! File: 3938C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:00:48:59 coverpage: title_1: FUV EMISSION LINE PROFILES OF W SERPENTIS BINARIES: title_2: FUTURE CYCLE CONTINUATION 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 hours_pri: 2.00 num_pri: 2 time_crit: X ! end of coverpage abstract: line_1: We propose to use the HRS at intermediate resolution for the line_2: study of FUV emission line profiles in W Ser and RX Cas line_3: (both are interacting binaries of the W Serpentis type). line_4: The lines of interest are: N V 1240, C II 1335, line_5: Si IV 1400, Si II 1533, and C IV 1550. These lines may be line_6: observed in these binaries with IUE at low dispersion, but line_7: all profile information is lost at this resolution: both of line_8: the listed systems are too faint to be observed at line_9: IUE high dispersion. The emission lines are believed to line_10: arise from a high excitation wind powered by the accretion line_11: process. Modelling of observed line profiles will yield line_12: information about the physical properties of the mass line_13: outflow in these systems, as well as providing insight into line_14: a stage of evolution which many close binaries appear to line_15: 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: Two W Ser systems ( RX Cas, W Ser) will be observed line_2: at medium resolution at five grating settings. We will use line_3: grating 2 (CsTe/MgF2 detector) only, with five grating tilts line_4: with central wavelengths calculated for optimum observation line_5: of N V 1240, C II 1335, Si IV 1400, Si II 1533, and line_6: C IV 1550. A signal to noise ratio of about 3-5 in line_7: the continuum is expected for the exposures. line_8: The observations are to occur post-COSTAR, hence are all line_9: scheduled for Cycle 9. Exposure times are calculated line_10: assuming COSTAR with MgF2+Al. ! question: 4 section: 1 line_1: Both of the W Ser binaries chosen for this proposal are too line_2: faint to be observed with IUE at high dispersion. Although line_3: these systems may be observed with IUE at low dispersion, line_4: all information about the detailed line profile is lost at line_5: this resolution. ! question: 5 section: 1 line_1: Orbital ephemerides for RX Cas will need to be updated prior line_2: to observation. Ephemerides provided will be valid for one line_3: year and will be provided as early in the requested cycle as line_4: possible. line_5: The observations of RX Cas are to be taken at any orbital line_6: phase which falls outside of primary eclipse. The line_7: character of the UV spectrum is essentially unchanged line_8: with orbital phase, but flux levels are higher outside of line_9: primary eclipse. By limiting observations to those outside line_10: of primary eclipse, good data is achieved in less line_11: integration time. line_12: Since the emission line strengths of both W Ser and line_13: RX Cas are known to vary from cycle to cycle, it is line_14: necessary to observe all line profiles for a given system line_15: during a single orbital cycle in order for comparisons line_16: of data within a system to be valid. ! question: 7 section: 1 line_1: The exact nature of the line profiles in the W Ser line_2: systems is unknown. Expectations are that the lines line_3: arise in a high-excitation outflow, in which case line_4: the lines may be P-Cygni in nature and preliminary line_5: analysis of the profiles can be similar to that which line_6: has been performed for profiles observed in the wind line_7: outflows from single O and B stars. Ionization and line_8: velocity structure of the outflow in the W Ser systems line_9: could thus be obtained. However, the two systems chosen line_10: for study exhibit a high degree of mass loss, and thus line_11: the observed line profiles may be more complex than line_12: a simple P-Cygni shape: 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 line_2: will be provided 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 RX Cas and W Ser. line_4: Lines to be studied are N V 1240, C II 1335, Si IV 1400, line_5: Si II 1533 and C IV 1550. The goal of the investigation line_6: is to determine the nature of the emission line profiles, line_7: and to derive physical parameters of the circumstellar line_8: plasma producing these lines. ! !end of general form text general_form_address: lname: BEAVER fname: EDWARD category: PI inst: UC, 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)=1.0+/-.2E-13 ! targnum: 2 name_1: RX-CAS name_2: (GSC4313-0258) descr_1: W SERPENTIS-TYPE INTERACTING BINARY pos_1: RA=03H07M45.801S+/-0.33", pos_2: DEC=+67D34'38.92"+/-0.33", pos_3: PLATE-ID=01MR equinox: 2000 fluxnum_1: 1 fluxval_1: V=9.1+/-0.5 fluxnum_2: 2 fluxval_2: F-CONT(1400)=1.1+/-.2E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 12.000 targname: RX-CAS 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_3: FAINT=240, param_4: LOCATE=YES,PEAKUP=YES, param_5: MAP=END-POINT req_1: ONBOARD ACQ FOR 13; req_2: CYCLE 9 / 12-13; req_3: REQ UPDATE / 12-13 comment_1: EXPECT 1200 CTS/200 MSEC. comment_2: STEP-TIME=0.2 comment_3: SEE GF5 FOR UPDATE INFO. ! linenum: 13.000 targname: RX-CAS config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1400 num_exp: 4 time_per_exp: 8.5M s_to_n: 3 fluxnum_1: 2 priority: 2 param_1: STEP-PATT=5 req_1: PHASE 0.50+/-0.35; req_2: PERIOD 32.33010D+/-0.00005D; req_3: ZERO-PHASE JD2446827.389+/-0.008D comment_1: RX CAS, OUTSIDE OF PRIMARY ECLIPSE. ! linenum: 18.000 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: 1 param_1: SEARCH-SIZE=5, param_3: FAINT=1000, param_4: LOCATE=YES,PEAKUP=YES, param_5: MAP=END-POINT req_1: ONBOARD ACQ FOR 19-22; req_2: CYCLE 9/18-22 comment_1: EXPECT 5000 CTS/200 MSEC. comment_2: STEP-TIME=0.2 ! linenum: 19.000 targname: W-SER config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1243 num_exp: 2 time_per_exp: 9M s_to_n: 3 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 req_1: SEQ 19-22 NO GAP ! linenum: 20.000 targname: W-SER config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1335 num_exp: 2 time_per_exp: 6.0M s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 ! linenum: 21.000 targname: W-SER config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1400 num_exp: 2 time_per_exp: 4.5M s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 ! linenum: 22.000 targname: W-SER config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1538 num_exp: 2 time_per_exp: 2.5M s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 comment_1: W SER, ANY PHASE. ! ! end of exposure logsheet ! No scan data records found