! $Id: 5358,v 4.1 1994/07/27 17:03:06 pepsa Exp $ coverpage: title_1: THE CHROMOSPHERE OF ALPHA TAU - CYCLE 4 MEDIUM sci_cat: COOL STARS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO pi_fname: KENNETH pi_mi: G. pi_lname: CARPENTER pi_inst: NASA GODDARD LASP pi_country: USA hours_pri: 6.00 num_pri: 1 hrs: Y funds_amount: 40163 funds_length: 12 off_fname: STEPHEN off_mi: S. off_lname: HOLT off_title: DIR. OF SPACE SCI. off_inst: 2856 off_addr_1: CODE 600 off_city: GREENBELT off_state: MD off_zip: 20771 off_country: USA off_phone: (301)-286-6066 ! end of coverpage abstract: line_1: We propose observations of the K5 III star Alpha Tau using the line_2: Goddard High-Resolution Spectrograph (GHRS), to follow-up on the line_3: exciting initial SAO observations of this star and the SV line_4: observations of the K5 III hybrid star Gamma Dra. These data will line_5: also allow a detailed comparison of its spectrum and the line_6: thermodynamic properties of its outer atmosphere with those of the line_7: cooler M giant and supergiant stars Gamma Cru and Alpha Ori, observed line_8: during previous cycles. We shall check for variations in the line_9: C II downflow discovered in the SAO observations and search for line_10: evidence of systematic flows in other emission lines. We shall make line_11: detailed comparisons of the chromospheric emission lines and wind line_12: signatures in the UV spectra of two stars of the same spectral class, line_13: where one is a hybrid and one is not. We shall search for evidence line_14: of shocks and/or propagating waves in the line variations predicted line_15: by our recent calculations. We will also determine the variation line_16: of wind velocity with height using semi-empirical non-LTE models line_17: assuming spherical symmetry, search for evidence of circumstellar and line_18: interstellar absorptions on resonance lines of O I, Fe II, and Mg II, line_19: and compare the short-wavelength continuum measured in this star with line_20: that detected in observations of Gamma Dra, Gamma Cru and Alpha Ori. ! ! end of abstract general_form_proposers: lname: CARPENTER fname: KENNETH title: PI mi: G. inst: NASA GODDARD LASP country: USA ! lname: JUDGE fname: PHILIP mi: G. inst: HIGH ALTITUDE OBSERVATORY country: USA ! lname: CUNTZ fname: MANFRED inst: HIGH ALTITUDE OBSERVATORY country: USA ! lname: BROWN fname: ALEXANDER inst: U.COLORADO JILA country: USA ! lname: ROBINSON fname: RICHARD mi: D. inst: COMPUTER SCIENCES CORPORATION country: USA ! lname: WAHLGREN fname: GLENN mi: M. inst: COMPUTER SCIENCES CORPORATION country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observations requested are: line_3: GHRS Central line_4: grating Wavelength(s) Aperture Exposure Time(s) Strong Features line_6: G270M 2345 SSA 20 min C II]/Si II] line_7: G160M 1296 SSA 40 min Fe II/O I line_8: G160M 1550 SSA 60 min C IV/CO/contin. line_9: G160M 1655 SSA 40 min C I/O I/O III line_10: G200M 1994 SSA 20 min C III/C I] line_11: G270M 2753 SSA 10.9 min Fe II line_12: ECH-B 2799 SSA 14.51 min Fe II/Mg II line_13: G270M 2345 SSA 20 min C II]/Si II] line_15: The G270M 2345 A exposures will be taken at the start and end line_16: of the main observing session to check for short term changes in the line_17: chromospheric turbulence and flow velocities. line_19: Each exposure will be taken using FP-SPLIT=STD such that each of line_20: the subexposures will be no longer than five minutes in duration line_21: to minimize geomagnetic and thermal drifts in the line_22: spectrograph and to allow a search for chromospheric variations on a line_23: very short time scale. ! question: 3 section: 2 line_1: The project is pure Cycle 4: line_3: Primary Hours: Parallel Hours: Exposures: