! File: 2485C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:07:12:09 coverpage: title_1: SLEUTHING THE DYNAMO: CYCLE 1 OBSERVATIONS sci_cat: STELLAR ASTROPHYSICS sci_subcat: EARLY EVOLUTION proposal_for: GO longterm: 2 pi_title: DR. pi_fname: THOMAS pi_mi: R. pi_lname: AYRES pi_inst: COLORADO, UNIVERSITY OF pi_country: USA pi_phone: 303-492-4051 keywords_1: OPEN CLUSTER, DWARF, MS STAR, CHROMOSPHERE, CORONA hours_pri: 6.00 num_pri: 5 hrs: Y funds_amount: 97000 funds_length: 12 funds_date: JUL-90 pi_position: RESEARCH PROFESSOR off_fname: LAURENCE off_lname: NELSON off_title: DIRECTOR off_inst: UNIVERSITY OF COLORADO off_addr_1: OFFICE OF CONTRACTS AND GRANTS off_addr_2: CAMPUS BOX B-19 off_city: BOULDER off_state: CO off_zip: 80309 off_country: USA off_phone: 303-492-2695 ! end of coverpage abstract: line_1: Innovative technologies of the 1990s will open new windows line_2: to the interior of the Sun and its hidden dynamics: the GONG line_3: project for helioseismology; rare-earth detectors for solar line_4: neutrinos; and SOLAR PROBE for high-order moments of the mass line_5: distribution. At the same time, newly-commissioned space line_6: observatories will provide unprecedented views of the vacuum-UV line_7: and X-ray emissions of stars in our Galactic neighborhood. These line_9: seemingly unrelated developments are in fact deeply connected. A line_10: central issue of solar-stellar physics is the nature and origin line_11: of magnetic activity: the profound link between the interior line_12: dynamics of a late-type star and the violent state of its line_13: outermost million-degree coronal layers. As solar physicists are line_14: unlocking the secrets of the hydromagnetic dynamo deep inside the line_15: Sun, we will apply one of the powerful new astronomical tools of line_16: the decade -- the HST -- to document the early evolution of the line_17: dynamo and its associated external gas-dynamic activity. In line_18: particular, we will obtain high-S/N FUV spectra of solar-type line_19: stars in young galactic clusters ranging in age from 1/10-th line_20: to 1/100-th that of the Sun. ! ! end of abstract general_form_proposers: lname: AYRES fname: THOMAS title: DR. mi: R. inst: COLORADO, UNIVERSITY OF country: USA ! lname: BASRI fname: GIBOR title: PROF. mi: S. inst: CALIFORNIA, UNIVERSITY OF, BERKELEY country: USA ! lname: SIMON fname: THEODORE title: DR. inst: HAWAII, UNIVERSITY OF country: USA ! lname: STAUFFER fname: JOHN title: DR. mi: R. inst: CFA country: USA ! lname: STERN fname: ROBERT title: DR. mi: A. inst: LOCKHEED PALO ALTO RESEARCH LABS country: USA ! lname: ANTIOCHOS fname: SPIRO title: DR. mi: K. inst: US NAVAL RESEARCH LABORATORY country: USA ! lname: BOOKBINDER fname: JAY title: DR. mi: A. inst: CFA country: USA ! lname: BROWN fname: ALEXANDER title: DR. inst: COLORADO, UNIVERSITY OF country: USA ! lname: DOSCHEK fname: GEORGE title: DR. mi: A. inst: US NAVAL RESEARCH LABORATORY country: USA ! lname: LINSKY fname: JEFFREY title: DR. mi: L. inst: COLORADO, UNIVERSITY OF country: USA ! lname: RAMSEY fname: LAWRENCE title: PROF. mi: W. inst: PENN STATE UNIVERSITY country: USA ! lname: WALTER fname: FREDERICK title: PROF. mi: M. inst: NEW YORK, STATE UNIVERSITY OF (STONY BROOK) country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: 