! File: 3578C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:12:38:35 coverpage: title_1: LINE ECLIPSE MAPPING OF AN ACCRETION DISK WIND sci_cat: STELLAR ASTROPHYSICS sci_subcat: ERUPTIVE BINARIES proposal_for: GO cont_id: 3578 pi_fname: KEITH pi_mi: O. pi_lname: MASON pi_inst: MULLARD SPACE SCIENCE LABORATORY pi_country: UK pi_phone: 44-483-274111 hours_pri: 4.00 num_pri: 1 hrs: Y time_crit: Y funds_amount: 127895 funds_length: 12 off_fname: J. off_mi: L. off_lname: CULHANE off_title: DIRECTOR off_inst: MULLARD SPACE SCIENCE LABORATORY off_addr_1: HOLMBURY ST.MARY off_addr_2: DORKING off_city: SURREY off_state: RH5 off_zip: 6NT off_country: UK off_phone: (44) 483 274111 ! end of coverpage abstract: line_1: We propose to measure changes in the profiles of wind-formed lines line_2: in the nova-like variable UX UMa as they are eclipsed by the line_3: companion star. Models predict that these changes are dramatic line_4: when viewed at high enough spectral resolution, and the line_5: measurements we make will allow us to map out the kinematics line_6: and density profile of an accretion disk wind for the first time. line_7: By comparing lines of different species we will determine the line_8: ionization structure of the wind, which is important for line_9: determining the total mass-loss rate. The proposed observations line_10: are well suited to the capabilities of the GHRS on HST, and will line_11: provide the raw material for a quantum leap in our understanding line_12: of accretion disk winds, a phenomenon encountered in a wide range line_13: of astrophysical settings. ! ! end of abstract general_form_proposers: lname: MASON fname: KEITH title: PI mi: O. inst: MULLARD SPACE SCIENCE LABORATORY country: U.K. esa: Y ! lname: DREW fname: JANET mi: E. inst: UNIVERSITY OF OXFORD country: U.K. esa: Y ! lname: MARSH fname: TOM inst: UNIVERSITY OF OXFORD country: U.K. esa: Y ! lname: HORNE fname: KEITH inst: STSCI country: USA esa: N ! lname: CORDOVA fname: FRANCE mi: A. inst: PENNSYLVANIA STATE UNIVERSITY country: U.S.A. esa: N ! lname: MAUCHE fname: CHRIS inst: LAWRENCE LIVERMORE LABORATORY country: U.S.A. esa: N ! lname: RAYMOND fname: JOHN inst: HARVARD CENTER FOR ASTROPHYSICS country: U.S.A. esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The target of our observation is UX UMa, a 13th mag eclipsing line_2: novalike variable. Our aim is to observe the eclipse of UV lines line_3: in UX UMa with sufficient phase resolution to probe spatial line_4: structure of order 1 white dwarf radius which means exposure times line_5: better than 1 min. The G160M grating will give us more than line_6: sufficient velocity sampling; indeed we expect to integrate signal line_7: from several diodes in order to optimise the velocity and phase line_8: resolution. We will concentrate on the two most important UV lines line_9: CIV1550A and HeII1640A. We wish to observe the CIV line through 3 line_10: separate eclipses starting at phase 0.895 and going through to line_11: phase 0.105, covering the 30 min eclipse plus sufficient out of line_12: eclipse phases to provide a reference. Observing 3 eclipses is line_13: important to distinguish phase-dependent from random variability. line_14: In 2 CIV measurements we will optimise the grating setting for line_15: the blue wing of the line, in the third we will optimise for the line_16: red wing. The central portion of the line will be covered at both line_17: grating settings. A short observation at the alternate grating line_18: setting after eclipse is included to provide a reference against line_19: long-term line profile changes. A fourth eclipse will be observed line_20: in the HeII line which is narrow enough that both wings can be well line_21: included in one observation. UX UMa is in the continuous viewing line_22: zone so long observations should be possible. ! question: 4 section: 1 line_1: The scientific goal of the proposed observations cannot be achieved line_2: from the ground. This is because the winds in cataclysmic variables line_3: contribute little to the optical hydrogen and helium emission lines line_4: observed in CV spectra (the accretion disk is the main source of line_5: optical line