! $Id: 5500,v 5.1 1994/07/27 18:40:47 pepsa Exp $ coverpage: title_1: ENERGY BALANCE AND EMISSION LINES IN DQ HERCULIS STARS title_2: CYCLE 4 - MEDIUM sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO pi_fname: JOSEPH pi_lname: PATTERSON pi_inst: COLUMBIA UNIVERSITY pi_country: USA hours_pri: 6.00 num_pri: 1 fos: Y funds_length: 12 off_fname: BETH off_mi: H. off_lname: ISRAEL off_title: ASSOC. DIRECTOR off_inst: 1770 off_addr_1: OFFICE OF PROJECTS AND GRANTS off_addr_2: 405 LOW MEMORIAL LIBRARY off_addr_3: COLUMBIA UNIVERSITY off_city: NEW YORK off_state: NY off_zip: 10027 off_country: USA off_phone: 212 854 6851 ! end of coverpage abstract: line_1: line_2: The accretion flows onto the magnetic white dwarfs in DQ Herculis line_3: stars are only dimly understood. Rapid rotation of the white dwarfs line_4: is signified by the presence of pulsations, but the flux in the line_5: observed pulses is small compared to that of the disk light, contrary line_6: to theory. We propose to use the continuum channels in the FOS to look line_7: for large-amplitude pulses in the UV light of YY Dra, and thereby line_8: constrain the flux and temperature associated with the accretion bright line_9: spot (presumably beneath the radial accretion shock.) line_11: We also propose to look for a wavelength-dependent phase shift across line_12: the strong UV emission lines, which would be indicative of an line_13: ionizing searchlight beam sweeping in azimuth around the disk. This line_14: would conclusively certify a photoionization origin for the UV lines, line_15: and the phase would decide between origin in an accretion column or a line_16: disk. ! ! end of abstract general_form_proposers: lname: PATTERSON fname: JOSEPH title: PI inst: COLUMBIA UNIVERSITY country: USA ! lname: HASWELL fname: CAROLE mi: A inst: STSCI country: USA ! ! end of general_form_proposers block general_form_text: ! question: 3 section: 1 line_1: We propose 6 hours of FOS observations with the G130H line_2: grating. This will yield ~0.3 ct/s/diode in the continuum, and line_3: we will have ~200 diodes in the continuum from 1350 to 1606 A. line_4: Thus a count rate of ~300 per 6.18s can be achieved, yielding line_5: a S/N ~20 for the summed continuum for each 6.18s data packet. line_7: The dominant optical period is 275 s, suggesting a readout line_8: time of 6.18s will resolve the pulse well. line_10: Most of the emission-line information is likely to come line_11: from the C IV line, which is ~40 A wide, and therefore can line_12: yield ~25 resolution elements. The count rate at line peak line_13: (saturated in the IUE exposure) will be at least 5 ct/s/diode, line_14: or 7.5 ct/s/resolution element. A S/N~12 can be obtained for line_15: each line peak spectral resolution element with a time line_16: resolution of 20s. ! question: 4 section: 1 line_1: A measurement of the pulsed flux at UV wavelengths is line_2: needed to ascertain if the "missing flux" is in the UV/EUV. line_3: Only HST offers the time resolution in the UV. line_5: We have been studying the target stars for ten years line_6: at optical, ultra-violet (IUE), and X-ray (HEAO-1, 2) line_7: wavelengths. We are increasing the density of our optical line_8: coverage, in order to derive unique long-term ephemerides. line_9: We have learned the pulsed fluxes in the intervals 1-100 A line_10: and 3500-7000 A; now we wish to push into the forbidden region line_11: by another factor of 3. line_13: For the emission-line study, it is also the line_14: time-resolution (and sensitivity) of HST/FOS which is line_15: needed. A few similar studies of other stars line_16: have been carried out using hydrogen lines; but these line_17: lines tend to come from EVERYWHERE in the binary, line_18: principally the outer disk which does not line_19: carry information about the inner accretion flows line_20: (and certainly not about the radiation field required line_21: to power the UV emission lines ! question: 4 section: 2 line_1: We need at least one binary orbit (4.0 hrs) of FOS data. line_2: This is principally in order to distinguish the two candidate line_3: periods of 530 s and 550 s, which go out of phase by 360 line_4: degrees in 1 orbit. We are requesting some over-sampling line_5: (to 7.1 hrs) in order to protect against an unfavorable line_6: distribution in orbital phase, which would