2. Scientific Justification line_3: ==> Not required for Phase II <== ! question: 3 section: 1 line_1: 3. Short Description of Proposed Observations line_3: We intend to record diagnostic-quality far-UV spectra of line_4: solar-type stars in young galactic clusters including the line_5: Hyades, the Pleiades, and ALPHA Persei. We selected five line_6: stars from each cluster which meet a number of strict line_7: criteria for membership, very likely are single, and which line_8: have reddening-corrected colors corresponding to G0-G3. line_10: Recording the critical spectral emissions in the far-UV -- line_11: from C III 1175, O V] 1218, and N V 1240 to C IV 1550 and line_12: He II 1640 -- requires two separate grating settings with the line_13: FOS: G130H & G190H. An additional brief exposure with G270H line_14: will record the bright Mg II 2800 h & k emissions at line_15: sufficient resolution to measure the integrated fluxes. ! question: 4 section: 1 line_1: 4. Need for HST line_3: We will investigate the high-excitation outer atmospheres line_4: of solar-type stars -- energized by magnetic activity -- as line_5: they age along their MS evolutionary tracks. On the Sun, line_6: co-spatiality between magnetic flux and high-excitation line_7: emissions is emphasized in the 100,000 K vacuum-UV resonance line_8: lines like C IV 1548 and N V 1238; whereas traditional line_9: ``chromospheric'' diagnostics accessible from the ground line_10: -- like Ca II and H-ALPHA -- tend to be contaminated to an line_11: uncertain degree by heating unrelated to magnetic activity, line_12: or suffer from uncertain modes of formation. line_14: Three stars of our sample -- HD28344, HD28992, and HZ1514 -- line_15: have been observed previously with IUE LWP-LO exposures to line_16: record the Mg II 2800 emission. There are no SWP-LO spectra line_17: of our program stars, and previous attempts to expose deep line_18: SWP-LOs of other (X-ray-selected) Hyads have produced only line_19: poor-quality spectral material. ! question: 5 section: 1 line_1: 5. Justification of Exposure Times line_3: We calculated FOS/BL G130H exposure times to achieve line_4: S/N = 35 at C IV 1548 in 30M. That ensures adequate S/N line_5: at C III] 1175 & N V 1238. For the Hyades (CYCLE-1 targets), line_6: we estimated f_1548 by scaling R_1548 (f_1548/f_bol) from line_7: measured values of R_2800 (Mg II) according to the power-law line_8: R_1548 = const R_2800^1.5. We will observe the 5 Hyads with line_9: the complete sequence of 3 FOS/BL gratings, with the same line_10: exposure time for each target to ensure uniformity. ! question: 6 section: 1 line_1: 6. a. Justification of special scheduling requests line_2: ==> none <== ! question: 6 section: 2 line_1: 6. b. Special calibration requirements line_2: ==> none <== ! question: 7 section: 1 line_1: 7. Data Reduction and Analysis line_3: Calibration of the FOS spectra will be undertaken at the line_4: STSci. Two team members are HRS/GTOs, and we expect to line_5: benefit from their experience. Initially, the spectral line_6: traces will be measured using standard fitting routines line_7: available at Colorado through the IUE RDAF. Subsequently, line_8: emission-measure modelling, density-sensitive line-ratio line_9: tests, and correlations with other diagnostics (like