! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6493,v 7.1 1996/04/17 17:27:43 pepsa Exp $ ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Karla Peterson ! Phone: 410-338-4774 , E-mail: peterson@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. Proposal_Information ! Section 4 Title: Accretion in the Interacting Binary UX Monocerotis Proposal_Category: GO Scientific_Category: BINARIES AND STAR FORMATION Cycle: 6 Investigators PI_name: Mirek Plavec PI_Institution: University of California CoI_Name: Ivan Hubeny CoI_Institution: USRA, NASA Goddard Space Flight Center, Greenbelt Contact: N ! Y or N (designate at most one contact) CoI_Name: Charles Keyes CoI_Institution: Space Telescope Science Institute Contact: N ! Y or N (designate at most one contact) CoI_Name: Geraldine Peters CoI_Institution: University of Southern California, Los Angeles Contact: N ! Y or N (designate at most one contact) CoI_Name: Steven Shore CoI_Institution: Indiana University at South Bend Contact: N ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We plan to use the GHRS spectrograph in order to obtain high-S/N UV spectra in two segments at three orbital phases of the interacting binary UX Monocerotis. This system is an intermediate case between the weakly interacting ordinary Algols and the strongly interacting W Serpentis systems (``hyperactive Algols''). This means that the rate of mass transfer is rather high to produce observable effects, yet the component stars are not completely obscured by the circumstellar matter, so that the fundamental parameters of the binary system are known. As such, UX Mon offers a rare opportunity to study mass transfer processes in interacting binaries: the mass-transfering stream, the impact region on the gainer, the ``splashed'' disk, and the outflowing stream or induced wind. These phenomena can be studied by analyzing and modeling suitably selected emission (and absorption) lines observed from different points of view, i.e. at several orbital phases. A recent study of W Serpentis suggests two emitting regions: the impact area and the disk boundary layer. In UX Mon, we can study these regions much more quantitatively, since the system parameters are much better defined and known. For analysis and modeling we have excellent programs, considerable experience, and extensive supporting data, photometric as well as spectroscopic. Questions ! Free format text (please update) Observing_Description: We plan to observe UX Mon with the GHRS LSA and the G160M grating in two regions centered at 1400 Angstrom (Si IV), and 1540 Angstrom (C IV, Si II), at 0.07 Angstrom spectral resolution. We will achieve a S/N of 25 or better per diode in each spectral range. These observations should be executed three times at different orbital phases. It is essential, if at all possible, to execute all observations within the same orbital cycle of 5.9 days. The observing sequence in each visit will be identical and will utilize a total exposure time of 38 minutes at the 1400 Angstrom setting, and a single 20 minute ACCUM at the 1540 Angstrom setting. Given the UX Mon 52-minute visibility period, HRS ACCUM overheads, and the GIM-related 20-minute exposure limit, our observing sequence allows one 20-minute science exposure in the acquisition orbit and two exposures (totalling 38 minutes) in each succeeding orbit as follows: acquisition orbit: GS ACQ (8m); LSA ACQ (11m); O/H (4m); G160M (1540 Angstrom) ACCUM (20m) second orbit: GS re- ACQ (6m); O/H (4m); G160M (1400 Angstrom) ACCUM (20m); O/H (4m); G160M (1400 Angstrom) ACCUM (18m). Two orbits and 3 individual exposures will be needed for each visit, hence our program requires 6 orbits and will obtain 9 exposures. The representative continuum flux over the entire spectral range to be observed is 4.e-13 erg/sec/cm**2/Angstrom; so a typical calculation shows that for this flux level at 1380 Angstrom, we will obtain 0.26 counts per diode per sec such that in 2280 sec (38 min), we expect about 590 counts or a S/N of 24 per diode. No special calibrations are needed for our observations. Real_Time_Justification: Observations should be executed three times at different