! File: 4297C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:20:49:29 coverpage: title_1: STABILITY OF THE WINDS FROM CATACLYSMIC VARIABLES: title_2: CYCLE3 MEDIUM sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO pi_fname: MELVIN pi_mi: G pi_lname: HOARE pi_inst: UNIVERSITY OF OXFORD pi_country: UK pi_phone: 0865 273292 hours_pri: 0.33 num_pri: 1 fos: Y off_fname: GEORGE off_mi: P off_lname: EFSTATHIOU off_title: HEAD OF ASTROPHYSICS off_inst: 8058 off_addr_1: DEPARTMENT OF PHYSICS off_addr_2: ASTROPHYSICS off_addr_3: KEBLE ROAD off_city: OXFORD off_zip: OX1 3RH off_country: UK off_phone: 0865 273303 ! end of coverpage abstract: line_1: We propose to use the FOS to obtain time-resolved, high-resolution UV spectra line_2: of the bright novalike variable V3885 Sgr in order to determine the stability line_3: of the winds from cataclysmic variables (CVs). Changes in the P Cygni line_4: line profiles on the flow timescale of the wind itself will provide vital clues line_5: for the ultimate goal of discovering the driving mechanism for these accretion line_6: disk winds. In particular we will look for transient features already seen in line_7: radiatively driven winds from hot single stars. line_8: With the high S/N accumalated spectra we will also line_9: be able to determine the extent to which many of the subordinate lines in the line_10: spectrum have wind-formed components. This will substantially increase our line_11: understanding of the ionization state of the wind which has implications line_12: for the total mass loss rate and illuminating radiation field. The latter is line_13: sensitive to the character of the boundary layer which will line_14: tell us whether the white dwarf has been spun up to near breakup speed. line_15: Finally, the accumulated spectra can be used to constrain new NLTE accretion line_16: disk model atmospheres. The proposed observations will greatly further line_17: our understanding of the driving force behind the winds in CVs with subsequent line_18: implications for winds from other accretion disk systems such as protostars line_19: and AGN. ! ! end of abstract general_form_proposers: lname: HOARE fname: MELVIN title: PI mi: G inst: UNIVERSITY OF OXFORD country: UNITED KINGDOM esa: Y ! lname: DREW fname: JANET mi: E inst: UNIVERSITY OF OXFORD country: UNITED KINGDOM esa: Y ! lname: MARSH fname: THOMAS mi: R inst: UNIVERSITY OF OXFORD country: UNITED KINGDOM esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to obtain two uninterrupted 10 minute exposures of V3885 Sgr: line_2: obtained as close as possible in time:one line_3: with the G130H grating and one with the G190H, line_4: both using the blue digicon. The latter grating is needed to determine the line_5: extent of the wind components in the important He II 1640 A and N IV 1718 A line_6: lines. We want the highest spectral resolution possible so we will use the line_7: 0.25x2.0 aperture. We will use the RAPID READOUT mode with 10 second exposures line_8: and 1 MHz data rate in order to look for variations in the line profiles on the line_9: flow timescale of the wind. ! question: 4 section: 1 line_1: line_2: The only alternative UV satellite is the IUE and it does not have sufficient line_3: sensitivity to carry out our proposed observations. Any transient narrow line_4: components in the P Cygni line profiles are likely to be less than 10% of the line_5: wind terminal velocity in width i.e. <500 km/s. This would need the high line_6: resolution mode on IUE which requires exposures lasting many hours in order to line_7: obtain a moderate S/N spectrum of our target. We require time resolution of 10 line_8: seconds to achieve the major aim of determining the stability of the wind. The line_9: high S/N spectrum required to determine the extent of the wind-formed line_10: components in the subordinate lines can never be achieved with the IUE due to line_11: its limitation on S/N of little more than 10 sigma in each exposure. ! question: 4 section: 2 line_1: V3885 Sgr (CD -42 14462) is the second brightest (visual mag.=9.6-10.3) line_2: non-eclipsing, non-magnetic, novalike variable. Low inclination systems are line_3: required to provide a strong source of background continuum against which to see line_4: the absorption lines formed in the wind. The optically brightest novalike, IX line_5: Vel, appears to be at a moderately high inclination since the blueshifted line_6: absorption is not nearly so well developed. In the UV, V3885 Sgr is of line_7: comparable brightness to IX Vel. line_8: The average 1550 A continuum flux for V3885 Sgr is 3E-12 ergs/cm**2/s/A (see line_9: Fig. 5). With the G130H grating and 0.25 x 2.0 aperture this gives a count rate line_10: of 17 counts/s/diode. Hence in 10 seconds of exposure a S/N of 13 sigma is line_11: achieved which is sufficient to look for transient features in the line profile line_12: and to assess overall equivalent width changes. The full 10 minute integration line_13: accumulated will result in a S/N of about 100 sigma over most of the wavelength line_14: range as required for the detailed studies of the line profiles of the line_15: resonance and the weaker subordinate wind lines. Even at C III 1176 A the S/N line_16: will be about 35 sigma despite the dropping efficiency of the grating. line_17: V3885 Sgr is also reasonably close to the continuous viewing zone being only line_18: 19.5 degrees from the pole of HST's orbit which should help in scheduling 2 line_19: close uninterrupted 10 minute integrations. ! question: 5 section: 1 line_1: We require 10 minute uninterrupted exposures in order to track any features line_2: observed in the line profiles over several flow timescales (approx. 