! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5817,v 1.1 1994/12/14 19:49:07 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: n/a ! Phone: n/a , E-mail: n/a ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: vrtilek-510.prop ! Date generated: Wed Dec 14 14:49:00 EST 1994 ! Proposal_Information ! Section 4 Title: The UV energy distributions of white dwarfs:, DP Leo, U Gem and OY Car Proposal_Category: AR Scientific_Category: Hot Stars Cycle: 5 Investigators PI_name: Saeqa Vrtilek PI_Institution: University of Maryland CoI_Name: Fuhua Cheng CoI_Institution: University of Maryland Contact: ! Y or N (designate at most one contact) CoI_Name: Keith Horne CoI_Institution: University of Utrecht Contact: ! Y or N (designate at most one contact) CoI_Name: Edward Sion CoI_Institution: Villanova University Contact: ! Y or N (designate at most one contact) CoI_Name: Ivan Hubeny CoI_Institution: NASA Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We have generated a grid of UV energy distributions for white dwarfs in the temperature range between 10,000 to 60,000 K at different high gravities and chemical abundances. These synthetic spectra include the contribution from quasi- molecular interactions of H atoms with H and H^+, seen in all DA stars between 9,000K and 19,000K, and have been applied to WZ Sge and VW Hyi systems (Sion et al. 1994a,b). We have also developed a code to calculate the absorption by intervening disk material that has been successfully applied to the OY Car system (Horne et al. 1994). Our proposed research requests HST archives of DP Leo, we will use our models to determine the temperature, gravity, magnetic field and chemical abundance in the white dwarf photosphere. This has not been done by the original HST project. We will also extend previous work on U Gem and OY Car to study the evolution of white dwarf temperature and chemical abundance between outbursts., Questions ! Free format text (please update) Observing_Description: Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: Target_Name: Alternate_Names: Description: Position: ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: ! Include at least V and B-V Comments: Solar_System_Targets ! Section 5.2 Target_Number: Target_Name: Description: Level_1: ! Satellite of Sun Level_2: ! Satellite of Level_1 Level_3: ! Satellite of Level_2 Window: Flux: ! Include at least V and B-V Comments: Generic_Targets ! Section 5.3 Target_Number: Target_Name: Description: Criteria: Flux: Comments: Scan_Data ! Appendix B Scan_Number: FGS_Scan: Cont_or_Dwell: Dwell_Points: Dwell_Secs: Scan_Width: Scan_Length: Sides_Angle: Number_Lines: Scan_Rate: First_Line_PA: Scan_Frame: Length_Offset: Width_Offset: ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: Visit_Requirements: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ! ORIENTation TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN