! $Id: 5674,v 6.1 1994/07/27 20:17:04 pepsa Exp $ coverpage: title_1: ULTRAVIOLET ECLIPSE MAPPING OF THE ACCRETION FLOW IN THE ECLIPSING title_2: INTERMEDIATE POLAR, EX HYA sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO/CAR cont_id: 4661 pi_fname: SIMON pi_mi: R pi_lname: ROSEN pi_inst: UNIVERSITY OF LEICESTER pi_country: U.K. hours_pri: 7.00 num_pri: 1 fos: Y time_crit: Y off_fname: KEN off_lname: POUNDS off_title: HEAD OF DEPT. off_inst: 8042 off_addr_1: DEPT. OF PHYSICS off_addr_2: UNIVERSITY OF LEICESTER off_addr_3: UNIVERSITY RD. off_city: LEICESTER off_country: U.K. off_phone: UK-533-523509 ! end of coverpage abstract: line_1: EX Hya offers a unique opportunity to study the accretion flow onto the white line_2: dwarf in an Intermediate Polar binary, being the only member of its class in line_3: which the environs of that star are eclipsed by its companion. We propose to line_4: exploit the unique ability of HST FOS to secure good S/N, highly time-resolved line_5: UV spectra to perform the first detailed UV eclipse mapping study of EX Hya. line_6: The detailed form of the accretion flow onto the white dwarf in these systems line_7: remains unresolved. It may occur as a funnelled flow along magnetic field lines line_8: from a truncated disk or it may be primarily in the form of an inhomogenous line_9: stream of material that penetrates the magnetosphere. UV observations are line_10: critical because much of the radiation output from this high energy environment line_11: emerges in this band. We aim to use FOS to a) study the line profile changes line_12: through the narrow eclipse to dissect the UV emitting accretion flow near the line_13: white dwarf, b) compare eclipse properties in different lines to search for line_14: ionization structure, c) monitor the evolution of the lines through the broader line_15: eclipse wings to map the putative inner `disk' flow and d) record the motion line_16: and broadening of the line wings as the white dwarf rotates to formulate an line_17: overall dynamical picture. ! ! end of abstract general_form_proposers: lname: ROSEN fname: SIMON title: PI mi: R inst: UNIVERSITY OF LEICESTER country: UNITED KINGDOM esa: Y ! lname: MUKAI fname: KOJI inst: NASA GODDARD SPACE FLIGHT CENTER country: USA esa: N ! lname: WATSON fname: MIKE mi: G inst: UNIVERSITY OF LEICESTER country: UNITED KINGDOM esa: Y ! lname: MASON fname: KEITH mi: O inst: MULLARD SPACE SCIENCE LABORATORY country: UNITED KINGDOM esa: Y ! lname: OSBORNE fname: JULIAN mi: P inst: UNIVERSITY OF LEICESTER country: UNITED KINGDOM esa: Y ! lname: KING fname: ANDREW mi: R inst: UNIVERSITY OF LEICESTER country: UNITED KINGDOM esa: Y ! lname: PRINJA fname: RAMAN mi: K inst: UNIVERSITY COLLEGE LONDON country: UNITED KINGDOM esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will use the FOS/BL with the G130H grating to measure the line_2: 1150A-1606A range, covering the important lines of N V 1240A, line_3: Si IV 1400A and especially C IV 1550A. We will use the 4.3 arc line_4: second aperture. Spectra will be recorded line_5: repetitively with 15s exposures using FOS RAPID mode, providing line_6: around >8 spectra through the narrow (2-3 minute) orbital eclipse line_7: and many more through the broader `eclipse effect' either side of line_8: it. We are requesting time-critical obervations so that we can line_9: monitor the eclipses in EX Hya that repeat every 98 mins (2 mins line_10: different from the HST orbital period); we are specifying an line_11: eclipse ephemeris so that observations can be centred near the line_12: eclipses. Since the eclipse drifts by 2 