line_4: 5.96 0.0 8 ! question: 4 section: 1 line_1: The data required for this program consist of UV spectra not obtainable line_2: from the ground. IUE has been used to study this star to the limits of line_3: its ability (e.g. Brown and Jordan, 1981, MNRAS, 191,37; Judge, 1986, line_4: MNRAS, 223, 239). Further progress in the modelling process requires line_5: observations which only the GHRS can provide. For example, to search line_6: for weak CO absorption features and to study the continuum shape in the line_7: far UV requires high sensitivity detector with a very low background line_8: noise and small fixed pattern noise. Studying the shapes af the line_9: spectral lines for turbulence and small amplitude bulk flows requires a line_10: high S/N, large dynamic range and a very accurate wavelength line_11: calibration. A small number of exposures have been obtained with the line_12: GHRS as part of the Science Assessment Program which clearly line_13: demonstrate the increased sensitivity, wavelength resolution, dynamic line_14: range and S/N characteristics of the GHRS over that obtainable with the line_15: IUE (Carpenter et al. 1991, Ap.J. (letters), 377, L45). ! question: 5 section: 1 line_1: The two C II] G270M exposures (at 2345 A) should be taken at the line_2: beginning and end of the observation sequence to allow line_3: the study of changes in turbulence, flow velocities and line line_4: profiles, all of which are sensitive probes of shock and wave passage line_5: through the atmosphere. The exposure logsheet contains "SEQ" line_6: special requirements to ensure the proper scheduling and no special line_7: handling should be required. ! question: 6 section: 1 line_1: We require the highest possible wavelength accuracy in order to measure line_2: absolute flow velocities in the chromosphere, wind and circumstellar shell of line_3: our target star (down to the 1 km/sec level in the medium and echelle line_4: observations) as well as aiding in the identification of the many weak features line_5: we expect in the low resolution data. Experience with SV and SAO data line_6: (Carpenter et al. 1991, HST Workshop) has demonstrated that the default line_7: calibration will produce uncertainties of up to 3 diodes due to magnetic and line_8: thermal drifts within the spectrograph. Using internal Pt lamp spectra taken line_9: during the SPYBAL procedures we can estimate the amount of drift and can line_10: therefore reduce the degree of uncertainty to about 0.5 diodes. To obtain the line_11: greatest possible wavelength accuracy we require dedicated WAVECAL exposures line_12: using the internal Pt lamps to be connected to each GHRS science exposure. line_13: Experience has shown that with care calibrations good to 0.1 diode can be line_14: obtained using this data. To do this the wavelength calibrations must be taken line_15: at the same carrousel position and close in time to the science exposures to line_16: remove uncertainties caused by the geomagnetic (GIMP) and thermal drifts which line_17: move the image around on the GHRS photocathode. Long exposures must be broken line_18: into time sequences of 5 minute integrations so that the drifts can be line_19: identified and corrected. ! ! question: 8 section: 1 line_1: none ! question: 9 section: 1 line_1: a. List HST program numbers and titles, and specify whether they are line_2: related to this project or not. line_4: GTO 1195: Outer Atmospheres of Cool Luminous Stars - Cycle 0 (Alpha Ori) line_5: 3212: Outer Atmospheres of Cool Luminous Stars - Cycle 1 (Gamma Cru) line_7: GTO 1198/4251 & 3934: Physical Conditions and Velocity Structures in the Red line_8: Giant Winds in the Binaries CI Cyg and EG And - Cycle 2 (2 targets) line_10: