ; comment_1: IDEALLY 15 HRS AFTER 12 ! ! end of exposure logsheet scan_data: line_list: 1,4 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.4 wid_offset: 0.0 ! line_list: 1.5,4.5 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.75 wid_offset: 0.35 ! ! end of scan data