! $Id: 81,v 37.1 1995/06/09 12:31:55 pepsa Exp $ coverpage: title_1: THE BOUNDARY LAYER-WHITE DWARF CONNECTION: CV WHITE DWARF ROTATION AND title_2: LINE FORMATION REGIONS IN THE PROTOTYPE DWARF NOVA U GEMINORUM sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO targ_of_opp: Y pi_fname: EDWARD pi_mi: M pi_lname: SION pi_inst: VILLANOVA UNIVERSITY pi_country: USA pi_phone: 216 519 7702 hours_pri: 4.50 num_pri: 1 hrs: Y time_crit: Y off_fname: WALTER off_lname: ZACHARIAS off_title: ASST.VP FOR RESEARCH off_addr_1: VILLANOVA UNIVERSITY off_addr_2: OFFICE OF RESEARCH AND SPONSORED PROJECTS off_city: VILLANOVA off_state: PA off_zip: 19085 off_country: USA off_phone: 215 519 4220 ! end of coverpage abstract: line_1: The central accreting object in compact binaries and other accreting systems is line_2: usually hidden from direct observation, enshrouded by optically thick accretion line_3: disks which are opaque to the radiation emitted by the central object as it line_4: accretes matter. In the dwarf nova U Gem the underlying white dwarf accreter is line_5: clearly exposed in the far UV during dwarf nova quiescence. By probing the white line_6: dwarf with the sensitivity and velocity resolution of GHRS, just after the line_7: deposition of mass, energy and angular momentum into its envelope by the dwarf line_8: nova outburst event and also later in quiescence, we will obtain fundamental line_9: information such as: (1) the first rate of rotation of a CV white dwarf and line_10: hence the expected temperature and extent of the boundary layer during the high line_11: accretion (dwarf nova outburst) episode; (2) the delineation of the lower line_12: temperature line formation regions associated with the rotating, average line_13: (30-40,000K), photosphere of the white dwarf from the line formation region(s) line_14: of higher temperature ion species (e.g. NV 1238,1242) (boundary layer/accretion line_15: belt or putative hot corona\?) surrounding the white dwarf; (3) the velocity line_16: amplitude and hence mass and gravitational redshift of the U Gem white dwarf; line_17: (4) the possible presence of persisting (but weaker in quiescence) radiation- line_18: driven selective ion wind (5) line profile variations to test physical mech- line_19: anisms that control the flow of accreted elements and hence abundance changes line_20: (diffusion, mixing, dilution, dredgeup and ongoing accretion during quiescence). ! ! end of abstract general_form_proposers: lname: SION fname: EDWARD mi: M inst: VILLANOVA UNIVERSITY country: USA ! lname: HUANG fname: MIN inst: VILLANOVA UNIVERSITY country: USA ! lname: SZKODY fname: PAULA inst: UNIVERSITY OF WASHINGTON country: USA ! lname: LONG fname: KNOX mi: S inst: STSCI country: USA ! lname: HORNE fname: KEITH inst: UTRECHT country: NETHERLANDS esa: Y ! lname: SPARKS fname: WARREN mi: M inst: LANL country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will obtain high quality UV spectra of the exposed white dwarf line_2: in the prototype dwarf nova U Geminorum at two epochs during dwarf line_3: nova quiescence, 7-21 days post-outburst and 90-110 days post-outburst. line_4: we are primarily interested in securing detailed line profiles, line line_5: velocities to within 50 km/s and the detection of weak features. line_6: We will cover three regions containing diagnostic high temperature and line_7: low temperature ions, 1220 to 1255, 1270-1305, and 1615-1650 line_8: We will utilize side 2 of GHRS, G160M, LSA, S/N=15/diode, =60/Angstrom line_9: resolution = 0.07 Angstrom/diode. We will use the Accumulation mode. ! question: 4 section: 1 line_1: No other telescope is capable of observing this faint (V=14.5) line_2: object at high spectral resolution and S/N in the UV when it is in line_3: quiescence. This experiment is impossible with any other telescope and line_4: requires the large HST mirror and GHRS sensitivity and wavelength line_5: (velocity) resolution capabilities in order