GTO 1199: Alpha Ori Team Project - Cycle 1 line_12: These proposals represent the GTO science program, as adjusted for line_13: spherical aberration, of GHRS IDT Co-I K. Carpenter. Programs 1195, line_14: 3212, and 1199 are related to this proposal. Proposals 1198/4251 & line_15: 3934 are studies of symbiotic stars and not directly related to the line_16: current proposal. SAO program 3023 (Alpha Tau) observations have been line_17: used to assess the feasibility of programs such as these which involve line_18: observations of narrow emission-line sources (see the Ap.J. reference line_19: below). NO FURTHER OBSERVATIONS OF ALPHA TAU ARE INCLUDED IN THE GTO line_20: PROPOSALS, AND NO ADDITIONAL GTO OBSERVATIONS, BEYOND THE CYCLE 0-1 line_21: OBSERVATIONS LISTED ABOVE, ARE PLANNED OF SINGLE COOL, LUMINOUS STARS. ! question: 9 section: 2 line_1: b. Summarize the main results obtained from previous related programs. line_3: Highlights include 1) the unambiguous detection of a far-UV continuum line_4: in Alpha Ori and Gamma Cru, which will provide a very important and line_5: previously unrecognized diagnostic of their chromospheric plasmas line_6: (formation temperature in Alpha Ori ranges from 3500-5000 K and line_7: increases steadily with decreasing wavelength), 2) the discovery of line_8: circumstellar CO (4th positive A-X system) absorption bands superposed line_9: on the far-UV continuum from Alpha Ori, providing a probe of regions of line_10: the circumstellar shell not available at visible or IR wavelengths line_11: (initial analysis indicates T=500 K, Vturb=5 km/s, N(CO)=1.0e18 cm-2), line_12: 3) detection of myriad new Fe II fluorescent line products, producing line_13: by Lyman Alpha radiation in Alpha Ori, 4) the determination that the O line_14: I and C I resonance line flux deficiencies are due to self-absorption line_15: in the chromosphere, 5) the determination that the differing Mg II (UV line_16: 1) line asymmetries are due to differing velocity shifts between the line_17: emission and self-absorption components rather than primarily due to line_18: overlying circumstellar absorption from Fe I and Mn I, and 5) the first line_19: direct measurement of the chromospheric turbulence (24 km/sec) and the line_20: detection of a downflow of about 4 km/sec in chromospheric C II] plasma line_21: in Alpha Tau. ! question: 9 section: 3 line_1: c. List publications resulting from the above data (Format: Title, line_2: Authors,Journal, Volume, Page, and Year.) line_4: Results have been presented: in the Ap.J. & MNRAS, at AAS meetings line_5: (1/91, 5/91 1/92, 1/93, & 6/93), the HST Joint Discussion at the IAU line_6: General Assembly (7/91), the 7th Cambridge Cool Star Workshop (10/91), line_7: and at both HST Workshops (5/91 & 7/92), including two invited reviews line_8: (AAS 1/91 and Cool Star Workshop 10/91). line_10: "GHRS Observations of Cool, Low-Gravity Stars. I. The Far-UV Spectrum of line_11: Alpha Ori (M2 Iab)", Carpenter, K., Robinson, R., Wahlgren, G., Linsky, J., line_12: and Brown, A., 1993 Ap.J., submitted. line_14: "A Search for Proton Beams Druing Flares on AU Mic", Robinson, R., line_15: Carpenter, K., Woodgate, B.W., and Maran, S.P. 1993 ApJ, in press. line_17: "Detection of A Proton Beam During the Impulsive Phase of A Stellar Flare," line_18: Woodgate, B., Robinson, R., Carpenter, K., Maran, S., and Shore, S. line_19: 1993 ApJ (Letters), 397, L95. line_21: "First Results from the Goddard High Resolution Spectrograph: The Chromosphere line_22: of Alpha Tauri", Carpenter, K., Robinson, R., Wahlgren, G., Ake, T., Linsky, line_23: J., Brown, A., and Walter, F., Ap.J. (Letters), 377, L45, 1991. ! question: 9 section: 4 line_1: "Si II Emission Line