1 minute). line_3: The discrete absorption components in OB star winds are observed to accelerate line_4: blueward over a few flow timescales. Note that the flow timescales in OB star line_5: winds are about 100 times slower than for CV winds. We also require the line_6: G130H and G190H exposures within the same acquisition so that we can construct a line_7: complete spectrum of the system at that particular state. There is probably line_8: some variablity of the wind profile on the 5.2 hour orbital period of line_9: V3885 Sgr as well as overall brightness changes on timescales of days. ! question: 7 section: 1 line_1: Data reduction will be carried out using standard software made available line_2: through the UK STARLINK network. Periodicities in any variability in the line line_3: profiles will be searched for using standard techniques. The high S/N profiles line_4: of the wind-formed resonance and subordinate lines will be analysed using the line_5: Monte Carlo and Sobolev codes that we have developed (e.g. Drew 1987, Woods, Ph. line_6: D. Thesis 1991, Hoare & Drew 1992). The former will have the capability to deal line_7: with complex velocity fields such as those in which rotational motion and line_8: non-radial outflow are combined. We will compare the derived concentrations of line_9: the various ionic species with those predicted by our photo-ionization models to line_10: further constrain the boundary layer temperature and luminosity as well as the line_11: total wind mass loss rate. To analyse the disk lines we will collaborate with line_12: whoever has the most well developed NLTE disk atmosphere code at the time. ! question: 9 section: 1 line_1: Cycle 1 line_2: GO-2380 "Instabilities in Accretion Disks and the Outbursts of Dwarf Novae" line_3: Horne & Marsh line_4: Cycle 2 line_5: GO-3578 "Line Eclipse Mapping of an Accretion Disk Wind" line_6: Mason, Drew, Marsh, Horne, Cordova, Mauche, Raymond line_7: None of these are closely related. ! question: 10 section: 1 line_1: The STARLINK node at the University of Oxford will provide the data reduction line_2: and analysis packages required. ! !end of general form text general_form_address: lname: HOARE fname: MELVIN mi: G category: PI inst: University of Oxford addr_1: DEPARTMENT OF PHYSICS addr_2: ASTROPHYSICS addr_3: KEBLE ROAD city: OXFORD zip: OX1 3RH country: UNITED KINGDOM phone: 0865 273292 telex: 83295 NUCLOX G ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: CD-42D14462 name_2: V3885-SGR name_3: GSC7941-00694 descr_1: A,151,905,906 pos_1: PLATE-ID=04FS, pos_2: RA = 19H 47M 40.51S +/- 0.03S, pos_3: DEC = -42D 0' 25.9" +/- 0.3" equinox: 2000 fluxnum_1: 1 fluxval_1: V=10.0+/-0.4,B-V=0.00+/-0.02 fluxnum_2: 2 fluxval_2: U-B=-0.75+/-0.08,E(B-V)=0.05 fluxnum_3: 3 fluxval_3: F-CONT(1550)=3.0+/-1.5 E-12 fluxnum_4: 4 fluxval_4: F-LINE(1550)=1.2+/-0.5 E-11 fluxnum_5: 5 fluxval_5: W-LINE(1550)=15+/-4 fluxnum_6: 6 fluxval_6: F-CONT(1718)=2.0+/-1.0 E-12 fluxnum_7: 7 fluxval_7: F-LINE(1718)=2.6+/-1.5 E-13 fluxnum_8: 8 fluxval_8: W-LINE(1718)=10+/-4 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: CD-42D14462 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 0.2S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: CYCLE 3 / 1-6; req_2: ONBOARD ACQ FOR 2; req_3: SPATIAL SCAN ! linenum: 2.000 targname: CD-42D14462 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 0.3S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: CYCLE 3 / 1-6; req_2: ONBOARD ACQ FOR 3; req_3: SPATIAL SCAN ! linenum: 3.000 targname: CD-42D14462 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G190H num_exp: 1 time_per_exp: 0.6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: CYCLE 3 / 1-6; req_2: ONBOARD ACQ FOR 4; req_3: SPATIAL SCAN ! linenum: 4.000 targname: CD-42D14462 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: G190H num_exp: 1 time_per_exp: 1.5S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: CYCLE 3 / 1-6; req_2: ONBOARD ACQ FOR 5-6; req_3: SPATIAL SCAN ! linenum: 5.000 targname: CD-42D14462 config: FOS/BL opmode: RAPID aperture: 0.25X2.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 10M s_to_n: 13 s_to_n_time: 10S fluxnum_1: 3 priority: 1 param_1: READ-TIME=10 param_2: STEP-PATT=SINGLE param_3: SUB-STEP=4 param_4: COMB=YES req_1: NON-INT / 5-6; req_2: GROUP 5-6 NO GAP ! linenum: 6.000 targname: CD-42D14462 config: FOS/BL opmode: RAPID aperture: 0.25X2.0 sp_element: G190H wavelength: 1950 num_exp: 1 time_per_exp: 10M s_to_n: 17 s_to_n_time: 10S fluxnum_1: 6 priority: 2 param_1: READ-TIME=10 param_2: STEP-PATT=SINGLE param_3: SUB-STEP=4 param_4: COMB=YES ! ! end of exposure logsheet scan_data: line_list: 1 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 ! line_list: 2 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 ! line_list: 3 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.5000 scan_length: 0.5000 sides_angle: 90.0000 number_lines: 3 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.25 wid_offset: 0.25 ! line_list: 4 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2 wid_offset: 0.0 ! ! end of scan data