! File: 3908C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:23:32:46 coverpage: title_1: SLEUTHING THE DYNAMO: CYCLE 2 CONTINUATION sci_cat: STELLAR ASTROPHYSICS sci_subcat: EARLY EVOLUTION proposal_for: GO longterm: 2 cont_id: 2485 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: 11.98 num_pri: 5 fos: Y funds_amount: 118718 funds_length: 12 funds_date: JUL-92 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. line_16: For the continuation program, we selected 3 targets from the line_17: Pleiades, and 2 targets from ALPHA Per. Owing to the line_18: faintness of the targets, we will obtain observations with line_19: G130H & G270H only, focusing on the critical C IV & Mg II line_20: emissions. ! 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. a. Justification of special scheduling requests line_3: ==> none <== ! question: 6 section: 2 line_1: 5. b. Special calibration requirements line_3: ==> 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_3: ==> none <== ! question: 9 section: 1 line_1: 9. Previous HST observing Time line_3: Cycle-1 part of program is on long-range schedule (10/92) ! 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 389 (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: STAR-0344+2447 name_2: HZ314 name_3: GSC OBJECT-ID=1803-574 descr_1: A; 137; 901; descr_2: C; 202 pos_1: RA=3H 44M 20.074S +/- 1", pos_2: DEC=+24D 47' 46.77" +/- 1", pos_3: PLATE-ID=009M equinox: J2000 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: PLEIADES G0 V STAR fluxnum_1: 1 fluxval_1: V = +10.6 +/- 0.1, TYPE = G0 V fluxnum_2: 2 fluxval_2: B-V = +0.64 +/- 0.02 fluxnum_3: 2 fluxval_3: E(B-V) = 0.06 +/- 0.02 fluxnum_4: 3 fluxval_4: F-LINE(2795) = 1 +/- 0.5 E-13 fluxnum_5: 3 fluxval_5: W-LINE(2795) = 1 +/- 0.2 fluxnum_6: 4 fluxval_6: F-LINE(1548) = 1 +/- 0.5 E-15 fluxnum_7: 4 fluxval_7: W-LINE(1548) = 1 +/- 0.2 ! targnum: 2 name_1: STAR-0347+2421 name_2: HZ1514 name_3: GSC OBJECT-ID=1800-1674 descr_1: A; 137; 901; descr_2: C; 202 pos_1: RA=3H 47M 40.439S +/- 1", pos_2: DEC=+24D 21' 53.04" +/- 1", pos_3: PLATE-ID=009M equinox: J2000 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: PLEIADES G0 V STAR fluxnum_1: 1 fluxval_1: V = +10.5 +/- 0.1, TYPE = G0 V fluxnum_2: 2 fluxval_2: B-V = +0.64 +/- 0.02 fluxnum_3: 2 fluxval_3: E(B-V) = 0.06 +/- 0.02 fluxnum_4: 3 fluxval_4: F-LINE(2795) = 1 +/- 0.5 E-13 fluxnum_5: 3 fluxval_5: W-LINE(2795) = 1 +/- 0.2 fluxnum_6: 4 fluxval_6: F-LINE(1548) = 1 +/- 0.5 E-15 fluxnum_7: 4 fluxval_7: W-LINE(1548) = 1 +/- 0.2 ! targnum: 3 name_1: STAR-0346+2434 name_2: HZ996 name_3: GSC OBJECT-ID=1804-2129 descr_1: A; 137; 901; descr_2: C; 202 pos_1: RA=3H 46M 22.668S +/- 1", pos_2: DEC=+24D 34' 12.96" +/- 1", pos_3: PLATE-ID=009M equinox: J2000 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: PLEIADES G0 V STAR fluxnum_1: 1 fluxval_1: V = +10.4 +/- 0.1, TYPE = G0 V fluxnum_2: 2 fluxval_2: B-V = +0.64 +/- 0.02 fluxnum_3: 2 fluxval_3: E(B-V) = 0.06 +/- 0.02 fluxnum_4: 3 fluxval_4: F-LINE(2795) = 1 +/- 0.5 E-13 fluxnum_5: 3 fluxval_5: W-LINE(2795) = 1 +/- 0.2 fluxnum_6: 4 fluxval_6: F-LINE(1548) = 1 +/- 0.5 E-15 fluxnum_7: 4 fluxval_7: W-LINE(1548) = 1 +/- 0.2 ! targnum: 7 name_1: STAR-0326+4954 name_2: HE709 name_3: GSC OBJECT-ID=3320-818 descr_1: A; 137; 901; descr_2: C; 202 pos_1: RA=3H 26M 43.913S +/- 1", pos_2: DEC=+49D 54' 34.99" +/- 1", pos_3: PLATE-ID=02RP equinox: J2000 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: ALPHA PERSEI G0 V STAR fluxnum_1: 1 fluxval_1: V = +10.9 +/- 0.1, TYPE = G0 V fluxnum_2: 2 fluxval_2: B-V = +0.68 +/- 0.02 fluxnum_3: 