Diagnostics," Judge, P. G., Carpenter, K. G., and line_2: Harper, G.M., MNRAS, 253, 123, 1991. line_4: "Early Scientific Results from the Goddard High Resolution Spectrograph" line_5: Carpenter, K. G. , Invited Review presented at the AAS Meeting, 1/13-17/91. line_7: "GHRS Chromospheric Emission Line Spectra of the Red Giant Alpha Tau" line_8: Carpenter, K. G., Robinson, R. D., Ebbets, D. C., Brown, A., and Linsky, J., line_9: in `The First Year of HST Observations,' 1991. line_11: "Chromospheres and Winds of Cool Stars", Carpenter, K.G., IAU General Assembly line_12: Joint Discussion, 'First Results from the Hubble Space Telescope', 7/31/91. line_14: "HST Observations of Late-Type Stars," (Invited Review) Carpenter, K. G., in line_15: `Proceedings of the 7th Cambridge Workshop on Cool Stars, Stellar Systems, and line_16: the Sun,' eds. M. Giampapa & J. Bookbinder, A.S.P. Conference Series, 26, 17, line_17: 1992. line_19: "Molecular Absorption in the UV Spectrum of Alpha Ori," Wahlgren, G. M., line_20: Robinson, R. D., and Carpenter, K. G., Proceedings of the Seventh line_21: Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, eds. M. Giampapa line_22: and J. Bookbinder, A.S.P. Conference Series, 26, 37, 1992. ! question: 9 section: 5 line_1: "The Chromosphere and Circumstellar Shell of Alpha Orionis as Observed with the line_2: Goddard High Resolution Spectrograph," Carpenter, K. G., Robinson, R. D., line_3: Wahlgren, G. M., Linsky, J. L., Brown, A., in Science with the Hubble line_4: Space Telescope, eds. P. Benvenuti and E. Schreier, ESO Conference and Workshop line_5: Proceedings No. 44, 387, 1992. line_7: "Plasma Flows in the Outer Atmosphere of Alpha Ori," Carpenter, K. G., line_8: Robinson, R. D., Wahlgren, G. M., Brandt, J.C., Linsky, J. L., Ebbets, D. and line_9: Weymann, R., BAAS, 24, #4, 1207, 1992. line_11: "The Ultraviolet Photospheric Spectrum of Alpha Orionis," Wahlgren, G. M., line_12: Robinson, R. D., and Carpenter, K. G., BAAS, 24, #4, 1280, 1992. line_14: "GHRS Spectroscopy of Cool Stars. I. O I and CO as Diagnostics of line_15: Winds and Circumstellar Shells" Carpenter, K., Robinson, R., Ebbets, D., line_16: Brown, A., Linsky, J., BAAS, 23, #2, 910, 1991. line_18: "GHRS Spectroscopy of Cool Stars. II. Gamma Draconis," Brown, A., line_19: Linsky, J., Carpenter, K., Robinson, R., Ebbets, D., BAAS, 23, #2, 910, 1991. line_21: "Molecular Absorption in the Ultraviolet Spectrum of Alpha Ori," Wahlgren, line_22: G.M., Robinson, R. D., and Carpenter, K. G., BAAS, 23, #4, 1386, 1991. line_23: (plus others) ! 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 VAX cluster is available for line_3: data reduction and analysis at GSFC. ! !end of general form text general_form_address: lname: CARPENTER fname: KENNETH mi: G. category: PI inst: NASA Goddard LASP addr_1: CODE 681 addr_2: NASA/GSFC - LAB. FOR ASTRONOMY AND SOLAR PHYSICS city: GREENBELT state: MD zip: 20771 country: USA phone: (301)-286-3453 telex: 89675 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD29139 name_2: ALPHA-TAU descr_1: A,140 pos_1: RA=04H35M55.24S+/-0.1", pos_2: DEC=+16D30'33.39"+/-0.1" equinox: 2000.0 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 2000.00 ra_pm_val: 0.004500 ra_pm_unct: 0.001000 dec_pm_val: -0.1890 dec_pm_unct: 0.0010 an_prlx_val: 0.0540 an_prlx_unct: 0.0050 rv_or_z: V=+54 comment_1: NOTE: RA PROPER MOTION IS comment_2: IN SEC OF TIME/YR **** comment_3: COORDINATES ARE FROM HIPPARCOS CAT. fluxnum_1: 1 fluxval_1: V=0.84+/-.2,TYPE=K5 III fluxnum_2: 2 fluxval_2: F(1314)=3.E-14 fluxnum_3: 3 fluxval_3: F(1655)=7.7E-13 fluxnum_4: 4 fluxval_4: F(1994)=4.E-13 fluxnum_5: 5 fluxval_5: F(2327)=4.E-12 fluxnum_6: 6 fluxval_6: F(2759)=1.5E-12 fluxnum_7: 7 fluxval_7: F(2770)=1.5E-12 fluxnum_8: 