! File: 4490C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:14:29:41 coverpage: title_1: THE CHROMOSPHERE OF ALPHA TAU - CYC3 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: 9.35 num_pri: 1 hrs: Y 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: Central line_4: GHRS grating Wavelength(s) Aperture Exposure Time(s) Strong Feature line_6: G160M 1296 SSA 60 min Fe II/O I line_7: G160M 1550 LSA 60 min C IV/CO/contin line_8: G160M 1655 LSA 48 min C I/O I/O III line_9: G200M 1994 LSA 20 min CI] line_10: G270M 2345 SSA 20 min (3x) C II]/Si II] line_11: G270M 2499 SSA 10 min Fluor. Fe II line_12: G270M 2609, 2753, 2803 SSA 10, 5, and 5 min Fe II/MgII/Fe line_13: ECH-B 2596, 2799 SSA 30, 10 min Fe II/Mg II line_15: The G270M 2345 A exposures will be taken at the start, middle and end of the line_16: main observing session to check for short term changes in the chromospheric line_17: turbulence and flow velocities. line_21: The project is pure Cycle 3. The spacecraft time is: line_22: Primary Hours: Parallel Hours: Exposures: line_23: 9.35 0.0 18 ! question: 4 section: 1 line_1: The data required for this program consists of UV spectra not obtainable from line_2: the ground. IUE has been used to study this star to the limits of its ability line_3: (e.g. Brown and Jordan, 1981, MNRAS, 191,37; Judge, 1986, MNRAS, 223, 239) and line_4: a small number of exposures have been obtained with the GHRS as part of the line_5: Science Assessment Program. These observations clearly demonstrate the line_6: increased sensitivity, wavelength resolution, dynamic range and S/N line_7: characteristics of the GHRS over that obtainable with the IUE (Carpenter et al. line_8: 1991, Ap.J. (letters), 377, L45). Only the GHRS is capable of providing us with line_9: the very high precision line profiles, fluxes, and absolute velocities required line_10: for our program. ! question: 5 section: 1 line_1: The three C II] G270M exposures (at 2345 A) should be taken at the line_2: beginning, middle, and end of the SSA 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 also broken line_18: into times sequences of 5 minute integrations so that the drifts can be line_19: identified and corrected. ! question: 7 section: 1 line_1: The data will be reduced and analyzed primarily with software developed at line_2: Goddard for analysis of IUE and GHRS data. Line widths, profiles, and line_3: wavelengths will be carefully measured to extract information on the velocity line_4: structure of the outer atmosphere, including both random non-thermal velocities line_5: and systematic flows. Methods are described in Carpenter et al. (1991 ApJ line_6: Letters, 377, L45) and in Carpenter (1984, ApJ. 285, 181 ). Relative and line_7: absolute fluxes will be measured to estimate densities and temperatures in the line_8: outer atmosphere. Planar and spherical versions of the NLTE MULTI code will line_9: be used to construct model chromospheres and spectra which will be compared line_10: with the observations and used to deduce the actual structure of the stellar line_11: chromosphere. The time dependence of the line profiles will be studied using line_12: the shock models of Cuntz (1987) with updated treatments of radiative transfer line_13: as described by Judge & Cuntz (1992, ApJL, submitted). Both reduced spectra line_14: and inferred chromospheric structures of Alpha Tau and the other giant and line_15: supergiant stars in our sample will be compared to study dependences on Teff line_16: and gravity. ! 