! File: 4801C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:04:05:39 coverpage: title_1: QUASI-PERIODIC OSCILLATIONS IN AM HERCULIS BINARIES-- title_2: REPEAT FOR HOPR#87/95 sci_cat: STELLAR ASTROPHYSICS sci_subcat: ERUPTIVE BINARIES proposal_for: RPT/GO cont_id: 3607 pi_title: DR pi_fname: GANESAR pi_lname: CHANMUGAM pi_inst: LOUISIANA STATE UNIVERSITY pi_country: USA pi_phone: 504-388-6849 hours_pri: 4.30 num_pri: 4 hsp: Y time_crit: Y funds_amount: 88000 funds_length: 12 pi_position: DR ! end of coverpage abstract: line_1: AM Her variables are close-binary systems in which a line_2: white dwarf with a magnetic field of 20--70 MG accretes matter line_3: from a companion star. Theoretical studies of magnetically line_4: channeled accretion flows in such systems predict that the line_5: shock formed near the white dwarf should oscillate with line_6: periods of order 0.1--1 s. Optical high-speed photometry has line_7: indeed shown the existence of such rapid, quasi-periodic line_8: oscillations in some AM Her binaries, but not in others. We line_9: will use HST to obtain ultraviolet high-speed line_10: photometry of several AM Her systems, in order to explore line_11: further the nature of the oscillations, and to extend the line_12: search into the UV. HSP observations of two systems (VV Pup line_13: and ST LMi, in which the accreting magnetic pole periodically line_14: passes behind the limb of the white dwarf) will allow detailed line_15: eclipse mapping of the accretion column and the shock line_16: oscillations to be carried out. ! ! end of abstract general_form_proposers: lname: CHANMUGAM fname: GANESAR title: DR inst: LOUISIANA STATE UNIVERSITY country: USA ! lname: BOND fname: HOWARD title: DR mi: E inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: (See original proposal for Scientific Justification) ! question: 3 section: 1 line_1: We will use the HSP to obtain broad-band ultraviolet photometry, line_2: with the aim of searching for high-frequency oscillations line_3: predicted to arise in the magnetic accretion columns of AM Her line_4: binaries. Since the predicted timescales are 0.1-1 sec, we will use line_5: an integration time of 0.01 sec for all of line_6: the observations. Two systems (EF Eri and VV Pup) have already shown line_7: oscillations in the optical, and will be observed with HST in order line_8: to characterize the oscillations in the UV. The remaining two line_9: targets (AM Her and ST LMi) do not show optical oscillations, and we line_10: will test the prediction that they will be found in the UV. line_11: We plan to obtain five photometric runs of 30 min each in length. In line_12: two of the targets, VV Pup and ST LMi, the accretion column is line_13: periodically eclipsed when it passes behind the white dwarf, and the line_14: 30-min runs will be timed to cover an ingress and egress in VV Pup, line_15: and an ingress in ST LMi. The 30-min runs on AM Her and EF Eri can line_16: be at any time. All runs must be continuous (NON-INT). ! question: 4 section: 1 line_1: Theoretical studies predict that shock oscillations with line_2: periods of 0.1-1 sec at X-ray, UV, and optical wavelengths will line_3: occur in the accretion columns in AM Her binaries. The observed line_4: optical oscillations are not coherent, making recovery of the signal line_5: from optical data, inevitably contaminated with atmospheric line_6: