! File: 1190C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:05:19:22 coverpage: title_1: FUV EMISSION LINE PROFILES OF W SERPENTIS BINARIES: title_2: CYCLE 1 OBSERVATIONS sci_cat: STELLAR ASTROPHYSICS proposal_for: GTO/HRS pi_fname: EDWARD pi_lname: BEAVER pi_inst: UC, SAN DIEGO pi_country: USA pi_phone: (619)534-1878 keywords_1: INTERACTING BINARIES - W SERPENTIS - RX CAS - SX CAS hours_pri: 2.02 num_pri: 1 time_crit: X ! end of coverpage abstract: line_1: We propose to use the HRS at intermediate resolution for line_2: the study of FUV emission line profiles in W Serpentis line_3: (which is the prototype of the 'W Serpentis' class of line_4: interacting binaries). The FUV spectrum of the W Ser systems line_5: is characterized by strong emissions at N V 1240, CII 1335, line_6: Si IV 1400, Si II 1533, C IV 1550 and Al II 1670. line_7: In cycle 1, we will concentrate on observations of the line_8: Si IV 1400 doublet in W Ser. Although these lines line_9: may be observed with IUE at low dispersion, all profile line_10: information is lost at this resolution, and the W Ser systems line_11: in general are too faint to be observed at IUE high dispersion. line_12: The emission lines are believed to arise from a high line_13: excitation wind powered by the accretion process. line_14: Modelling of observed line profiles will yield information line_15: about the physical properties of the mass outflow in these line_16: systems, as well as providing insight into a stage of line_17: evolution which many close binaries appear to undergo. ! ! end of abstract general_form_proposers: lname: BEAVER fname: EDWARD inst: UC, SAN DIEGO country: USA ! lname: WEILAND fname: JANET inst: GENERAL SCIENCES CORPORATION country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: In cycle 1, the Si IV emission line in W Ser will line_2: be observed at medium resolution at two specific line_3: orbital phases (phase = 0.0, 0.50). The summary line_4: of observations is as follows: line_5: EXPOSURE LINENUM GRATING WAVELENGTH ORB. PHASE line_6: 2 G160M 1400 0.0 line_7: 4 G160M 1400 0.50 line_8: A signal-to-noise ratio in the continuum of about line_9: 4-5 is expected for the target exposures. ! question: 4 section: 1 line_1: All of the W Ser binaries chosen for this proposal are too faint to be line_2: observed with IUE at high dispersion. Although all of these systems may be line_3: observed with IUE at low dispersion, all information about the detailed line line_4: profile is lost at this resolution. ! question: 5 section: 1 line_1: The observations of W Ser are orbital-phase critical. line_2: Observations both inside and outside of primary eclipse line_3: are desired as a means of isolating whether certain line_4: features of the emission line profile can be directly line_5: associated with the primary component of W Ser. line_6: Since the emission line strengths at a given orbital line_7: phase are known to be highly time-variable, it is line_8: necessary to observe the line profiles during a single line_9: orbital cycle in order to ensure a valid comparison of line_10: the behavior of the profile in and out of eclipse. ! question: 7 section: 1 line_1: The exact nature of the line profiles in the W Ser line_2: systems is unknown. Line profiles will be examined line_3: for changes in the line profile structure as a line_4: function of orbital phase in an attempt to isolate line_5: how much of the emitting volume may be associated with line_6: the primary component. Expectations are that the line_7: lines arise in a high-excitation outflow, in which line_8: case the lines may be P-Cygni in nature and preliminary line_9: analysis of the profiles can be similar to that which line_10: has been performed for profiles observed in the wind line_11: outflows from single O and B