emission). To map an accretion disk wind, it is line_6: essential to obtain ultraviolet spectroscopy. The proposal cannot be line_7: accomplished using IUE because the combination of time and spectral line_8: resolution achievable is inadequate (well exposed low dispersion line_9: spectra of UX UMa out of eclipse require 30 minutes line_10: exposures made of UX UMa with IUE, at five minutes long, are too line_11: noisy to do anything other than obtain crude estimates for the line_12: resonance line fluxes (see King et al. 1983). With the GHRS on HST, line_13: much better time and spectral resolution can be achieved (we expect line_14: more than an order of magnitude improvement in the effective time line_15: resolution coupled with a 4-fold increase in spectral resolution). line_17: UX UMa has also been observed with the Hopkins Ultraviolet Telescope line_18: during the ASTRO mission (Long, private communication). However, line_19: the statistical quality of the data and its spectral resolution (3A) line_20: are not adequate for the present purpose. Moreover, the time line_21: resolved data from the central 10 minutes of the eclipse were lost line_22: owing to a telemetry failure. ! question: 5 section: 1 line_1: The observations are time-critical in the sense that each line_2: needs to be centred on the target's primary eclipse to an accuracy line_3: of about +/- 5 minutes. The ephemeris of UX UMa is well-known. line_4: UX~UMa borders on the continuous viewing zone for the spacecraft. ! question: 6 section: 1 line_1: The objective is to measure how the UV line shape and flux line_2: is modified through the eclipse. Thus uninterupted line_3: observations of the eclipse are essential. ! question: 7 section: 1 line_1: Standard techniques for wavelength and flux calibration of the GHRS line_2: spectra will be adequate. To interpret the data we have available a line_3: sophisticated, purpose-built Monte Carlo code for simulating line line_4: profile changes for various wind, disk and binary input parameters. line_5: This program was written by Woods as part of his graduate studies line_6: working with Drew and has already been applied to the study of CV line_7: wind line profiles (Woods 1990). One of the features of this code is line_8: its flexibility which gives us confidence that we will be able to line_9: adapt it to take account of unexpected features of the data. Indeed line_10: it is planned to adapt it to deal with rotational motion within the line_11: next year. ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: a. List HST program numbers and titles, and specify whether they are line_2: related to this project or not. line_4: "Instabilities in accretion disks and the outbursts of dwarf novae" line_5: Program No. 2380 Unrelated to this project line_7: b. Summarize the main results obtained from previous related line_8: programs. line_10: No observations taken yet. line_12: c. List publications resulting from the above data (Format: Title, line_13: Authors,Journal, Volume, Page, and Year.) line_15: N/A ! question: 10 section: 1 line_1: All members of the consortium routinely have access to DEC Vax line_2: computers and UNIX workstations dedicated to astronomical data line_3: reduction, and all members are linked by computer networks. A line_4: number of us also regularly supervise postgraduate research students line_5: who can be involved in the task of reducing and analysing HST line_6: observations. ! !end of general form text general_form_address: lname: MASON fname: KEITH mi: O. category: PI inst: MULLARD SPACE SCIENCE LABORATORY addr_1: HOLMBURY ST.MARY addr_2: DORKING city: SURREY state: SU zip: RH5 6NT country: UK phone: (44) 483 274111 telex: 859185 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: UXUMA descr_1: A, 151 pos_1: RA = 13H 36M 40.97S +/- 0.02S, pos_2: DEC = +51D 54' 50.2" +/- 0.3", pos_3: PLATE-ID=00XN equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 1983.35 comment_1: ECLIPSING STAR - MID-ECLIPSE V=14.1 fluxnum_1: 1 fluxval_1: V=12.7 +/- 0.1 fluxnum_2: 2 fluxval_2: F-LINE(1549)=5 +/- 1 E-13 fluxnum_3: 3 fluxval_3: W-LINE(1549)=15 +/- 5 fluxnum_4: 4 fluxval_4: F-CONT(1549)=2 +/- 0.1 E-13 fluxnum_5: 5 fluxval_5: E(B-V)=0.02 +/- 0.02 fluxnum_6: 6 fluxval_6: B-V=0.0 fluxnum_7: 7 fluxval_7: F-LINE(1640)=2 +/- 0.2 E-13 fluxnum_8: 8 fluxval_8: W-LINE(1640)=10 +/- 3 fluxnum_9: 9 fluxval_9: F-CONT(1640)=1.6 +/- 0.1 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: UXUMA config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 4 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 2-3; req_2: CYCLE 2; ! linenum: 2.