! $Id: 5495,v 7.1 1994/07/27 18:37:42 pepsa Exp $ coverpage: title_1: UV EMISSION LINE FORMATION PROCESSES AROUND THE title_2: BRIGHTEST HERBIG AE STAR HD104237 CYCLE 4 - MED sci_cat: COOL STARS sci_subcat: EARLY EVOLUTION proposal_for: GO pi_title: DR. pi_fname: ALEXANDER pi_lname: BROWN pi_inst: U. OF COLORADO pi_country: USA pi_phone: (303) 492-7810 keywords_1: HERBIG AE STAR hours_pri: 3.99 num_pri: 1 hrs: Y funds_amount: 30000 funds_length: 12 funds_date: MAR-93 pi_position: SENIOR RES ASSOCIATE off_fname: CARL off_lname: WIEMAN off_title: CHAIRMAN off_inst: JOINT INSTITUTE FOR LABORATORY ASTROPHYSICS off_addr_1: UNIVERSITY OF COLORADO off_addr_2: CAMPUS BOX 440 off_city: BOULDER off_state: CO off_zip: 803090440 off_country: USA off_phone: (303) 492 5128 off_telex: (303) 492 5235 ! end of coverpage abstract: line_1: Herbig Ae stars are intermediate mass pre-main sequence (PMS) stars, and line_2: the more massive counterparts of the well-known T Tauri stars. Their line_3: evolution and atmospheric properties are still poorly understood. We line_4: propose to study the profiles of emission lines formed in the outer line_5: atmosphere/ circumstellar regions of the brightest and closest Herbig Ae line_6: star, HD104237, using GHRS spectra at moderate and high resolution of line_7: selected high temperature emission lines. At present it is not clear if line_8: these lines form in a stellar wind, an accretion disk, or a classical line_9: transition region (TR)/chromosphere. The emission line profiles will be line_10: analyzed to investigate atmospheric (density and temperature structure) line_11: and wind (mass loss rate, velocity and density laws) properties of this line_12: star. One goal is to discover if the winds from Herbig Ae stars can line_13: totally dominate the atmospheric structure of the star with TR plasma line_14: forming an integral part of the stellar wind or if physically separate, line_15: stationary, confined regions exist at the base of the wind. We shall line_16: determine quantitative constraints on the non-radiative heating, line_17: accretion and mass loss processes in the atmosphere, which will allow line_18: a better understanding of the evolution of PMS stars, since the heating line_19: and mass loss are driven by processes related to the sub-photospheric line_20: stellar structure. ! ! end of abstract general_form_proposers: lname: BROWN fname: ALEXANDER title: PI inst: 1764 country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: 1764 country: USA ! lname: BENNETT fname: PHILIP inst: 1764 country: USA ! lname: SKINNER fname: STEPHEN mi: L. inst: 6510 country: JAPAN ! lname: BLONDEL fname: PETER inst: 6810 country: NETHERLANDS ! lname: TJIN A DJIE fname: HERMAN mi: R. inst: 6810 country: NETHERLANDS ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Our proposed observations will provide the first high-quality (S/N = 15- line_2: 100) line profiles for emission lines of H I (1216A), Si III (1206A), line_3: O V (1218A),O I (1302,4,6 + S I, Si II), C II (1335A), Si IV (1396,1403A) line_4: O IV (1402,140)7, C IV (1548,1550A) and Mg II (2796,2803A). All of these line_5: spectra will be obtained with the G160M grating, except for Mg II which line_6: will be obtained with ECH-B. G140L spectra of the 1170-1700 A region will line_7: be obtained so that emission lines too weak to be detected by IUE can be line_8: measured. The observations requested in Phase 1 were: line_10: Central Strong line_11: GHRS grating Wavelength(s) Aperture Exposure S/N Features line_12: Time line_13: G160M 1216 LSA 11 min 30 H I/Si III/O V line_14: G160M 1302 LSA 12 min 30 O I/S I line_15: G160M 1335 LSA 20 min 15 C II line_16: G160M 1400 LSA 45 min 31 Si IV line_17: 10 O IV line_18: G160M 1550 LSA 34 min 20 C IV line_19: ECH-B 2799 LSA 5 min 100 Mg II line_20: G140L 1305,1575 LSA 5,10min 50 ...... line_21: The quoted signal-to-noise values refer to the peak of the strongest line_22: emission line in the particular spectrum. TO FIT OUR ALLOCATION THE line_23: 1335 A EXPOSURE IS ELIMINATED AND THE 1216 A EXPOSURE HALVED ! question: 4 section: 1 line_1: The data required for this program consists of UV spectra not obtainable line_2: from the ground. IUE has been used extensively to study this target to line_3: the limits of its capability (including high resolution exposures up to line_4: 16 hours), and further observational advances depend on the acquisition line_5: of higher S/N spectra with GHRS. The increased sensitivity, wavelength line_6: resolution, dynamic