to explore the physics line_6: described in this proposal. ! question: 5 section: 1 line_1: We need time critical observations for U Gem in the sense of line_2: obtaining spectra just after the last dwarf nova outburst and just line_3: before the next outburst so as to sample line variations over the widest line_4: possible span of time. We need a spectrum 7-21 days after an outburst line_5: and 90 -110 days after an outburst. The outbursts are statistically line_6: very well-characterized by AAVSO and very predictable. We will notify STScI once line_7: an outburst occurs and will expect a spectrum 15-25 days after outburst. We are line_8: in close working communication with Janet Mattei (Director of AAVSO) concerning line_9: the outbursts of U Gem which occur every 90-120 days. ! ! ! question: 10 section: 1 line_1: Workstations, IBM Mainframe and VAXes at Villanova, line_2: Supercomputer facilities at LANL, Workstations at STScI, line_3: Workstations at the University of Washington ! !end of general form text general_form_address: lname: Sion fname: Edward mi: M category: PI inst: Villanova University addr_1: Department of Astronomy and Astrophysics addr_2: Villanova University city: Villanova state: PA zip: 19085 country: USA phone: 215 519 7702 telex: EMSION@VUVAXCOM.bitnet ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: U-GEM descr_1: A,149,161 pos_1: RA = 07H 55M 05.29S +/- 0.15S, pos_2: DEC = +22D 00' 05.67" +/- 0.15", pos_3: PLATE-ID=02UF, equinox: 2000 fluxnum_1: 1 fluxval_1: V=14.5 +/-0.1, B-V=+0.00 +/- 0.05 fluxnum_2: 2 fluxval_2: F-CONT(1300) = 5 +/- 1 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: U-GEM config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S s_to_n: 15 s_to_n_time: 25S fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE=5,BRIGHT=RETURN req_1: ONBOARD ACQ FOR 2-5; req_2: CYCLE 4;TARG OF OPP; req_3: PERIOD 0.1769061911D +/- 0.0000000004D; req_4: ZERO-PHASE JD2437638.82325 +/- 0.001D; comment_1: EXECUTE WITHIN 7-21 DAYS AFTER PI comment_2: REQUEST TO ACTIVATE THESE EXPOSURES. ! linenum: 2.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1220-1255 num_exp: 130 time_per_exp: 13.6s s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; req_3: PHASE 0.25 +/- 0.02 OF REF 1; ! linenum: 3.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1270-1305 num_exp: 130 time_per_exp: 13.6S s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; ! linenum: 4.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1615-1650 num_exp: 130 time_per_exp: 13.6S s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; ! linenum: 5.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1615-1650 num_exp: 30 time_per_exp: 13.6S s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; ! linenum: 11.000 targname: U-GEM config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S s_to_n: 15 s_to_n_time: 25S fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE=5,BRIGHT=RETURN req_1: ONBOARD ACQ FOR 12-15; req_2: CYCLE 4;TARG OF OPP; req_3: AFTER 4 BY 150D +/- 15D; req_4: PERIOD 0.1769061911D +/- 0.0000000004D; req_5: ZERO-PHASE JD2437638.82325 +/- 0.001D; ! linenum: 12.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1220-1255 num_exp: 130 time_per_exp: 13.6S s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; req_3: PHASE 0.75 +/- 0.02 OF REF 11; ! linenum: 13.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1270-1305 num_exp: 130 time_per_exp: 13.6S s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; ! linenum: 14.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1615-1650 num_exp: 130 time_per_exp: 13.6S s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; ! linenum: 15.000 targname: U-GEM config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1615-1650 num_exp: 30 time_per_exp: 13.6S s_to_n: 15 s_to_n_time: 45M fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CYCLE 4;TARG OF OPP; req_2: NON-INT; ! ! end of exposure logsheet ! No scan data records found