stars. Ionization and line_12: velocity structure of the outflow in the W Ser systems line_13: could thus be obtained. However, the line profiles line_14: may be more complex than this: the emissions may line_15: have contributions from more than one source. ! question: 10 section: 1 line_1: Computer resources for the modelling of the line profiles will be provided line_2: by GSC. ! question: 13 section: 1 line_1: The HRS at medium resolution will be used to study line line_2: profiles of the strongest FUV emissions seen in the line_3: W Serpentis systems of SX Cas, RX Cas, and W Ser. line_4: Cycle 1 observations are of the Si IV 1400 doublet line_5: of W Ser, at two different orbital phases. The goal of the line_6: investigation is to determine the nature of the emission line_7: line profiles, and to derive physical parameters line_8: of the circumstellar plasma producing these lines. ! !end of general form text general_form_address: lname: BEAVER fname: EDWARD category: PI inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO addr_1: CASS DEPT., C-011 city: LA JOLLA state: CA zip: 92093 country: USA phone: 619-534-1878 telex: 3-5369 (RAPIFAX) ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: W-SER name_2: (GSC6264-1358) descr_1: W SERPENTIS-TYPE INTERACTING BINARY pos_1: RA=18H09M50.658S +/- 0.33", pos_2: DEC=-15D33'0.17" +/- 0.33", pos_3: PLATE-ID=067F equinox: 2000 fluxnum_1: 1 fluxval_1: V=9.2+/-0.5 fluxnum_2: 2 fluxval_2: F-CONT(1400)=1.1+/-.2E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: W-SER config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 57.8S fluxnum_1: 1 priority: 2 param_1: SEARCH-SIZE=5, param_2: MAP=END-POINT, param_3: FAINT=200, param_4: LOCATE=YES req_1: CYCLE 1 / 1-2; req_2: ONBOARD ACQ FOR 1.1; comment_1: EXPECT 500 CTS/200 MSEC. comment_2: STEP-TIME=0.2 SEC ! linenum: 1.100 targname: W-SER config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 73.6S fluxnum_1: 1 priority: 2 req_1: ONBOARD ACQ FOR 1.2; comment_1: EXP= 46*STEP_TIME, comment_2: STEP-TIME=1.6 SEC RE KGC ! linenum: 1.200 targname: W-SER config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 53.0S fluxnum_1: 1 priority: 2 param_1: SEARCH-SIZE=1, param_2: MAP=END-POINT, param_3: LOCATE=NO, param_4: FAINT=0 req_1: ONBOARD ACQ FOR 2; comment_1: TAKE LSA MAP AFTER CENTERING comment_2: 200 MSEC INTEGRATIONS ! linenum: 2.000 targname: W-SER config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1400 num_exp: 4 time_per_exp: 9M s_to_n: 4 fluxnum_1: 2 priority: 2 param_1: STEP-PATT=5 req_1: PHASE 0.00+/-0.01; req_2: PERIOD 14.1683D+/-0.0030D; req_3: ZERO-PHASE JD2443646.658D+/-0.050D comment_1: W-SER, PRIMARY ECLIPSE ! linenum: 3.000 targname: W-SER config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 57.8S fluxnum_1: 1 priority: 2 param_1: SEARCH-SIZE=5, param_2: MAP=END-POINT, param_3: FAINT=240, param_4: LOCATE=YES req_1: CYCLE 1 / 3-4; req_2: ONBOARD ACQ FOR 3.1; comment_1: EXPECT 600 CTS/200 MSEC. comment_2: STEP-TIME=0.2 SEC ! linenum: 3.100 targname: W-SER config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 73.6S fluxnum_1: 1 priority: 2 req_1: ONBOARD ACQ FOR 3.2; comment_1: EXP= 46*STEP_TIME, comment_2: STEP-TIME=1.6 SEC RE KGC ! linenum: 3.200 targname: W-SER config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 53.0S fluxnum_1: 1 priority: 2 param_1: SEARCH-SIZE=1, param_2: MAP=END-POINT, param_3: LOCATE=NO, param_4: FAINT=0 req_1: ONBOARD ACQ FOR 4; comment_1: TAKE LSA MAP AFTER CENTERING comment_2: 200 MSEC INTEGRATIONS ! linenum: 4.000 targname: W-SER config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1400 num_exp: 4 time_per_exp: 9M s_to_n: 4 fluxnum_1: 2 priority: 2 param_1: STEP-PATT=5 req_1: AFTER 2 BY 7.0D+/-0.3D comment_1: W-SER, PHASE 0.5 ! ! end of exposure logsheet ! No scan data records found