2 fluxval_3: E(B-V) = 0.09 +/- 0.02 fluxnum_4: 3 fluxval_4: F-LINE(2795) = 1 +/- 0.5 E-13 fluxnum_5: 3 fluxval_5: W-LINE(2795) = 1 +/- 0.2 fluxnum_6: 4 fluxval_6: F-LINE(1548) = 1 +/- 0.5 E-15 fluxnum_7: 4 fluxval_7: W-LINE(1548) = 1 +/- 0.2 ! targnum: 8 name_1: STAR-0317+4850 name_2: HE350 name_3: GSC OBJECT-ID=3319-306 descr_1: A; 137; 901; descr_2: C; 202 pos_1: RA=3H 17M 36.908S +/- 1", pos_2: DEC=+48D 50' 9.65" +/- 1", pos_3: PLATE-ID=02RP equinox: J2000 comment_1: FAR-UV SPECTRA comment_2: OF SOLAR-TYPE STARS comment_3: IN YOUNG GALACTIC CLUSTERS comment_4: ALPHA PERSEI G0 V STAR fluxnum_1: 1 fluxval_1: V = +11.0 +/- 0.1, TYPE = G0 V fluxnum_2: 2 fluxval_2: B-V = +0.68 +/- 0.02 fluxnum_3: 2 fluxval_3: E(B-V) = 0.09 +/- 0.02 fluxnum_4: 3 fluxval_4: F-LINE(2795) = 1 +/- 0.5 E-13 fluxnum_5: 3 fluxval_5: W-LINE(2795) = 1 +/- 0.2 fluxnum_6: 4 fluxval_6: F-LINE(1548) = 1 +/- 0.5 E-15 fluxnum_7: 4 fluxval_7: W-LINE(1548) = 1 +/- 0.2 ! ! 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/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.7S s_to_n: 10 fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 2-3; req_2: GROUP 1-3 NO GAP; req_3: CYCLE 2 / 1-3 ! 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: 300S s_to_n: 50 s_to_n_time: 5M fluxnum_1: 3 priority: 1 ! linenum: 3.000 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: 5350S s_to_n: 10 s_to_n_time: 90M fluxnum_1: 4 priority: 1 ! linenum: 4.100 sequence_1: DEFINE sequence_2: POASH2 targname: # config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: FAINT=947 req_1: ONBOARD ACQ FOR 4.2-4.3; req_2: GROUP 4.2-4.3 NO GAP; req_3: CYCLE 2 / 4.10-4.30 ! linenum: 4.200 sequence_1: DEFINE sequence_2: POASH2 targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 300S s_to_n: 50 s_to_n_time: 5M fluxnum_1: 3 priority: 1 ! linenum: 4.300 sequence_1: DEFINE sequence_2: POASH2 targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 5350S s_to_n: 10 s_to_n_time: 90M fluxnum_1: 4 priority: 1 ! linenum: 5.100 sequence_1: DEFINE sequence_2: POASH3 targname: # config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: FAINT=1037 req_1: ONBOARD ACQ FOR 5.2-5.3; req_2: GROUP 5.2-5.3 NO GAP; req_3: CYCLE 2 / 5.10-5.30 ! linenum: 5.200 sequence_1: DEFINE sequence_2: POASH3 targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 300S s_to_n: 50 s_to_n_time: 5M fluxnum_1: 3 priority: 1 ! linenum: 5.300 sequence_1: DEFINE sequence_2: POASH3 targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 5350S s_to_n: 10 s_to_n_time: 90M fluxnum_1: 4 priority: 1 ! linenum: 6.100 sequence_1: DEFINE sequence_2: POASH4 targname: # config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: FAINT=1146 req_1: ONBOARD ACQ FOR 6.2-6.3; req_2: GROUP 6.2-6.3 NO GAP; req_3: CYCLE 2 / 6.10-6.30 ! linenum: 6.200 sequence_1: DEFINE sequence_2: POASH4 targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 300S s_to_n: 50 s_to_n_time: 5M fluxnum_1: 3 priority: 1 ! linenum: 6.300 sequence_1: DEFINE sequence_2: POASH4 targname: # config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 5350S s_to_n: 10 s_to_n_time: 90M fluxnum_1: 4 priority: 1 ! linenum: 10.000 sequence_1: USE sequence_2: POASH2 targname: STAR-0344+2447 ! linenum: 11.000 sequence_1: USE sequence_2: POASH3 targname: STAR-0347+2421 ! linenum: 12.000 sequence_1: USE sequence_2: POASH4 targname: STAR-0346+2434 ! linenum: 13.000 sequence_1: USE sequence_2: POASH targname: STAR-0326+4954 ! linenum: 14.000 sequence_1: USE sequence_2: POASH targname: STAR-0317+4850 ! ! end of exposure logsheet ! No scan data records found