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: Physical Conditions and Velocity Structures in the Red Giant line_8: 3934: 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 spherical line_13: abberation, of GHRS IDT Co-I K. Carpenter. Programs 1195, 3212, and 1199 are line_14: related to this proposal. Proposals 1198 & 3934 are studies of symbiotic stars line_15: and not directly related to the current proposal. SAO program 3023 (Alpha Tau) line_16: observations have been used to assess the feasibility of programs such as these line_17: which involve observations of narrow emission-line sources (see the Ap.J. line_18: reference below). NO FURTHER OBSERVATIONS OF ALPHA TAU ARE INCLUDED IN THE GTO line_19: PROPOSALS, AND NO ADDITIONAL GTO OBSERVATIONS, BEYOND THE CYCLE 0-1 line_20: 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 in Alpha line_4: Ori and Gamma Cru, which will provide a very important and previously line_5: unrecognized diagnostic of their chromospheric plasmas (formation temperature line_6: in Alpha Ori ranges from 3500-5000 K and increases steadily with decreasing line_7: wavelength), 2) the discovery of circumstellar CO (4th positive A-X system) line_8: absorption bands superposed on the far-UV continuum from Alpha Ori, providing a line_9: probe of regions of the circumstellar shell not available at visible or IR line_10: wavelengths (initial analysis indicates T=500 K, Vturb=5 km/s, N(CO)=1.0e18 line_11: cm-2), 3) detection of myriad new Fe II fluorescent line products, producing by line_12: Lyman Alpha radiation in Alpha Ori, 4) the determination that the O I and C I line_13: resonance line flux deficiences are due to self-absorption in the chromosphere, line_14: 5) the determination that the differing Mg II (UV 1) line asymmetries are line_15: due to differing velocity shifts between the emission and self-absorption line_16: components rather than primarily due to overlying circumstellar absorption from line_17: Fe I and Mn I, and 5) the first direct measurement of the chromospheric line_18: turbulence (24 km/sec) and the detection of a downflow of about 4 km/sec in line_19: chromospheric C II] plasma 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 meeting (1/91, 5/91 line_5: & 1/92), the HST Joint Discussion at the IAU General Assembly (7/91), the 7th line_6: Cambridge Cool Star Workshop (10/91), and at both HST Workshops (5/91 & 7/92), line_7: including two invited reviews (AAS 1/91 and Cool Star Workshop 10/91). line_9: "First Results from the Goddard High Resolution Spectrograph: The Chromospher line_10: of Alpha Tauri", Carpenter, K., Robinson, R., Wahlgren, G., Ake, T., Linsky, line_11: J., Brown, A., and Walter, F., Ap.J. (Letters), 377, L45, 1991. line_13: "Si II Emission Line Diagnostics," Judge, P. G., Carpenter, K. G., and line_14: Harper, G.M., MNRAS, 253, 123, 1991. line_16: "Early Scientific Results from the Goddard High Resolution Spectrograph" line_17: Carpenter, K. G. , Invited Review presented at the AAS Meeting, 1/13-17/91. line_19: "GHRS Chromospheric Emission Line Spectra of the Red Giant Alpha Tau" line_20: Carpenter, K. G., Robinson, R. D., Ebbets, D. C., Brown, A., and Linsky, J., line_21: in `The First Year of HST Observations,' 1991. ! question: 9 section: 4 line_1: "Chromospheres and Winds of Cool Stars", Carpenter, K.G., IAU General Assembly line_2: Joint Discussion, 'First Results from the Hubble Space Telescope', 7/31/91. line_4: "HST Observations of Late-Type Stars," (Invited Review) Carpenter, K. G., in line_5: `Proceedings of the 7th Cambridge Workshop on Cool Stars, Stellar Systems, an line_6: the Sun,' eds. M. Giampapa & J. Bookbinder, A.S.P. Conference Series, 26, 17, line_7: 1992. line_9: "Molecular Absorption in the UV Spectrum of Alpha Ori," Wahlgren, G. M., line_10: Robinson, R. D., and Carpenter, K. G., Proceedings of the Seventh line_11: Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, eds. M. Giampap line_12: and J. Bookbinder, A.S.P. Conference Series, 26, 37, 1992. line_14: "The Chromosphere and Circumstellar Shell of Alpha Orionis as Observed with th line_15: Goddard High Resolution Spectrograph," Carpenter, K. G., Robinson, R. D., line_16: Wahlgren, G. M., Linsky, J. L., Brown, A., in Science with the Hubble line_17: Space Telescope, eds. P. Benvenuti and E. Schreier, in press, 1992. line_19: "The Far-UV Spectrum of Alpha Ori," Carpenter, K. G., Robinson, R. D., line_20: Wahlgren, G. M., Linsky, J.L., and Brown, A., Ap. J., submitted, 1992. ! question: 9 section: 5 line_1: line_2: "GHRS Spectroscopy of Cool Stars. I. O I and CO as Diagnostics of line_3: Winds and Circumstellar Shells" Carpenter, K., Robinson, R., Ebbets, D., line_4: Brown, A., Linsky, J., BAAS, 23, #2, 910, 1991. line_6: "GHRS Spectroscopy of Cool Stars. II. Gamma Draconis," Brown, A., line_7: Linsky, J., Carpenter, K., Robinson, R., Ebbets, D., BAAS, 23, #2, 910, 1991. line_9: "Molecular Absorption in the Ultraviolet Spectrum of Alpha Ori," Wahlgren, line_10: G.M., Robinson, R. D., and Carpenter, K. G., BAAS, 23, #4, 1386, 1991. ! 