range and S/N characteristics of the GHRS over those line_7: obtainable with the IUE (Carpenter et al. 1992, Ap.J. Lett., 377, L45.) line_8: will allow more accurate and detailed modelling of physical processes line_9: occurring in the outer atmosphere of HD104237. Only the GHRS is capable line_10: of providing us with the high precision line profiles, fluxes, and line_11: absolute velocities required for our program. ONLY GHRS CAN PROVIDE line_12: THE LINE PROFILES OF OPTICALLY-THIN, DENSITY-SENSITIVE EMISSION LINES. line_13: . line_14: The exposures requested are summarized in section 2. The exposure times line_15: have been estimated using absolute fluxes previously measured with the line_16: IUE. For the first order and echelle gratings we used sensitivity values line_17: given in the GHRS instrument handbook. The LSA is used. ! question: 5 section: 1 line_1: No real-time observations or special scheduling is required. ! question: 6 section: 1 line_1: Internal Pt lamp SPYBAL spectra should provide a sufficiently accurate line_2: wavelength scale for our first order grating observations. We include a line_3: WAVE observation for our single echelle (Mg II 2800 A) observation, so line_4: that precise measurements of the interstellar and circumstellar line_5: absorption velocities can be made. ! ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: GO Program 3626 - Empirical determination of the wind velocity and line_2: density laws for the K supergiant Zeta Aurigae from eclipse ingress line_3: Spectra (A. Brown PI, J. Linsky, R. Weyman, D. Reimers, R. Baade, line_4: T. Kirsch) ! question: 10 section: 1 line_1: Software developed by the GHRS IDT and the proposers will be used in the line_2: reduction and analysis of these observations. A workstation at JILA line_3: connected to the CASA cluster is available for data reduction and line_4: analysis. ! !end of general form text general_form_address: lname: Brown fname: Alexander title: Dr. category: PI inst: Joint Institute for Laboratory Astrophysics addr_1: University of Colorado city: Boulder state: CO zip: 803090440 country: USA phone: (303) 492-7810 telex: 755842 JILA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD104237 descr_1: A,127 pos_1: RA=11H57M33.47S+/-0.15S, pos_2: DEC=-77D54'50.5"+/-0.5" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.016200 ra_pm_unct: 0.001000 dec_pm_val: 0.0140 dec_pm_unct: 0.0070 rv_or_z: V=0.0 fluxnum_1: 1 fluxval_1: V=6.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 10.000 targname: HD104237 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 9S priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 12; req_2: CYCLE 4/10-55 ; req_3: GROUP 10-55 NO GAP comment_1: STEP TIME = 1 SEC comment_2: EXPECTED A2 COUNTS ARE comment_3: APPROX. 1500 PER SECOND ! linenum: 12.000 targname: HD104237 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 163.2S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 21.0-55.0 comment_1: STEP-TIME=1.6 SEC comment_2: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 21.000 targname: HD104237 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1222.5 num_exp: 1 time_per_exp: 871.0S priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 26.000 targname: HD104237 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1302.0 num_exp: 1 time_per_exp: 762.0S priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 36.000 targname: HD104237 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1401.0 num_exp: 2 time_per_exp: 1415.0S priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 41.000 targname: HD104237 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1548.0 num_exp: 2 time_per_exp: 1088.0S priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 45.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B20 wavelength: 2800 num_exp: 1 time_per_exp: 32S priority: ^ param_1: STEP-PATT=3 req_1: CALIB FOR 46 NO SLEW; req_2: SEQ 45-46 NO GAP ! linenum: 46.000 targname: HD104237 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B20 wavelength: 2800 num_exp: 1 time_per_exp: 327S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 47.000 targname: HD104237 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1305.0 num_exp: 1 time_per_exp: 436.0S priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 55.000 targname: HD104237 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1575.0 num_exp: 1 time_per_exp: 654.0S priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! ! end of exposure logsheet ! No scan data records found