scintillation, difficult. High-speed UV photometry cannot be done at line_7: all from the ground or with IUE, making HST a unique choice for line_8: these observations. ! question: 5 section: 1 line_1: We wish to observe critical binary phases for two of the line_2: targets, VV Pup and ST LMi, in which the accretion columns undergo line_3: eclipses. We are requesting timing such that the three 30-min runs are line_4: centered on an ingress and egress of VV Pup, and an ingress of ST line_5: LMi. The other two targets can be observed at any time, since their line_6: accretion columns are always visible. line_7: Note that very accurate timing (+/- a few minutes) is required for line_8: the start times of the 30-min runs on VV Pup and ST LMi. Our time line_9: specifications are in HELIOCENTRIC Julian Dates. line_10: Note also that the ACQUISITION observations of VV Pup and ST LMi are line_11: time-critical. This is because these two objects are bright for line_12: only a fraction of their orbital periods, and faint for the rest of line_13: the orbital period. It is especially important line_14: to avoid the transitions from faint to bright due to the rapidly line_15: changing light level which would ruin the acquisition. ! question: 6 section: 1 line_1: No special calibrations are needed. We do include a S/C line_2: mode parallel observation to assure that the guiding history is line_3: recorded at high data rate, for subsequent attempts at removing line_4: guiding jitter from the data. All five runs must be uninterrupted, line_5: and should avoid terminator crossings to the extent possible. ! question: 7 section: 1 line_1: (see original proposal) ! question: 8 section: 1 line_1: (see original proposal) ! question: 9 section: 1 line_1: (See original proposal) ! question: 10 section: 1 line_1: (See original proposal) ! !end of general form text general_form_address: lname: CHANMUGAM fname: GANESAR category: PI inst: LOUISIANA STATE UNIVERSITY ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: AM-HER name_2: GSC3533-1105 descr_1: A,153,161 pos_1: PLATE-ID=00TB, pos_2: RA = 18H 16M 13.34S +/- 0.7", pos_3: DEC = +49D 52' 04.1" +/- 0.7" equinox: J2000 comment_1: FOR EACH TARGET, V MAGNITUDE GIVEN comment_2: IS MAX. STARS VARY ON TIMESCALES comment_3: OF MINUTES TO MONTHS BY UP TO comment_4: SEVERAL MAGNITUDES. fluxnum_1: 1 fluxval_1: V=12 ! targnum: 2 name_1: EF-ERI name_2: 2A0311-227 name_3: GSC6439-120 descr_1: A,153,161 pos_1: PLATE-ID=027U, pos_2: RA = 03H 14M 13.03S +/- 0.7", pos_3: DEC = -22D 35' 41.3" +/- 0.7" equinox: J2000 comment_1: FOR EACH TARGET, V MAGNITUDE GIVEN comment_2: IS MAX. STARS VARY ON TIMESCALES comment_3: OF MINUTES TO MONTHS BY UP TO comment_4: SEVERAL MAGNITUDES. fluxnum_1: 1 fluxval_1: V=13.7 ! targnum: 3 name_1: ST-LMI name_2: CW1103+253 descr_1: A,153,161 pos_1: PLATE-ID=0256, pos_2: RA = 11H 05M 39.75S +/- 0.7", pos_3: DEC = +25D 06' 28.9" +/- 0.7" equinox: J2000 comment_1: FOR EACH TARGET, V MAGNITUDE GIVEN comment_2: IS MAX. STARS VARY ON TIMESCALES comment_3: OF MINUTES TO MONTHS BY UP TO comment_4: SEVERAL MAGNITUDES. fluxnum_1: 1 fluxval_1: V=15 ! targnum: 4 name_1: VV-PUP descr_1: A,153,161 pos_1: PLATE-ID=01Z4, pos_2: RA = 08H 15M 06.73S +/- 0.7", pos_3: DEC = -19D 03' 16.9" +/- 0.7" equinox: J2000 comment_1: FOR EACH TARGET, V MAGNITUDE GIVEN comment_2: IS MAX. STARS VARY ON TIMESCALES comment_3: OF MINUTES TO MONTHS BY UP TO comment_4: SEVERAL MAGNITUDES. fluxnum_1: 1 fluxval_1: V=14.