! File: 4945C.PROP
! Database: PEPDB
! Date: 23-FEB-1994:11:46:32
coverpage:
title_1: PERIODIC VARIATIONS IN DQ HERCULIS STARS - CYC2HIGH
sci_cat: STELLAR ASTROPHYSICS
sci_subcat: SUBLUMINOUS STARS
proposal_for: GTO/HSP
cont_id: 1090
pi_fname: ROBERT
pi_mi: C.
pi_lname: BLESS
pi_inst: WISCONSIN, UNIVERSITY OF
pi_country: USA
pi_phone: (608) 262-1715
keywords_1: CATACLYSMIC VARIABLE STARS
hours_pri: 5.67
num_pri: 9
! end of coverpage
abstract:
line_1: The DQ Herculis Stars are cataclysmic variables
line_2: showing rapid, strictly periodic luminosity
line_3: variations at either optical or X-ray wavelengths,
line_4: and usually both. The periods range from 33 sec in
line_5: AE AQR through 71 sec in DQ Her to 18690 sec in TV
line_6: Col. The cataclysmic variables are all close binary
line_7: stars consisting of a late-type star transferring
line_8: mass to its companion white dwarf star. The white
line_9: dwarf in the DQ Her stars is magnetized. The
line_10: periodicities of the DQ Her stars are caused by
line_11: rotation of the magnetized, acreting white dwarf. We
line_12: propose to observe the DQ Her stars at ultraviolet
line_13: wavelengths using the high speed photometer on the
line_14: space telescope. The purpose of the observations is
line_15: to investigate the physics of accretion onto compact
line_16: stars. Revision History: Received on RPS 9/1/89;
line_17: Added to SCCS 9/5/89 RPSS V7.2 remote & local; Typos
line_18: corrected; Added data-fmt - SALM 9/7/89 Updated text
line_19: - SALM 9/28/89; Moved 5 targ to cycle 2 - SALM
line_20: 2/12/90 Switched 1 targ in cycles 1 & 2 - SALM
!
! end of abstract
general_form_proposers:
lname: WHITE
fname: RICHARD
mi: L.
inst: SPACE TELESCOPE SCIENCE INSTITUTE
country: USA
!
lname: BLESS
fname: ROBERT
mi: C.
inst: WISCONSIN, UNIVERSITY OF
country: USA
!
lname: DOLAN
fname: JOSEPH
mi: F.
inst: NASA, GODDARD SPACE FLIGHT CENTER
country: USA
!
lname: ELLIOT
fname: JAMES
mi: L.
inst: MASSACHUSETTS INSTITUTE OF TECHNOLOGY
country: USA
!
lname: ROBINSON
fname: EDWARD
mi: L.
inst: TEXAS, UNIVERSITY OF
country: USA
!
lname: VAN CITTERS
fname: G.
mi: W.
inst: NATIONAL SCIENCE FOUNDATION
country: USA
!
! end of general_form_proposers block
general_form_text:
question: 3
section: 1
line_1: The phases and amplitudes of the pulsations of the
line_2: DQ Her stars usually vary with orbital phase. It is
line_3: critically important to know how they vary to
line_4: interpret the pulsations properly. Observations over
line_5: at least one entire orbit are necessary to define
line_6: these variations, and, since each star is different,
line_7: all the stars should be observed. Therefore, we will
line_8: observe each of the DQ Her stars (except AE Aqr,
line_9: whose orbital period is exceptionally long) for a
line_10: length of time equal to one orbital period. The
line_11: total observing time will be 35 hours. The
line_12: appropriate filters to use are the continuum filters
line_13: at 1350 A and 2400 A in the prism pair of filters,
line_14: and the appropriate integration times are 1/2 second
line_15: per pair. Cycle 0: 1 Cycle 1: remainder
!
question: 4
section: 1
line_1: The periodic variations exhibited by the DQ Herculis
line_2: stars in the optical regime may be of a
line_3: substantially larger amplitude in the ultraviolet
line_4: region accessible for ST. The funneling of the
line_5: accretion flows onto the magnetic poles produces
line_6: regions which are substantially hotter, and thus
line_7: more luminous, in the ultraviolet than accretion
line_8: processes in the absence of fields. The ultraviolet
line_9: photometry may also actually detect the presence of
line_10: the underlying white dwarf as well.
!
question: 13
section: 1
line_1: A program of high speed ultraviolet photometry of
line_2: the DQ Herculis stars (the intermediate polars) is
line_3: proposed to search for the ultraviolet counterparts
line_4: of the rapid, periodic variations previously seen in
line_5: the optical and X-ray regions. The observations will
line_6: help to outline the process of viscous accretion in
line_7: the presence of strong magnetic fields.
!
!end of general form text
general_form_address:
lname: ROBINSON
fname: EDWARD
mi: L.
category: CON
inst: UNIVERSITY OF TEXAS
addr_1: DEPARTMENT OF ASTRONOMY
city: AUSTIN
state: TX
zip: 78712
country: USA
phone: (512) 471-3401
!
lname: BLESS
fname: ROBERT
mi: C.
category: PI
inst: UNIVERSITY OF WISCONSIN
addr_1: WASHBURN OBSERVATORY
addr_2: 475 N. CHARTER STREET
city: MADISON
state: WI
zip: 53706
country: USA
phone: (608) 262-1715
!
! end of general_form_address records
fixed_targets:
targnum: 1
name_1: DQ-HER
descr_1: VARIABLE STAR
descr_2: INTERACTING BINARY
pos_1: RA = 18H 7M 30.22S +/- .5",
pos_2: DEC = +45D 51' 30.9" +/- .5"
equinox: 2000
pm_or_par: NO
plate_req: NO
comment_1: POSREF = ROBINSON
fluxnum_1: 1
fluxval_1: V = 16 +/- 1
!
! end of fixed targets
! No solar system records found
! No generic target records found
exposure_logsheet:
linenum: 1.500
targname: DQ-HER
config: HSP/UV1
opmode: ACQ
num_exp: 1
time_per_exp: 72S
fluxnum_1: 1
priority: 2
param_1: DATA-FORMAT=WORD,
req_1: ONBOARD ACQUISITION FOR 2;
req_2: CYCLE 3 / 1.5-2;
req_3: PCS MODE FINE / 1.500-2.000;
!
linenum: 2.000
targname: DQ-HER
config: HSP/UV1
opmode: SINGLE
aperture: 1.0
sp_element: F220W
num_exp: 1
time_per_exp: 4.7H
fluxnum_1: ^
priority: ^
param_1: SAMPLE-TIME=0.07,
comment_1: FOR LINES 1.5-2, GAPS DUE TO EARTH
comment_2: OCCULTATION SHOULD BE MINIMIZED.
!
! end of exposure logsheet
! No scan data records found