minutes relative to the line_13: HST orbital window every HST orbit, we seek a scheduling of two line_14: blocks of 7 contiguous HST orbits to keep the eclipse within line_15: +/- 10 mins of the center of the HST orbital window (first line_16: eclipse in each block should occur towards -10 mins from centre). line_17: This arrangement will also maximise our ability to monitor line_18: the effects of the white dwarf's rotation on the line profiles line_19: outside the eclipses (using data before and after eclipse). ! question: 5 section: 1 line_1: Our primary objective is to obtain detailed, time-resolved UV line_2: spectroscopy through the eclipse in EX Hya. The eclipse lasts line_3: for 2-3 minutes (with an additional maximum of 14 minutes either line_4: side of the main eclipse if the eclipse of the accretion disk line_5: is also considered) and occurs every 98 minutes. We will specify line_6: our constraints via an eclipse ephemeris, requesting observations line_7: throughout the HST (unblocked) orbital window containing the line_8: eclipse (with the eclipse roughly centred in that window). We are line_9: requesting two blocks of 7 contiguous HST orbits so that the line_10: eclipses can be reasonably centred (it drifts by 2 minutes line_11: relative to the window with every HST orbit). This approach will line_12: probably also sample eclipses at a greater range of 67 minute line_13: spin cycle phases. ! question: 6 section: 1 line_1: Routine FOS calibration data will be sufficient for our purposes. ! question: 8 section: 1 line_1: We will be endeavouring to obtain contemporaneous optical line_2: spectroscopy of EX Hya with the HST observations to compare the line_3: behaviour of the UV and optical lines. This may be particularly line_4: useful with regard to searching for ionization structure. However, line_5: we stress that we will arrange these observations to conform to line_6: the HST schedule, i.e. we do NOT need to impose additional line_7: constraints on the HST scheduling. We will apply for observing line_8: time at the 3.9m Anglo Australian telescope or Mount Stromlo line_9: observatory and/or we will arrange observations with collaborators line_10: (D. Buckley, B. Warner) at the South African Astronomical line_11: Observatory. Such arrangements have been very productive in line_12: previous satellite/ground-based simultaneous observations. ! ! !end of general form text general_form_address: lname: ROSEN fname: SIMON mi: R category: PI inst: University of Leicester addr_1: Dept. of Physics, addr_3: University Rd., city: Leicester country: UNITED KINGDOM phone: 0533 552077 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: EX-HYA descr_1: A, 154 pos_1: RA = 12H 52M 24.40S +/- 0.03S, pos_2: DEC = -29D 14' 56.7" +/- 0.4", pos_3: PLATE-ID = 02C8 equinox: J2000 comment_1: MAGNITUDE ERROR IS THE TYPICAL comment_2: VARIATION ABOUT THE MEAN OVER THE comment_3: 67 MINUTE CYCLE. DURING 2 MINUTE comment_4: ECLIPSE, MAGNITUDE MAY REACH ABOUT comment_5: 14. UV FLUXES ARE FROM IUE comment_6: SPECTRA. S/N NEEDED IS AROUND comment_7: 10/PIXEL/SPECTRUM AT C IV PEAK. fluxnum_1: 1 fluxval_1: V = 13.0 +/- 0.4 fluxnum_2: 2 fluxval_2: B-V = 0.1 +/- 0.2 fluxnum_3: 3 fluxval_3: E(B-V) = 0.0 +/- 0.1 fluxnum_4: 4 fluxval_4: F-CONT(1200) = 2.0 +/- 0.7 E-13 fluxnum_5: 5 fluxval_5: F-CONT(1550) = 1.8 +/- 0.7 E-13 fluxnum_6: 6 fluxval_6: F-LINE(1550) = 5.0 +/- 1.5 E-13 fluxnum_7: 7 fluxval_7: W-LINE(1550) = 10 +/- 3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: EX-HYA config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 1S s_to_n: 10 s_to_n_time: 