ground- line_10: based Ca K fluxes or ROSAT X-ray detections) will be line_11: conducted by specific team members. ! question: 8 section: 1 line_1: 8. Special Comments line_2: ==> none <== ! question: 9 section: 1 line_1: 9. Previous HST observing Time line_2: ==> none <== ! question: 10 section: 1 line_1: 10. Resources to be Supplied by Institution(s) line_3: Several domestic institutions are involved in our consortium. line_4: The resources and facilities that will be devoted to the line_5: project are extensive and varied. ! !end of general form text general_form_address: lname: AYRES fname: THOMAS mi: R. title: DR. category: PI inst: UNIVERSITY OF COLORADO addr_1: CAMPUS BOX 391 (CASA) city: BOULDER state: CO zip: 80309 country: USA phone: 303-492-4051 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD25825 descr_1: STAR; TYPE=G0 V; OPEN CLUSTER pos_1: RA=4H 6M 15.96S +/- 1", pos_2: DEC=+15D 41' 52.91" +/- 1", pos_3: PLATE-ID=000O equinox: 2000 pm_or_par: Y pos_epoch_yr: 1983.00 ra_pm_val: 0.009200 ra_pm_unct: 0.000500 dec_pm_val: -0.0180 dec_pm_unct: 0.0090 an_prlx_val: 0.0230 an_prlx_unct: 0.0010 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: HYADES G0 V STAR fluxnum_1: 1 fluxval_1: V = +7.85 +/- 0.02, TYPE = G0 V fluxnum_2: 1 fluxval_2: B-V = +0.59 +/- 0.02 fluxnum_3: 3 fluxval_3: F-LINE(2795) = 1 +/- 0.5 E-12 fluxnum_4: 3 fluxval_4: W-LINE(2795) = 1 +/- 0.2 fluxnum_5: 4 fluxval_5: F-LINE(1892) = 2 +/- 1 E-14 fluxnum_6: 4 fluxval_6: W-LINE(1892) = 0.4 +/- 0.1 fluxnum_7: 5 fluxval_7: F-LINE(1548) = 2 +/- 1 E-13 fluxnum_8: 5 fluxval_8: W-LINE(1548) = 0.3 +/- 0.1 ! targnum: 2 name_1: HD26767 descr_1: STAR; TYPE=G2 V; OPEN CLUSTER pos_1: RA=4H 14M 27.14S +/- 1", pos_2: DEC=+12D 26' 7.25" +/- 1", pos_3: PLATE-ID=01X0 equinox: 2000 pm_or_par: Y pos_epoch_yr: 1983.00 ra_pm_val: 0.007200 ra_pm_unct: 0.008000 dec_pm_val: 0.0030 dec_pm_unct: 0.0090 an_prlx_val: 0.0230 an_prlx_unct: 0.0010 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: HYADES G2 V STAR fluxnum_1: 1 fluxval_1: V = +8.06 +/- 0.02, TYPE = G2 V fluxnum_2: 1 fluxval_2: B-V = +0.64 +/- 0.02 fluxnum_3: 3 fluxval_3: F-LINE(2795) = 1 +/- 0.5 E-12 fluxnum_4: 3 fluxval_4: W-LINE(2795) = 1 +/- 0.2 fluxnum_5: 4 fluxval_5: F-LINE(1892) = 2 +/- 1 E-14 fluxnum_6: 4 fluxval_6: W-LINE(1892) = 0.4 +/- 0.1 fluxnum_7: 5 fluxval_7: F-LINE(1548) = 2 +/- 1 E-13 fluxnum_8: 5 fluxval_8: W-LINE(1548) = 0.3 +/- 0.1 ! targnum: 3 name_1: HD27835 descr_1: STAR; TYPE=G0 V; OPEN CLUSTER pos_1: RA=4H 24M 12.695S +/- 1", pos_2: DEC=+16D 22' 44.45" +/- 1", pos_3: PLATE-ID=000P equinox: 2000 pm_or_par: Y pos_epoch_yr: 1983.00 ra_pm_val: 0.006100 ra_pm_unct: 0.000500 dec_pm_val: -0.0170 dec_pm_unct: 0.0090 an_prlx_val: 0.0230 an_prlx_unct: 0.0010 comment_1: FAR-UV SPECTROPHOTOMETRY comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: HYADES G0 V STAR fluxnum_1: 1 fluxval_1: V = +8.24 +/- 0.02, TYPE = G0 V fluxnum_2: 1 fluxval_2: B-V = +0.59 +/- 0.02 fluxnum_3: 3 fluxval_3: F-LINE(2795) = 1 +/- 0.5 E-12 fluxnum_4: 3 fluxval_4: W-LINE(2795) = 1 +/- 0.2 fluxnum_5: 4 fluxval_5: F-LINE(1892) = 2 +/- 1 E-14 fluxnum_6: 4 fluxval_6: W-LINE(1892) = 0.4 +/- 0.1 fluxnum_7: 5 fluxval_7: F-LINE(1548) = 2 +/- 1 E-13 fluxnum_8: 5 fluxval_8: W-LINE(1548) = 0.3 +/- 0.1 ! targnum: 4 name_1: HD28344 descr_1: STAR; TYPE=G2 V; OPEN