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1538 num_exp: 1 time_per_exp: 15M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 2 fluxnum_2: 3 priority: 2 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: NON-INT; ! linenum: 3.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1538 num_exp: 1 time_per_exp: 45M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: PERIOD 0.196671300D +/- 0.000000001D; req_3: PHASE 0.921 +/- 0.02; req_4: ZERO-PHASE JD2420238.241 +/- 0.002D; req_5: NON-INT; comment_1: EXPOSURE TIME DICTATED BY NEED TO comment_2: COVER ECLIPSE PHASE -0.1 TO +0.1, comment_3: RATHER THAN BY S/N REQUIREMENTS. comment_4: OK TO INCREASE EXPOSURE TO FILL OUT comment_5: HST ORBIT. S/N PER DIODE GIVEN: comment_6: S/N PER ANG PER MIN = 8 ! linenum: 4.000 targname: UXUMA config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 4 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 5-6; req_2: CYCLE 2; ! linenum: 5.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1538 num_exp: 1 time_per_exp: 15M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 2 fluxnum_2: 3 priority: 2 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: NON-INT; ! linenum: 6.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1538 num_exp: 1 time_per_exp: 45M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: PERIOD 0.196671300D +/- 0.000000001D; req_3: PHASE 0.921 +/- 0.02; req_4: ZERO-PHASE JD2420238.241 +/- 0.002D; req_5: NON-INT comment_1: EXPOSURE TIME DICTATED BY NEED TO comment_2: COVER ECLIPSE PHASE -0.1 TO +0.1, comment_3: RATHER THAN BY S/N REQUIREMENTS. comment_4: OK TO INCREASE EXPOSURE TO FILL OUT comment_5: HST ORBIT. S/N PER DIODE GIVEN: comment_6: SEVERAL DIODES WILL BE BINNED. ! linenum: 7.000 targname: UXUMA config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 4 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 8-9; req_2: CYCLE 2; ! linenum: 8.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1555 num_exp: 1 time_per_exp: 15M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 2 fluxnum_2: 3 priority: 2 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: NON-INT; ! linenum: 9.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1555 num_exp: 1 time_per_exp: 45M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: PERIOD 0.196671300D +/- 0.000000001D; req_3: PHASE 0.921 +/- 0.02; req_4: ZERO-PHASE JD2420238.241 +/- 0.002D; req_5: NON-INT comment_1: EXPOSURE TIME DICTATED BY NEED TO comment_2: COVER ECLIPSE PHASE -0.1 TO +0.1, comment_3: RATHER THAN BY S/N REQUIREMENTS. comment_4: OK TO INCREASE EXPOSURE TO FILL OUT comment_5: HST ORBIT. S/N PER DIODE GIVEN: comment_6: SEVERAL DIODES WILL BE BINNED. ! linenum: 10.000 targname: UXUMA config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 9 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 11-12; req_2: CYCLE 2; ! linenum: 11.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1636 num_exp: 1 time_per_exp: 15M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 2 fluxnum_2: 3 priority: 2 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: NON-INT; ! linenum: 12.000 targname: UXUMA config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1636 num_exp: 1 time_per_exp: 45M s_to_n: 4 s_to_n_time: 5M fluxnum_1: 7 fluxnum_2: 8 priority: 1 param_1: SAMPLE-TIME = 5 req_1: CYCLE 2; req_2: PERIOD 0.196671300D +/- 0.000000001D; req_3: PHASE 0.921 +/- 0.02; req_4: ZERO-PHASE JD2420238.241 +/- 0.002D; req_5: NON-INT; comment_1: EXPOSURE TIME DICTATED BY NEED TO comment_2: COVER ECLIPSE PHASE -0.1 TO +0.1, comment_3: RATHER THAN BY S/N REQUIREMENTS. comment_4: OK TO INCREASE EXPOSURE TO FILL OUT comment_5: HST ORBIT. S/N PER DIODE GIVEN: comment_6: SEVERAL DIODES WILL BE BINNED. ! ! end of exposure logsheet ! No scan data records found