15S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 1.1; req_2: GROUP 1-8 WITH 12H; req_3: CYCLE 4 / 1-16; req_4: AFTER 1-JAN-1995 comment_1: STAR VARIES BY AS MUCH AS 0.4 comment_2: MAGNITUDES ABOUT ITS MEAN comment_3: OF 13.0. IN ECLIPSE (2-3 MINS comment_4: OUT OF THE 98 MIN ORBITAL comment_5: PERIOD) THE STAR MAY DROP TO comment_6: ABOUT MAGNITUDE 14. ! linenum: 1.100 targname: EX-HYA config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G400H num_exp: 1 time_per_exp: 1S s_to_n: 10 s_to_n_time: 15S fluxnum_1: 1 fluxnum_2: 3 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: ONBOARD ACQ FOR 1.2 ! linenum: 1.200 targname: EX-HYA config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G400H num_exp: 1 time_per_exp: 1S s_to_n: 10 s_to_n_time: 15S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SEARCH-SIZE-X=3 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-X=.3 param_4: SCAN-STEP-Y=.3 req_1: ONBOARD ACQ FOR 2-8 ! linenum: 2.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PERIOD 0.068233846D +/- 0.000000005D; req_3: ZERO-PHASE JD2437699.9414 +/- 0.0005D; req_4: PHASE 0.9 +/- 0.06; comment_1: WE SEEK A SCHEDULING THAT PLACES comment_2: ECLIPSES WITHIN +/- 10 MINUTES OF comment_3: THE MID-POINT OF THE UNBLOCKED comment_4: HST ORBITAL WINDOWS, HENCE USE OF comment_5: TWO BLOCKS OF 7 CONTIGUOUS HST comment_6: ORBITS (2-8, 10-16). SEE Q3. ! linenum: 3.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 4.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 5.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 6.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 7.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 8.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 9.000 targname: EX-HYA config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 1S s_to_n: 10 s_to_n_time: 15S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 9.1; req_2: GROUP 9-16 WITHIN 12H; req_3: AFTER 1-JAN-1995 comment_1: STAR VARIES BY AS MUCH AS 0.4 comment_2: MAGNITUDES ABOUT ITS MEAN comment_3: OF 13.0. IN ECLIPSE (2-3 MINS comment_4: OUT OF THE 98 MIN ORBITAL comment_5: PERIOD) THE STAR MAY DROP TO comment_6: ABOUT MAGNITUDE 14. ! linenum: 9.100 targname: EX-HYA config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G400H num_exp: 1 time_per_exp: 1S s_to_n: 10 s_to_n_time: 15S fluxnum_1: 1 fluxnum_2: 3 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: ONBOARD ACQ FOR 10-16 ! linenum: 9.200 targname: EX-HYA config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G400H num_exp: 1 time_per_exp: 1S s_to_n: 10 s_to_n_time: 15S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SEARCH-SIZE-X=3 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-X=.3 param_4: SCAN-STEP-Y=.3 req_1: ONBOARD ACQ FOR 10-16 ! linenum: 10.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; comment_1: WE SEEK A SCHEDULING THAT PLACES comment_2: ECLIPSES WITHIN +/- 10 MINUTES OF comment_3: THE MID-POINT OF THE UNBLOCKED comment_4: HST ORBITAL WINDOWS, HENCE USE OF comment_5: TWO BLOCKS OF 7 CONTIGUOUS HST comment_6: ORBITS (2-8, 10-16). SEE Q3. ! linenum: 11.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 12.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 13.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 14.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 15.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! linenum: 16.000 targname: EX-HYA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 s_to_n_time: 15S fluxnum_1: 6 priority: 1 param_1: COMB=YES param_2: READ-TIME=15 req_1: NON-INT; req_2: PHASE 0.9 +/- 0.06 OF REF2; ! ! end of exposure logsheet