! $Id: 5733,v 7.1 1995/02/20 18:48:26 pepsa Exp $ coverpage: title_1: DYNAMICS AND ENERGY BALANCE IN STELLAR TRANSITION REGIONS title_2: CYCLE 3 AUGMENTATION - MISSING EXPOSURE sci_cat: STELLAR ASTROPHYSICS sci_subcat: COOL STARS proposal_for: AUG/HRS cont_id: 4874 pi_fname: JEFFREY pi_mi: L. pi_lname: LINSKY pi_inst: COLORADO, UNIVERSITY OF pi_country: USA pi_phone: (303)492-7838 keywords_1: HYDROGEN COLUMN DENSITY, DEUTERIUM COLUMN DENSITY, keywords_2: DEUTERIUM ABUNDANCE hours_pri: 1.96 num_pri: 1 time_crit: X pi_position: ASTROPHYSICST abstract: line_1: We will observe with 80,000 spectral resolution the stellar line_2: Lyman alpha emission line and interstellar hydrogen and line_3: deuterium absorption towards local late-type stars to derive line_4: the H and D column densities and D/H ratios along different line_5: lines of sight. High resolution (90,000) spectra of the MgII and line_6: FeII lines will help determine the interstellar line broadening line_7: and whether material along each line of sight has more than one line_8: velocity component. This is critical for accurate measurements line_9: of D/H, because both the D and H lines are on or near the flat line_10: part of the curve of growth. Previous IUE and Copernicus line_11: observations, which had low signal/noise and inadequate spectral line_12: resolution, provided very crude D/H values and suggested that line_13: the D/H ratio may vary within a few parsecs of the Sun. We will line_14: measure D/H with at least one order of magnitude improved line_15: precision and determine whether the proposed local variations line_16: are real. The local value(s) of D/H may be extrapolated to zero line_17: metal abundance to estimate the primordial value, which is line_18: valuable for constraining cosmological models. line_19: THIS PHASE II IS FOR OBSERVATION OF AN UNSCHEDULED CYCLE3 LYMAN line_20: ALPHA OBSERVATION OF HR1099 AT ORBITAL PHASE 0.75. general_form_proposers: lname: JURA fname: MICHAEL inst: UC, LOS ANGELES country: USA lname: SAVAGE fname: BLAIR mi: D. inst: WISCONSIN, UNIVERSITY OF country: USA lname: LINSKY fname: JEFFREY mi: L. inst: COLORADO, UNIVERSITY OF country: USA lname: HEAP fname: SARA mi: R. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA lname: LANDSMAN fname: WAYNE inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA lname: SMITH fname: ANDREW mi: M. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA lname: BROWN fname: ALEXANDER inst: COLORADO, UNIVERSITY OF country: USA general_form_text: question: 3 section: 1 line_1: We intend to observe 5 stars at 1.0E+5 resolution with the HRS in 3 line_2: grating settings. Two stars (Capella and HR 1099) are spectroscopic line_3: binary systems that will be observed at orbital quadrature in order line_4: to shift the interstellar absorption feature relative to the stellar line_5: emission line. question: 4 section: 1 line_1: The required spectral lines cannot be observed from the ground. question: 5 section: 1 line_1: HR 1099 is a spectroscopic binary and should be observed at the line_2: quadrature with phase 0.75. Ephemeris for HR1099 is PHI=0.00 line_3: at JD (helio) = 2,442,766.069 + 2d.83782E. line_4: GTO program 4873 observed phase 0.25 and GO program 4447 line_5: observed muliple phases of HR1099. Previous GTO 4874 line_6: observations of Mg II and Fe II were made at phase 0.75 during line_7: Cycle 3. Observations may be scheduled at any suitable phase line_8: 0.75 quadrature during Cycle 4. question: 8 section: 1 line_1: question: 10 section: 1 line_1: Data analysis programs and postdoctoral research associates supported by the line_2: HRS GTO program. general_form_address: lname: LINSKY fname: JEFFREY mi: L. category: PI inst: JILA, UNIVERSITY OF COLORADO addr_1: CAMPUS BOX 440 city: BOULDER state: CO zip: 80309 country: USA phone: (303) 492-7838 telex: 755842 JILA fixed_targets: targnum: 5 name_1: HD22468 name_2: HR1099 descr_1: A,167 pos_1: RA=03H34M13.169S+/-0.01S, pos_2: DEC=+00D25'33.17"+/-0.1" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.002 ra_pm_unct: 0.0002 dec_pm_val: -0.1610 dec_pm_unct: 0.0010 an_prlx_val: 0.0320 rv_or_z: V=-23 fluxnum_1: 1 fluxval_1: V=5.71 exposure_logsheet: ! linenum: 1.000 sequence_1: DEFINE sequence_2: LISM1 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1215.70 num_exp: # time_per_exp: 108.8S s_to_n: 100 priority: # param_1: STEP-PATT=7, param_2: FP-SPLIT=STD ! linenum: 33.000 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S priority: 2 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 34; req_2: ZERO-PHASE JD2442766.069 +/- 0.001D; req_3: PERIOD 2.83782D +/- 0.0001D; req_4: PHASE 0.75 +/- 0.05; req_5: CYCLE 4/33-51; req_6: GROUP 33-51 NO GAP comment_1: STEP TIME = 200 MSEC ! linenum: 34.000 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 5S fluxnum_1: 1 param_1: SEARCH-SIZE=5, priority: 2 req_1: ONBOARD ACQ FOR 50.0-51.0 comment_1: STEP-TIME= 0.2 SEC ! linenum: 50.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-A wavelength: 1215.70 num_exp: 1 time_per_exp: 64S priority: 2 param_1: STEP-PATT=3 req_1: CALIB FOR 51 NO SLEW; req_2: SEQ 50-51 NO GAP comment_1: NO CARROUSEL MOTION BETWEEN 50 AND 51 ! linenum: 51.000 sequence_1: USE sequence_2: LISM1 targname: HD22468 num_exp: 4 time_per_exp: X9 priority: ^