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: AM-HER config: HSP/UV2 opmode: ACQ num_exp: 1 time_per_exp: 45S fluxnum_1: 1 priority: 1 param_1: DATA-FORMAT=WORD req_1: ONBOARD ACQ FOR 2; req_2: PCS MODE F; req_3: CYCLE 2 ! linenum: 2.000 targname: AM-HER config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 27.37M fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.01, param_2: PRECISION=HIGH req_1: PCS MODE F; req_2: NON-INT; req_3: CYCLE 2 comment_1: OBSERVATION IS VERY SENSITIVE TO comment_2: JITTER; SHOULD BE SCHEDULED TO AVOID comment_3: DAY-NIGHT TRANSITIONS IF POSSIBLE; OR comment_4: TRANSITIONS SHOULD BE AT BEGINNING OR comment_5: END OF EXPOSURE. ! linenum: 2.500 targname: DARK config: S/C opmode: DATA aperture: NONE num_exp: 1 time_per_exp: 1S priority: 1 param_1: FORMAT=FN req_1: PAR WITH 2; req_2: CRIT OBS; req_3: CYCLE 2 comment_1: THE FN FORMAT IS SPECIFIED IN ORDER TO comment_2: ASSURE THAT THE ENGINEERING DATA ARE comment_3: RECORDED AT 32 KBPS, FOR SUBSEQUENT comment_4: ATTEMPTS TO REMOVE GUIDING JITTER FROM comment_5: THE HSP PHOTOMETRY ! linenum: 3.000 targname: EF-ERI config: HSP/UV2 opmode: ACQ num_exp: 1 time_per_exp: 45S fluxnum_1: 1 priority: 1 param_1: DATA-FORMAT=WORD req_1: ONBOARD ACQ FOR 4; req_2: PCS MODE F; req_3: CYCLE 2 ! linenum: 4.000 targname: EF-ERI config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 27.37M fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.01, param_2: PRECISION=HIGH req_1: PCS MODE F; req_2: NON-INT; req_3: CYCLE 2 comment_1: OBSERVATION IS VERY SENSITIVE TO comment_2: JITTER; SHOULD BE SCHEDULED TO AVOID comment_3: DAY-NIGHT TRANSITIONS IF POSSIBLE; OR comment_4: TRANSITIONS SHOULD BE AT BEGINNING OR comment_5: END OF EXPOSURE. ! linenum: 4.500 targname: DARK config: S/C opmode: DATA aperture: NONE num_exp: 1 time_per_exp: 1S priority: 1 param_1: FORMAT=FN req_1: PAR WITH 4; req_2: CRIT OBS; req_3: CYCLE 2 comment_1: THE FN FORMAT IS SPECIFIED IN ORDER TO comment_2: ASSURE THAT THE ENGINEERING DATA ARE comment_3: RECORDED AT 32 KBPS, FOR SUBSEQUENT comment_4: ATTEMPTS TO REMOVE GUIDING JITTER FROM comment_5: THE HSP PHOTOMETRY ! linenum: 5.000 targname: ST-LMI config: HSP/UV2 opmode: ACQ num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 1 param_1: DATA-FORMAT=WORD req_1: ONBOARD ACQ FOR 6; req_2: PCS MODE F; req_3: CYCLE 2; req_4: PHASE 0.375 +/- 0.275; req_5: ZERO-PHASE JD2445059.7024 +/- 0.0003D; req_6: PERIOD 0.07908908D +/- 0.0000008D comment_1: THE ACQUISITION IS DONE DURING THE comment_2: FAINT PHASE OF ST LMI. NOTE THAT THE comment_3: ZERO-PHASE IS GIVEN AS A HELIOCENTRIC comment_4: JULIAN DATE FOR ALL OBSERVATIONS. ! linenum: 6.000 targname: ST-LMI config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 30M fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.01, param_2: PRECISION=HIGH req_1: PCS MODE F; req_2: NON-INT; req_3: CYCLE 2; req_4: PHASE 0.868 +/- 0.050; req_5: ZERO-PHASE JD2445059.7024 +/- 0.0003D; req_6: PERIOD 0.07908908D +/- 0.00000008D comment_1: OBSERVATION IS VERY SENSITIVE TO comment_2: JITTER; SHOULD BE SCHEDULED TO AVOID comment_3: DAY-NIGHT TRANSITIONS IF POSSIBLE; OR comment_4: TRANSITIONS SHOULD BE AT BEGINNING OR comment_5: END OF EXPOSURE. comment_6: THIS IS INGRESS OBSERVATION OF ST LMI. ! linenum: 6.500 targname: DARK config: S/C opmode: DATA aperture: NONE num_exp: 1 time_per_exp: 1S priority: 1 param_1: FORMAT=FN req_1: PAR WITH 6; req_2: CRIT OBS; req_3: CYCLE 2 comment_1: THE FN FORMAT IS SPECIFIED IN ORDER TO comment_2: ASSURE THAT THE ENGINEERING DATA ARE comment_3: RECORDED AT 32 KBPS, FOR SUBSEQUENT comment_4: ATTEMPTS TO REMOVE GUIDING JITTER FROM comment_5: THE HSP PHOTOMETRY ! linenum: 7.000 targname: VV-PUP config: HSP/UV2 opmode: ACQ num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 param_1: DATA-FORMAT=WORD req_1: ONBOARD ACQ FOR 8; req_2: PCS MODE F; req_3: CYCLE 2; req_4: PHASE 0.45 +/- 0.25; req_5: ZERO-PHASE JD2427889.6474 +/- 0.0001D; req_6: PERIOD 0.0697468256D +/- 0.0000000003D comment_1: THE ACQUISITION IS DONE DURING THE comment_2: FAINT PHASE OF VV PUP. NOTE THAT THE comment_3: ZERO-PHASE IS GIVEN AS A HELIOCENTRIC comment_4: JULIAN DATE FOR ALL OBSERVATIONS. ! linenum: 8.000 targname: VV-PUP config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 30M fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.01, param_2: PRECISION=HIGH req_1: PCS MODE F; req_2: NON-INT; req_3: CYCLE 2; req_4: PHASE 0.981 +/- 0.050; req_5: ZERO-PHASE JD2427889.6474 +/- 0.0001D; req_6: PERIOD 0.0697468256D +/- 0.0000000003D comment_1: OBSERVATION IS VERY SENSITIVE TO comment_2: JITTER; SHOULD BE SCHEDULED TO AVOID comment_3: DAY-NIGHT TRANSITIONS IF POSSIBLE; OR comment_4: TRANSITIONS SHOULD BE AT BEGINNING OR comment_5: END OF EXPOSURE. comment_6: THIS IS INGRESS OBSERVATION OF VV PUP. ! linenum: 8.500 targname: DARK config: S/C opmode: DATA aperture: NONE num_exp: 1 time_per_exp: 1S priority: 1 param_1: FORMAT=FN req_1: PAR WITH 8; req_2: CRIT OBS; req_3: CYCLE 2 comment_1: THE FN FORMAT IS SPECIFIED IN ORDER TO comment_2: ASSURE THAT THE ENGINEERING DATA ARE comment_3: RECORDED AT 32 KBPS, FOR SUBSEQUENT comment_4: ATTEMPTS TO REMOVE GUIDING JITTER FROM comment_5: THE HSP PHOTOMETRY ! linenum: 9.000 targname: VV-PUP config: HSP/UV2 opmode: ACQ num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 param_1: DATA-FORMAT=WORD req_1: ONBOARD ACQ FOR 10; req_2: PCS MODE F; req_3: CYCLE 2; req_4: PHASE 0.95 +/- 0.13; req_5: ZERO-PHASE JD2427889.6474 +/- 0.0001D; req_6: PERIOD 0.0697468256D +/- 0.0000000003D comment_1: THE ACQUISITION IS DONE DURING THE comment_2: BRIGHT PHASE OF VV PUP. NOTE THAT THE comment_3: ZERO-PHASE IS GIVEN AS A HELIOCENTRIC comment_4: JULIAN DATE FOR ALL OBSERVATIONS. ! linenum: 10.000 targname: VV-PUP config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 30M fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.01, param_2: PRECISION=HIGH req_1: PCS MODE F; req_2: NON-INT; req_3: CYCLE 2; req_4: PHASE 0.621 +/- 0.050; req_5: ZERO-PHASE JD2427889.6474 +/- 0.0001D; req_6: PERIOD 0.0697468256D +/- 0.0000000003D comment_1: OBSERVATION IS VERY SENSITIVE TO comment_2: JITTER; SHOULD BE SCHEDULED TO AVOID comment_3: DAY-NIGHT TRANSITIONS IF POSSIBLE; OR comment_4: TRANSITIONS SHOULD BE AT BEGINNING OR comment_5: END OF EXPOSURE. comment_6: THIS IS EGRESS OBSERVATION OF VV PUP. ! linenum: 10.500 targname: DARK config: S/C opmode: DATA aperture: NONE num_exp: 1 time_per_exp: 1S priority: 1 param_1: FORMAT=FN req_1: PAR WITH 10; req_2: CRIT OBS; req_3: CYCLE 2 comment_1: THE FN FORMAT IS SPECIFIED IN ORDER TO comment_2: ASSURE THAT THE ENGINEERING DATA ARE comment_3: RECORDED AT 32 KBPS, FOR SUBSEQUENT comment_4: ATTEMPTS TO REMOVE GUIDING JITTER FROM comment_5: THE HSP PHOTOMETRY ! ! end of exposure logsheet ! No scan data records found