certainly line_7: clobber the experiment if these two periods could not line_8: be distinguished. line_10: We calculated the expected count rate using the IUE line_11: spectrum in quiescence and the XCAL package at STScI. ! question: 5 section: 1 line_1: No special scheduling requests. We will take responsibility line_2: for obtaining ground-based photometry which is sufficiently line_3: "contemporaneous" to assure correctly phased comparison of line_4: the UV and optical light curves. ! question: 6 section: 1 line_1: N/A ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: No previous data/observing time received. ! question: 10 section: 1 line_1: 1.The analysis of the UV time series will use a battle-tested line_2: set of software written over the last 15 years for optical line_3: photometry. These run on any computer; no special features are needed. line_5: 2. We have official "long-term status" at Cerro Tololo, and line_6: also access to Lick Observatory, which we will use to insure line_7: knowledge of the optical pulse ephemerides. line_9: 3. We hope to use EUVE to detect or set bounds to these stars line_10: at shorter wavelengths. line_12: 4. One graduate student at Columbia will be supported full line_13: time on this project. ! !end of general form text general_form_address: lname: Patterson fname: Joseph category: PI inst: Columbia University addr_1: Dept. of Astronomy addr_2: Columbia University addr_3: 538 West 120th Street city: New York state: NY zip: 10027 country: USA phone: 212 854 3276 telex: 220094 COLU UR ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: YY-DRA name_2: PG-1140+72 name_3: DO-DRA descr_1: A,149,154,906 pos_1: PLATE-ID = 01L3, pos_2: RA = 11H 43M 38.364S +/- 1.0", pos_3: DEC = +71D 41' 20.18" +/- 1.0" equinox: J2000.0 pm_or_par: N comment_1: IN QUIESCENCE comment_2: INCLUDES M DWARF MASS DONOR. comment_3: (B-V)=-0.1 FOR HOT COMPONENT. comment_4: ERROR DUE TO IUE SATURATION comment_5: ERROR INC INTRINSIC VARNS comment_6: OBJECT UNDERGOES RARE DWARF NOVA comment_7: OUTBURSTS: 3WKS PER 10 YEARS. comment_8: IN OUTBURST OBJECT BRIGHTENS BY comment_9: 5 MAGNITUDES. comment_10: T(HOT)~40000K fluxnum_1: 1 fluxval_1: V = 15.65 +/- 0.55 fluxnum_2: 2 fluxval_2: B-V = 0.5 fluxnum_3: 3 fluxval_3: E(B-V) = 0.05 +/- 0.05 fluxnum_4: 4 fluxval_4: F-LINE(1549) = 29 +/- 9 E-13 fluxnum_5: 4 fluxval_5: W-LINE(1549) = 16 +/- 2 fluxnum_6: 5 fluxval_6: F-CONT(1300) = 2 +/- 0.6 E-14 fluxnum_7: 5 fluxval_7: F-CONT(1650) = 1.5 +/- 0.5 E-14 fluxnum_8: 5 fluxval_8: F-CONT(1950) = 1.0 +/- 0.3 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: YYDRA targname: YY-DRA config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 9S fluxnum_1: 5 priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 2 comment_1: VARIABLE STAR comment_2: EXPECT 30% VARNS IN FLUX comment_3: EXP FOR ~10000 COUNTS ! linenum: 2.000 sequence_1: DEFINE sequence_2: YYDRA targname: YY-DRA config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 15S fluxnum_1: 5 priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: ONBOARD ACQ FOR 2.5 comment_1: VARIABLE STAR comment_2: EXPECT 30% VARNS IN FLUX comment_3: EXP FOR ~10000 COUNTS ! linenum: 2.500 sequence_1: DEFINE sequence_2: YYDRA targname: YY-DRA config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 15S fluxnum_1: 5 priority: 1 param_1: SEARCH-SIZE-X=5 param_2: SEARCH-SIZE-Y=5 param_3: SCAN-STEP-X=.172 param_4: SCAN-STEP-Y=.172 req_1: ONBOARD ACQ FOR 3 comment_1: VARIABLE STAR comment_2: EXPECT 30% VARNS IN FLUX comment_3: EXP FOR ~10000 COUNTS ! linenum: 3.000 sequence_1: DEFINE sequence_2: YYDRA targname: YY-DRA config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H wavelength: 1150-1606 num_exp: 1 time_per_exp: 387.898M priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE CHECK WE USE SHORTEST comment_2: READ-TIME ALLOWED FOR 32KHZ comment_3: DATA RATE. TONY KEYES CONFIRMED comment_4: FOS MANUAL PRESCRIPTION INCORRECT comment_5: NO S/N CALC WE OPTIMISE TIME-RES comment_6: PLS INCREASE EXP-TIME TO FILL ORBIT. ! linenum: 4.000 sequence_1: USE sequence_2: YYDRA req_1: CYCLE 4 / 1-4 ; comment_1: TO PERMIT COORDINATED OBSERVATIONS, comment_2: PLEASE NOTIFY P.I. WHEN DATES ARE comment_3: SCHEDULED OR CHANGED. comment_4: RELAX TIMING CONSTRAINT IF REQUIRED comment_5: FOR SCHEDULING. ! ! end of exposure logsheet ! No scan data records found