8 fluxval_8: F(2799)=8.E-11 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 10.000 targname: HD29139 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5, param_2: BRIGHT=RETURN req_1: CYCLE 4 / 10-61; req_2: ONBOARD ACQ FOR 11; req_3: SEQ 10-61 NO GAP comment_1: STEP TIME = 0.4 SEC comment_2: EXPECT 226 CTS/400 MSEC ! linenum: 11.000 targname: HD29139 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 40.0S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 12-61 comment_1: STEP-TIME=1.6SEC; comment_2: EXP. TIME ASSUMES 3X3 SEARCH. ! linenum: 12.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2345.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 13 NO SLEW; req_2: SEQ 12-13 NON-INT ! linenum: 13.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2345.0 num_exp: 1 time_per_exp: 20.0M s_to_n: 35 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD comment_1: FIRST C II EXPOSURE (1 OF 2) ! linenum: 31.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1296 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 32 NO SLEW; req_2: SEQ 31-32 NON-INT ! linenum: 32.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1296 num_exp: 1 time_per_exp: 20.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 32.100 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1296 num_exp: 1 time_per_exp: 20.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 32.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 32.7 NO SLEW; req_2: SEQ 32.3-32.7 NON-INT ! linenum: 32.700 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 20.0M s_to_n: 8 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 32.800 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1550 num_exp: 2 time_per_exp: 20.0M s_to_n: 8 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 34.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1655 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 34.7 NO SLEW; req_2: SEQ 34.3-34.7 NON-INT ! linenum: 34.700 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1655 num_exp: 1 time_per_exp: 20.0M s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 34.800 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1655 num_exp: 1 time_per_exp: 20.0M s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 37.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G200M wavelength: 1994 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 38.0 NO SLEW; req_2: SEQ 37-38 NON-INT ! linenum: 38.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G200M wavelength: 1994 num_exp: 1 time_per_exp: 20.0M fluxnum_1: 4 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 39.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2753 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 40 NO SLEW; req_2: SEQ 39-40 NON-INT ! linenum: 40.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2753 num_exp: 1 time_per_exp: 10.9M s_to_n: 30 fluxnum_1: 6 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 53.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B20 wavelength: 2799.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 54 NO SLEW; req_2: SEQ 53-54 NON-INT ! linenum: 54.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B20 wavelength: 2799.0 num_exp: 1 time_per_exp: 14.51M fluxnum_1: 8 priority: 1 param_1: STEP-PATT=7, param_2: FP-SPLIT=STD ! linenum: 60.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2345.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 61 NO SLEW; req_2: SEQ 60-61 NON-INT ! linenum: 61.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2345.0 num_exp: 1 time_per_exp: 20.0M s_to_n: 35 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD comment_1: SECOND C II EXPOSURE (2 OF 2) ! ! end of exposure logsheet ! No scan data records found