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=04H33M02.896S+/-0.1", pos_2: DEC=+16D24'37.51"+/-0.1" equinox: 1950.0 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 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 **** 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 3 / 10-74; req_2: ONBOARD ACQ FOR 11; req_3: SEQ 10-74 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 12-74 comment_1: CENTER IN SSA AFTER NEW DEFCAL comment_2: STEP-TIME=1.6SEC ! linenum: 12.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2345.5 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: 2345.5 num_exp: 4 time_per_exp: 5.0M s_to_n: 35 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5 comment_1: FIRST C II EXPOSURE (1 OF 3) ! 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 NO GAP ! linenum: 32.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1296 num_exp: 12 time_per_exp: 5.0M s_to_n: 13 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 ! linenum: 33.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2345.5 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 34 NO SLEW; req_2: SEQ 33-34 NON-INT ! linenum: 34.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2345.5 num_exp: 4 time_per_exp: 5.0M s_to_n: 35 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5 comment_1: SECOND C II EXPOSURE (2 OF 3) ! linenum: 35.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2499.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 36 NO SLEW; req_2: SEQ 35-36 NON-INT ! linenum: 36.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2499.0 num_exp: 2 time_per_exp: 5.0M priority: 1 param_1: STEP-PATT=5 ! linenum: 37.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2609.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 38 NO SLEW; req_2: SEQ 37-38 NON-INT ! linenum: 38.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2609 num_exp: 2 time_per_exp: 5.0M priority: 1 param_1: STEP-PATT=5 ! 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: 2 time_per_exp: 5.0M s_to_n: 30 fluxnum_1: 6 priority: 1 param_1: STEP-PATT=5 ! linenum: 41.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2807.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 42 NO SLEW; req_2: SEQ 41-42 NON-INT ! linenum: 42.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2807.0 num_exp: 2 time_per_exp: 5.0M fluxnum_1: 8 priority: 1 param_1: STEP-PATT=5 ! linenum: 51.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B22 wavelength: 2596.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 52 NO SLEW; req_2: SEQ 51-52 NON-INT ! linenum: 52.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B22 wavelength: 2596.0 num_exp: 6 time_per_exp: 5M s_to_n: 27 priority: 1 param_1: STEP-PATT=7 ! 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: 2 time_per_exp: 5M fluxnum_1: 8 priority: 1 param_1: STEP-PATT=7 ! linenum: 60.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2345.5 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: 2345.5 num_exp: 4 time_per_exp: 5.0M s_to_n: 35 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5 comment_1: THIRD C II EXPOSURE (3 OF 3) ! linenum: 71.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 12 time_per_exp: 5.0M s_to_n: 8 priority: 1 param_1: STEP-PATT=5 ! linenum: 72.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1655 num_exp: 9 time_per_exp: 5.0M s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=5 ! linenum: 74.000 targname: HD29139 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1994 num_exp: 2 time_per_exp: 10.0M fluxnum_1: 4 priority: 1 param_1: STEP-PATT=5 ! ! end of exposure logsheet ! No scan data records found