! $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