! File: 4183C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:12:25:39 coverpage: title_1: DYNAMICS AND ENERGY BALANCE IN STELLAR TRANSITION REGIONS title_2: LATER CYCLE OBSERVATIONS sci_cat: STELLAR ASTROPHYSICS sci_subcat: COOL STARS proposal_for: GTO/HRS cont_id: 1176 pi_fname: JEFFREY pi_mi: L. pi_lname: LINSKY pi_inst: COLORADO, UNIVERSITY OF pi_country: USA pi_phone: (303)492-7838 keywords_1: STELLAR CHROMOSPHERES, STELLAR TRANSITION REGIONS, F-M keywords_2: DWARF STARS, G-K GIANT STARS, STELLAR ACTIVITY hours_pri: 2.55 num_pri: 1 pi_position: ASTROPHYSICIST ! end of coverpage abstract: line_1: Late-type stars with convective zones and magnetic fields line_2: have plasma above the photosphere heated to temperatures line_3: above 10,000 K. We will use the GHRS to study the dynamics, line_4: energy balance, and nonradiative heating rates in these hot line_5: regions for a sample of late-type stars spanning a range of line_6: spectral type and luminosity. We will study the dynamics of line_7: stellar transition regions by measuring the redshifts, line_8: indicative of downflows, with high precision in lines of line_9: C III, C IV, Si IV, and O IV. The energy balance and local line_10: heating rates in stellar transition regions will be derived line_11: from an emission measure analysis of emission line fluxes line_12: and electron densities inferred from density-sensitive line line_13: ratios. Cycle 0 observations of the RS CVn system Capella line_14: show that the GHRS can measure ALL of the UV intersystem line_15: lines of Si III, C III, O III, N III, O IV, and S IV, which line_16: are useful density diagnostics. These data may require line_17: atmospheric models with two components (quiet and active line_18: regions). ! ! end of abstract general_form_proposers: lname: BROWN fname: ALEXANDER inst: COLORADO, UNIVERSITY OF country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: COLORADO, UNIVERSITY OF country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We intend to observe 6 stars with the HRS with 2 grating settings each at line_2: low dispersion and 4 grating settings each at moderate dispersion. Two targets line_3: (HR 1099 and Capella) are spectroscopic binary systems and are to be observed line_4: at 1 or 2 phases each. HR 1099 is to be observed at a PHI = 0.75 quadrature. line_5: Capella is to be observed at a conjunction (PHI = 0.0 or 0.5) and at a PHI = line_6: 0.25 quadrature. Ephermerides for PHI = 0.0 are line_8: HR 1099: JD (helio) = 2,442,766.069 + 2d.83782E line_9: Capella: JD (helio) = 2,442,039.4 + 104d.0204E line_11: Cycle 2, 3, and 4. line_12: Capella was observed in Cycle 0 and AU Mic and Beta Dra in Cycle 1. ! question: 4 section: 1 line_1: Stellar transition regions can only be observed in the ultraviolet. ! question: 5 section: 1 line_1: Many of these targets are in common with our GTO program "Local line_2: Interstellar Medium and D/H Ratio" or the program "Coronal Flares" for which S. line_3: Maran is the PI. Since these targets are variable and the data from each line_4: program supports the other, we request that observations of the same target for line_5: both programs be contiguous in time with few data gaps. The observations of HR line_6: 1099 and Capella at conjunction and quadrature are to use the orbital radial line_7: velocity differences to seperate the spectra of the component stars. ! question: 7 section: 1 line_1: We have developed extensive computer programs to analyze these spectra line_2: using emission measure and model atmosphere techniques. ! question: 10 section: 1 line_1: Computer analysis codes and postdoctoral research associates to be funded line_2: by the HST GTO program. ! question: 12 section: 1 line_1: The total exposure time for this program assumes the following overhead line_2: times: line_4: ALPHA-CMI 345s line_5: BETA-CET 375s line_6: ALPHA-CEN A 285s line_7: EPSILON-ERI 285s line_8: HR 1099 255s line_9: ALPHA-AUR 690s (total for the two phases) line_10: BETA-DRA 435s line_11: AU-MIC 255s line_12: LAMBDA-AND 255s ! question: 13 section: 1 line_1: We propose to study the dynamics of stellar transition regions by line_2: measuring the redshifts, indicative of downflows, in lines of C III, Si III, C line_3: IV, Si IV, and O IV. The energy balance and heating rates in stellar line_4: chromospheres and transition regions will be derived from an emission measure line_5: analysis of emission line fluxes and densities inferred from density sensitive line_6: line ratio. Stars of interest include dwarf stars of spectral type F-M, line_7: active G and K giants, and RS CVn binary systems. ! !end of general form text 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: 755842JILA ! ! end of general_form_address records fixed_targets: targnum: 4 name_1: HD22049 name_2: EPSILON-ERI descr_1: A,139 pos_1: RA=03H32M55.8S+/-.1S, pos_2: DEC=-09D27'30"+/-1" equinox: 2000 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.065267 ra_pm_unct: 0.000067 dec_pm_val: 0.0190 dec_pm_unct: 0.0010 an_prlx_val: 0.3040 rv_or_z: V=+16 fluxnum_1: 1 fluxval_1: V=3.73 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 20.000 targname: HD22049 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 21; req_2: CYCLE 4/ 20-25; req_3: GROUP 20-25 NO GAP; req_4: SEQ 20-21 comment_1: STEP TIME = 0.4 SEC comment_2: FAINT REVISED 19/MAY/1991 comment_3: FAINT= ! linenum: 21.000 targname: HD22049 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 73.6S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 23-25 comment_1: STEP-TIME=1.6SEC comment_2: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 23.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G200M wavelength: 1900 num_exp: 1 time_per_exp: 32S priority: 2 param_1: STEP-PATT=3 req_1: CALIB FOR 24 NO SLEW; req_2: SEQ 23-24 NO GAP ! linenum: 24.000 targname: HD22049 config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 6 time_per_exp: 327S priority: ^ param_1: STEP-PATT=5 ! linenum: 24.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1640 num_exp: 1 time_per_exp: 32S priority: 2 param_1: STEP-PATT=3 req_1: CALIB FOR 24.5 NO SLEW; req_2: SEQ 24.4-24.5 NO GAP ! linenum: 24.500 targname: HD22049 config: ^ opmode: ^ aperture: 2.0 sp_element: G160M wavelength: 1640 num_exp: 2 time_per_exp: 300S priority: ^ param_1: STEP-PATT=5 ! linenum: 24.900 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 32S priority: 2 param_1: STEP-PATT=3 req_1: CALIB FOR 25.0 NO SLEW; req_2: SEQ 24.9-25.0 NO GAP ! linenum: 25.000 targname: HD22049 config: ^ opmode: ^ aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 4 time_per_exp: 327S priority: ^ param_1: STEP-PATT=5 ! ! end of exposure logsheet ! No scan data records found