orbital phases, preferably within the same orbital cycle of 5.9 days; ideally, the first observation should start about 3.0 days after the mid-eclipse, defined by the ephemeris: T(mid-ecl) = HJD 243329.00 + 5.9045505 * E. The second observation should be made 1.0 days later, and the third should follow after another 1.0 days. In other words, the observations should be made at orbital phases near 0.51 P, 0.68 P, and 0.85 P. The actual timing should lie within +/- 0.2 days of the times indicated above. It is important to execute the observations within one orbital cycle, or over two adjacent orbital cycles, since the object undergoes fairly large flux variations from cycle to cycle. Fixed_Targets ! Section 5.1 Target_Number:1 Target_Name:HD65607 Alternate_Names:UX-MON,SAO135333,PPM190848,GSC5412-305 Description:STAR,A0-A3 V-IV,INTERACTING BINARY,ALGOL SYSTEM Position: RA=07H 59M 16.365S +/-0.05S, DEC=-07D 30' 18.04" +/-0.1", PLATE-ID=03VY Equinox:J2000 RV_or_Z:V=-3 RA_PM:-0.0005 Dec_PM:-0.001 Epoch:1983.5 Annual_Parallax:0.00 Flux: V=8.2 B-V=0.03 TYPE=A2IV E(B-V)=0.00 A(V)=0.0 F-CONT(1540)=4+/-1 E-13 F-CONT(1400)=4+/-1 E-13 F-LINE(1550)=15+/-2 E-13 F-LINE(1403)=16+/-2 E-13 Comments:ECLIPSING BINARY, BUT WILL BE OBSERVED OUTSIDE ECLIPSE, THUS BRIGHTNESS VARIATIONS ARE NOT LARGE TARGET COORDINATES ARE GSC VALUES. (Hipparcos coord differ by .006 sec in RA (~.09 arcsec) and .44 arcsec in DEC. We do not see any need to change the values on the basis of these modest differences.) Visits ! Section 6 Visit_Number: 01 Visit_Requirements: PERIOD 5.9045505D AND ZERO-PHASE JD2433329.00 SEQ 1-3 WITHIN 3.0D On_Hold_Comments: Visit_Comments: Exposure_Number: 1 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N2 Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1.8S Special_Requirements: ONBOARD ACQ FOR 100-200 ! Section 7.2 Comments: STEP-TIME assumed to be .2 seconds for 3x3 search. Exposure_Number: 100 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G160M Wavelength: 1550 Optional_Parameters: FP-SPLIT=FOUR Number_of_Iterations: 1 Time_Per_Exposure: 1632S Special_Requirements: PHASE 0.50 TO 0.53 NO SPLIT Exposure_Number: 200 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G160M Wavelength: 1400 Optional_Parameters: FP-SPLIT=FOUR Number_of_Iterations: 2 Time_Per_Exposure: 1196.8S Special_Requirements: NO SPLIT Comments: Visit_Number: 02 Visit_Requirements: PERIOD 5.9045505D AND ZERO-PHASE JD2433329.00 On_Hold_Comments: Visit_Comments: Exposure_Number: 1 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N2 Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1.8S Special_Requirements: ONBOARD ACQ FOR 100-200 ! Section 7.2 Comments: STEP-TIME assumed to be .2 seconds for 3x3 search. Exposure_Number: 100 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G160M Wavelength: 1550 Optional_Parameters: FP-SPLIT=FOUR Number_of_Iterations: 1 Time_Per_Exposure: 1632S Special_Requirements: PHASE 0.67 TO 0.70 NO SPLIT Exposure_Number: 200 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G160M Wavelength: 1400 Optional_Parameters: FP-SPLIT=FOUR Number_of_Iterations: 2 Time_Per_Exposure: 1196.8S Special_Requirements: NO SPLIT ! Section 7.2 Comments: Visit_Number: 03 Visit_Requirements: PERIOD 5.9045505D AND ZERO-PHASE JD2433329.00 On_Hold_Comments: Visit_Comments: Exposure_Number: 1 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N2 Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1.8S Special_Requirements: ONBOARD ACQ FOR 100-200 ! Section 7.2 Comments: STEP-TIME assumed to be .2 seconds for 3x3 search. Exposure_Number: 100 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G160M Wavelength: 1550 Optional_Parameters: FP-SPLIT=FOUR Number_of_Iterations: 1 Time_Per_Exposure: 1632S Special_Requirements: PHASE 0.84 TO 0.87 ! Section 7.2 NO SPLIT Exposure_Number: 200 ! Section 6.5 Target_Name: HD65607 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G160M Wavelength: 1400 Optional_Parameters: FP-SPLIT=FOUR Number_of_Iterations: 2 Time_Per_Exposure: 1196.8S Special_Requirements: NO SPLIT ! Section 7.2 Comments: Data_Distribution Medium: 8MM Blocking_Factor: 10 Ship_To: PI_Address Ship_Via: UPS Recipient_Email: