! File: 3845C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:21:30:48 coverpage: title_1: DECIPHERING THE UV EMISSION LINES IN T TAURI SYSTEMS sci_cat: STELLAR ASTROPHYSICS sci_subcat: EARLY EVOLUTION proposal_for: GO cont_id: 3845 pi_fname: GIBOR pi_lname: BASRI pi_inst: UNIV. OF CALIFORNIA, BERKELEY pi_country: USA pi_phone: 415-642-8198 hours_pri: 5.42 num_pri: 5 hrs: Y funds_amount: 62603 funds_length: 12 off_inst: UNIV. OF CALIFORNIA, BERKELEY off_addr_1: ASTRONOMY DEPARTMENT off_addr_2: UNIV. OF CALIFORNIA off_city: BERKELEY off_state: CA off_zip: 94720 off_country: USA off_phone: 415-642-5275 ! end of coverpage abstract: line_1: Currently there is complete confusion as to the physical origin of the UV line_2: emission lines in T Tauri stars, although they are the strongest known UV line_3: emissions from cool stars. Possibilities include closed magnetic field line_4: loops in analogy to active main sequence stars, a hot region in an Alfven line_5: wind, the accretion boundary layer between star and disk, accretion line_6: columns in the stellar magnetic field, or some other region associated line_7: with a disk-generated wind. Emission measure analyses have been unable to line_8: distinguish between the possibilities listed above. What is clearly line_9: needed is line profile information: in particular a good measurement of line_10: the breadth of the profiles and a reasonable idea of their symmetry. line_11: Narrow lines will indicate plasma originating either on the stellar line_12: surface or in closed magnetic loops. Broad lines will indicate a line_13: turbulent boundary layer or wind region. The asymmetry of the lines will line_14: indicate whether they arise in accretion, outflow, or relatively static line_15: plasma, and something about the size of the region (via occulation line_16: effects). Taken with some emission measures, density diagnostics, and line_17: wind diagnostic information, the current mystery about the origin of line_18: these strong hot emission lines can be illuminated. We propose to line_19: measure enough profiles and emission measures in a representative small line_20: sample of stars to constrain, support or eliminate the above hypotheses. ! ! end of abstract general_form_proposers: lname: BASRI fname: GIBOR title: PI inst: UNIV. OF CALIFORNIA, BERKELEY country: USA ! lname: WALTER fname: FREDERICK mi: M inst: STATE UNIV. OF NEW YORK AT STONY BROOK country: USA ! lname: HARTMANN fname: LEE inst: HARVARD-SMITHSONIAN CENTER FOR ASTROPHYSICS country: USA ! lname: CALVET fname: NURIA inst: CENTRO DE INVESTIGACIONES DE ASTRONOMIA country: VENEZUELA ! ! end of general_form_proposers block general_form_text: question: 3 section: 0 line_1: Our program for each star will be: (1) an exposure using line_2: G160M to achieve S/N of 20 in the Si IV lines at a line_3: resolution of 20000; this will also include the density line_4: sensitive O IV lines, (2) exposures using G160M to obtain line_5: line fluxes in the 1345A, 1555A, and 1640A regions as line_6: feasible (which include C I, O I, CII, He II, Fe II and line_7: other ions) to get profiles and deblend complexes, and (3) line_8: an exposure using G270M to obtain a high resolution profile line_9: of Mg II at 2800A. We will read out the spectra line_10: every 5 minutes in order to mitigate against geo- line_11: magnetically induced image motion. This will also give some line_12: indication if there is very short time-scale variability in line_13: the lines. ! question: 4 section: 0 line_1: We are pursuing observations of the UV lines in TTS for line_2: several reasons. 1) They are the only direct diagnostics of line_3: the transition region plasma and accretion shock plasma line_4: available. 2) Because they are not very optically thick line_5: their interpretation is much easier than optical lines. 