CLUSTER pos_1: RA=4H 28M 48.155S +/- 1", pos_2: DEC=+17D 17' 7.88" +/- 1", pos_3: PLATE-ID=000P equinox: 2000 pm_or_par: Y pos_epoch_yr: 1983.00 ra_pm_val: 0.007000 ra_pm_unct: 0.000500 dec_pm_val: -0.0430 dec_pm_unct: 0.0090 an_prlx_val: 0.0230 an_prlx_unct: 0.0010 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: HYADES G2 V STAR fluxnum_1: 1 fluxval_1: V = +7.85 +/- 0.02, TYPE = G2 V fluxnum_2: 1 fluxval_2: B-V = +0.61 +/- 0.02 fluxnum_3: 3 fluxval_3: F-LINE(2795) = 1 +/- 0.5 E-12 fluxnum_4: 3 fluxval_4: W-LINE(2795) = 1 +/- 0.2 fluxnum_5: 4 fluxval_5: F-LINE(1892) = 2 +/- 1 E-14 fluxnum_6: 4 fluxval_6: W-LINE(1892) = 0.4 +/- 0.1 fluxnum_7: 5 fluxval_7: F-LINE(1548) = 2 +/- 1 E-13 fluxnum_8: 5 fluxval_8: W-LINE(1548) = 0.3 +/- 0.1 ! targnum: 5 name_1: HD28992 descr_1: STAR; TYPE=G1 V; OPEN CLUSTER pos_1: RA=4H 34M 35.177S +/- 1", pos_2: DEC=+15D 30' 17.56" +/- 1", pos_3: PLATE-ID=002J equinox: 2000 pm_or_par: Y pos_epoch_yr: 1983.00 ra_pm_val: 0.007200 ra_pm_unct: 0.000500 dec_pm_val: -0.0400 dec_pm_unct: 0.0090 an_prlx_val: 0.0230 an_prlx_unct: 0.0010 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: HYADES G1 V STAR fluxnum_1: 1 fluxval_1: V = +7.94 +/- 0.02, TYPE = G1 V fluxnum_2: 1 fluxval_2: B-V = +0.63 +/- 0.02 fluxnum_3: 3 fluxval_3: F-LINE(2795) = 1 +/- 0.5 E-12 fluxnum_4: 3 fluxval_4: W-LINE(2795) = 1 +/- 0.2 fluxnum_5: 4 fluxval_5: F-LINE(1892) = 2 +/- 1 E-14 fluxnum_6: 4 fluxval_6: W-LINE(1892) = 0.4 +/- 0.1 fluxnum_7: 5 fluxval_7: F-LINE(1548) = 2 +/- 1 E-13 fluxnum_8: 5 fluxval_8: W-LINE(1548) = 0.3 +/- 0.1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: POASH targname: # config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: TYPE = UP req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 1.100; req_3: SEQ 1.000-1.100 NO GAP; req_4: GROUP 1-4 NO GAP; req_5: CYCLE 1 / 1-4 ! linenum: 1.100 sequence_1: DEFINE sequence_2: POASH targname: # config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 1S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: TYPE = UP req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 2-4; ! linenum: 2.000 sequence_1: DEFINE sequence_2: POASH targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 50S s_to_n: 100 s_to_n_time: 60S fluxnum_1: 3 priority: 3 ! linenum: 3.000 sequence_1: DEFINE sequence_2: POASH targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 930S s_to_n: 20 s_to_n_time: 30M fluxnum_1: 4 priority: 2 ! linenum: 4.000 sequence_1: DEFINE sequence_2: POASH targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 1650S s_to_n: 35 s_to_n_time: 30M fluxnum_1: 5 priority: 1 ! linenum: 10.000 sequence_1: USE sequence_2: POASH targname: HD28344 ! linenum: 11.000 sequence_1: USE sequence_2: POASH targname: HD28992 ! linenum: 12.000 sequence_1: USE sequence_2: POASH targname: HD25825 ! linenum: 13.000 sequence_1: USE sequence_2: POASH targname: HD26767 ! linenum: 14.000 sequence_1: USE sequence_2: POASH targname: HD27835 ! ! end of exposure logsheet scan_data: line_list: 1.0 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 4.3000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 2.1 wid_offset: 0.0 ! line_list: 1.1 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 4.3000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 2.1 wid_offset: 0.0 ! ! end of scan data