! 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