3) line_6: They are the only lines with which to distinguish a number line_7: of competing hypotheses about the relation between coronae line_8: and winds in TTS, and should be very helpful in line_9: understanding the wind generation region and the interface line_10: between star and disk. line_11: IUE observations at low resolution have been pursued for line_12: many TTS (Imhoff and Appenzeller 1987). These are primarily line_13: longward of 2000A, and concentrated on the flux in the Mg II line_14: lines (which are analogous to the Ca II lines). There are line_15: some low S/N low resolution observations of the lines line_16: shortward of 2000A, and those provide the justification for line_17: this proposal without accomplishing its science. That data line_18: has been insufficient to allow examination of the many line_19: hypotheses tested here, and has been only interpretable in line_20: terms of a solar analogy which misses the main properties line_21: unique to CTTS - the wind and disk accretion. The IUE data line_22: suffers severe blending, which precludes use of the denstiy line_23: diagnostics in this proposal. ! question: 6 section: 0 line_1: One of the scientific goals is to interpret the profiles and line_2: features in them in terms of accretion and outflow. To be line_3: sure about this, we must have the velocity in the stellar line_4: frame accurately known (to a few km/s). Previous experience line_5: has shown that sometimes features are near line center and line_6: an accurate velocity scale is crucial to their line_7: interpretation. To be safe, we are requesting wavelength line_8: calibration exposures for the Si IV profile line_9: observations, so there will be no question whether a profile line_10: peak or dip is red or blue shifted, and by how much. The line_11: other exposures can be interpreted safely with only the line_12: standard calibration, once we have done this. ! question: 7 section: 0 line_1: Since one of us (FW) is a GTO and intimately familiar with line_2: GHRS, he will be primarily responsible for receiving the line_3: data from the Institute, and putting it into a form that is line_4: amenable for analysis. FW and GB will concentrate on the "active star" line_5: analysis. This will include an emission measure analysis of line_6: the low dispersion spectrum, and any measurements we have line_7: managed with other instruments on chromospheric or coronal line_8: diagnostics. GB and LH will compare the profiles with line_9: their extensive collections of optical echelle spectra line_10: (lines of H, Ca II, Na I, He I, etc.). They will also line_11: consider to what extent the UV data is consistent with an line_12: origin in the boundary layer. This will include looking for line_13: the double-peaked signature of ring-like regions, and line_14: comparing the velocity width to the Keplarian expectation line_15: near the star. The primary profile modelling will be done by NC, in line_16: collaboration with LH and GB and his students. The general line_17: procedure for hydrogen is given by Hartmann et al.(1990). line_18: GB has a number of optically thin codes line_19: also available which work in a variety of geometries. line_20: NC is presently working on extending the escape probability line_21: treatment to more generalized geometries, in particular to a line_22: dipole-type geometry, to obtain a better description of the line_23: flow in the magnetosphere. ! question: 8 section: 0 line_1: We will use the GASP astrometric system to improve target line_2: coordinates prior to scheduling of the observations. GB line_3: will obtain optical echelle spectra of the targets as close line_4: to the HST observations as possible. FW will obtain data on line_5: NTTS as part of his GTO program which will be very useful in line_6: understanding what the purely stellar component of the UV line_7: emissions looks like. His program 1209 will look at line_8: HDE283572, SAO76411A, and V410 Tau with high resolution in line_9: the Mg II and Si IV regions, and also obtain low resolution line_10: spectra of these stars without disks which will be directly line_11: comparable to the spectra obtained in this program. That line_12: program does not overlap with this one, but is very line_13: complementary. ! question: 9 section: 1 line_1: Fred Walter is involved with the following programs: line_2: 1207 Ultraviolet Tomography This observation has yet to be undertaken. line_3: of V471 Tauri It bears no relation to this proposal. line_4: (GTO, cycle 2) line_5: 1208 Doppler Imaging of the This observation has yet to be undertaken. line_6: Chromospheres and It bears no relation to this proposal. line_7: Transition Regions of line_8: AR Lacertae line_9: (GTO, cycle 1) line_10: 1209 Non-radiative Heating This observation has yet to be undertaken. line_11: in Pre-Main Sequence This proposal, including augmentation targets, line_12: Stars studies NTTS and extreme CTTS at high dispersion, line_13: (GTO, cycle 1) and using G140L with shorter exposure times line_14: (no overlap in targets; no normal CTTS done) line_15: 1210 Age Dependence of Two spectra have been obtained to date. line_16: Non-radiative Heating There is no relation to this proposal, but the line_17: in Stellar Chromospheres spectra will be useful for comparison. line_18: (GTO, cycle 0) line_19: Lee Hartmann is involved with the following program: line_20: ???? The Formation and Evolution This proposal has yet to be undertaken. line_21: of Solar Nebulae Surrounding It bears no direct relation to this line_22: Pre-Main Sequence Stars program (it involves imaging). line_23: (GO, cycle 1) (S.Strom, PI) ! question: 10 section: 0 line_1: FW has access to the full range of GHRS team software for line_2: data extraction and analysis. GB has access to IDL and line_3: various radiative transfer codes. LH and NC have many line_4: powerful radiative transfer codes. We all have computer line_5: facilities which will allow both analysis of spectra and the line_6: running of various models to interpret the data. We are line_7: requesting some computing funds to support this, but no line_8: hardware or software acquisitions. GB and FW have thesis line_9: students who are working on aspects of this problem and will line_10: include work on this proposal in their dissertations. GB line_11: has the use of Lick Observatory which is flexible about line_12: getting echelle data on reasonably short notice (using a line_13: coude feed and the Hamilton spectrograph). We also have line_14: access to automated photometric monitoring, which will be line_15: valuable in assessing the activity state of the targets. ! !end of general form text general_form_address: lname: BASRI fname: GIBOR category: PI inst: UNIV. OF CALIFORNIA addr_1: ASTRONOMY DEPARTMENT city: BERKELEY state: CA zip: 94720 country: USA phone: 415-642-8198 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: BP-TAU name_2: GSC-554 descr_1: A,156,139 pos_1: PLATE-ID=0051, pos_2: RA = 04H 19M 15.86S +/- 0.3S, pos_3: DEC = +29D 06' 27.22" +/- 0.3S equinox: 2000 rv_or_z: V = +16 comment_1: SOURCE IS QUITE VARIABLE comment_2: PARTICULARLY IN THE ULTRAVIOLET fluxnum_1: 1 fluxval_1: V = 11.6 +/- 0.5, TYPE = K7 IV fluxnum_2: 1 fluxval_2: A(V) = 1.0 +/- 0.3, B-V = 1.1 +/- 0.3 fluxnum_3: 1 fluxval_3: F-LINE(1550) = 1 +/- 0.5 E-13 fluxnum_4: 1 fluxval_4: W-LINE(1550) = 1 +/- 0.5 fluxnum_5: 1 fluxval_5: F-LINE(2880) = 9 +/- 1 E-13 fluxnum_6: 1 fluxval_6: W-LINE(2880) = 2.4 +/- 0.3 ! targnum: 2 name_1: DF-TAU name_2: GSC-525 descr_1: A,156,139 pos_1: PLATE-ID=000L, pos_2: RA = 04H 27M 02.80S +/- 0.3S, pos_3: DEC = +25D 42' 23.11" +/- 0.3S equinox: 2000 rv_or_z: V = +16 comment_1: SOURCE IS QUITE VARIABLE comment_2: PARTICULARLY IN THE ULTRAVIOLET fluxnum_1: 1 fluxval_1: V = 11.8 +/- 0.5, TYPE = K7 IV fluxnum_2: 1 fluxval_2: A(V) = 1.0 +/- 0.3, B-V = 1.1 +/- 0.3 fluxnum_3: 1 fluxval_3: F-LINE(1550) = 1.5 +/- 0.5 E-13 fluxnum_4: 1 fluxval_4: W-LINE(1550) = 1 +/- 0.5 fluxnum_5: 1 fluxval_5: F-LINE(2880) = 1 +/- 1 E-12 fluxnum_6: 1 fluxval_6: W-LINE(2880) = 2 +/- 0.5 ! targnum: 3 name_1: DR-TAU name_2: GSC-1233 descr_1: A,156,139 pos_1: PLATE-ID=00FI, pos_2: RA = 04H 47M 06.22S +/- 0.3S, pos_3: DEC = +16D 58' 43.39" +/- 0.3S equinox: 2000 rv_or_z: V = +16 comment_1: SOURCE IS QUITE VARIABLE comment_2: PARTICULARLY IN THE ULTRAVIOLET fluxnum_1: 1 fluxval_1: V = 11.05 +/- 0.5, TYPE = M0 IV fluxnum_2: 1 fluxval_2: A(V) = 1.0 +/- 0.3, B-V = 0.8 +/- 0.2 fluxnum_3: 1 fluxval_3: F-LINE(1550) = 1 +/- 0.5 E-13 fluxnum_4: 1 fluxval_4: W-LINE(1550) = 1 +/- 0.5 fluxnum_5: 1 fluxval_5: F-LINE(2880) = 1.3 +/- 1 E-12 fluxnum_6: 1 fluxval_6: W-LINE(2880) = 2 +/- 0.5 ! targnum: 4 name_1: RW-AUR name_2: GSC-955 descr_1: A,156,139 pos_1: PLATE-ID=00DH, pos_2: RA = 05H 07M 49.51S +/- 0.3S, pos_3: DEC = +30D 24' 05.47" +/- 0.3S equinox: 2000 rv_or_z: V = +16 comment_1: SOURCE IS QUITE VARIABLE comment_2: PARTICULARLY IN THE ULTRAVIOLET fluxnum_1: 1 fluxval_1: V = 10.35 +/- 0.5, TYPE = K5 IV fluxnum_2: 1 fluxval_2: A(V) = 1.0 +/- 0.3, B-V = 0.7 +/- 0.2 fluxnum_3: 1 fluxval_3: F-LINE(1550) = 2 +/- 0.5 E-13 fluxnum_4: 1 fluxval_4: W-LINE(1550) = 1.5 +/- 0.5 fluxnum_5: 1 fluxval_5: F-LINE(2880) = 8 +/- 2 E-13 fluxnum_6: 1 fluxval_6: W-LINE(2880) = 2.8 +/- 0.4 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: BP-TAU config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 5.4S priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 2; ONBOARD ACQ FOR 1.3-1.6 ! linenum: 1.300 targname: BP-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G270M wavelength: 2800 num_exp: 2 time_per_exp: 5M s_to_n: 10 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 1.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1400 num_exp: 1 time_per_exp: 1M priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2; CALIB FOR 1.5; req_2: SEQ 1.4-1.5 NO GAP ! linenum: 1.500 targname: BP-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1400 num_exp: 6 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 1.600 targname: BP-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 5 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 2.000 targname: DF-TAU config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 3.6S priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 2; ONBOARD ACQ FOR 2.3-2.7 ! linenum: 2.300 targname: DF-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G270M wavelength: 2800 num_exp: 2 time_per_exp: 5M s_to_n: 10 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 2.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1400 num_exp: 1 time_per_exp: 1M priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2; CALIB FOR 2.5; req_2: SEQ 2.4-2.5 NO GAP ! linenum: 2.500 targname: DF-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1400 num_exp: 4 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 2.600 targname: DF-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 4 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 2.700 targname: DF-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1345 num_exp: 5 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 3.000 targname: DR-TAU config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 2; ONBOARD ACQ FOR 3.3-3.8 ! linenum: 3.300 targname: DR-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G270M wavelength: 2800 num_exp: 1 time_per_exp: 5M s_to_n: 10 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 3.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1400 num_exp: 1 time_per_exp: 1M priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2; CALIB FOR 3.5; req_2: SEQ 3.4-3.5 NO GAP ! linenum: 3.500 targname: DR-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1400 num_exp: 6 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 3.600 targname: DR-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 6 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 3.700 targname: DR-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1345 num_exp: 5 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 3.800 targname: DR-TAU config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1650 num_exp: 4 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 4.000 targname: RW-AUR config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 2; ONBOARD ACQ FOR 4.3-4.6 ! linenum: 4.300 targname: RW-AUR config: HRS opmode: ACCUM aperture: 2.0 sp_element: G270M wavelength: 2800 num_exp: 1 time_per_exp: 5M s_to_n: 10 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 4.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1400 num_exp: 1 time_per_exp: 1M priority: 2 param_1: STEP-PATT=DEF req_1: CYCLE 2; CALIB FOR 4.5; req_2: SEQ 4.4-4.5 NO GAP ! linenum: 4.500 targname: RW-AUR config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1400 num_exp: 3 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! linenum: 4.600 targname: RW-AUR config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 3 time_per_exp: 5M s_to_n: 10 fluxnum_3: 1 priority: 1 param_1: STEP-PATT=DEF req_1: CYCLE 2 ! ! end of exposure logsheet ! No scan data records found