! File: 1180C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:04:55:41 coverpage: title_1: TRANSITION REGIONS IN VERY LATE M DWARFS title_2: CYCLE LATER OBSERVATIONS sci_cat: STELLAR ASTROPHYSICS sci_subcat: COOL STARS proposal_for: GTO/HRS pi_fname: JEFFREY pi_mi: L. pi_lname: LINSKY pi_inst: COLORADO, UNIVERSITY OF pi_country: USA pi_phone: (303) 492-7838 keywords_1: MS STAR, MV STARS, X-RAY STAR, FLARE STAR hours_pri: 2.63 num_pri: 2 pi_position: ASTROPHYSICIST ! end of coverpage abstract: line_1: We propose to search for transition region emission lines indicative of 1.0E+5 line_2: K plasma in the ultraviolet spectra of the coolest M dwarf stars of both the dM line_3: and dMe types. With such data we will study the heating rates and energy line_4: balance in the transition regions of these stars and compare such data with line_5: stars of earlier spectral type. An important question is whether transition line_6: regions disappear or have significantly smaller heating rates in the late M line_7: dwarfs as is suggested by the X-ray data. ! ! end of abstract general_form_proposers: lname: GIAMPAPA fname: MARK inst: NATIONAL SOLAR OBSERVATORY country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: COLORADO, UNIVERSITY OF country: USA ! lname: AMBRUSTER fname: CAROL inst: JILA, UNIVERSITY OF COLORADO country: USA ! lname: MARAN fname: STEPHEN mi: P. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA ! lname: BROWN fname: ALEXANDER inst: JILA, UNIVERSITY OF COLORADO country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: HRS observations of 2 stars are requested with one grating setting line_2: (G140L) for each star using the 2.0" aperture. There are no scheduling line_3: requirements. We are obtaining the data with a time resolution line_4: of 4.5 minutes to study time variability that may be indicative of line_5: flaring. line_6: Note that Targets 5 and its offset star Target 4 are Priority 1, while line_7: Target 3 is Priority 3. ! question: 4 section: 1 line_1: There are no available transition region lines in the visible or infrared. ! question: 6 section: 1 line_1: We request that the observations not be interrupted to determine whether line_2: or not the emission is steady or highly variable indicative of flaring. ! question: 7 section: 1 line_1: We have written computer codes and tested them on available IUE spectra line_2: that determine the emission measure distribution, heating rates, line_3: pressure-temperature distribution, and energy balance for the chromosphere and line_4: transition region from ultraviolet emission line fluxes. ! question: 10 section: 1 line_1: We will supply data analysis and atmospheric modelling computer codes. ! question: 12 section: 1 line_1: The total observing time includes an estimated overhead of 100 seconds per line_2: target. ! question: 13 section: 1 line_1: This program will test the hypothesis that magnetic nonradiative heating line_2: processes become inefficient in the coolest M dwarf stars, including both dM line_3: and dMe stars. We will search for emission lines of C II, Si IV, C IV, and N V line_4: in a sample of 6 very late M dwarf stars and compare the surface fluxes with line_5: those from warmer stars to test the hypothesis. From the observed fluxes we line_6: will derive the emission measure distribution, nonradiative heating rates, and line_7: the local energy balance. ! !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: 755842 JILA ! ! end of general_form_address records fixed_targets: targnum: 4 name_1: GL752B-OFFSET descr_1: A,141 pos_1: RA = 19H 14M 29S +/- 1S, pos_2: DEC = +05D 05' 54" +/- 3" equinox: 1950.00 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.030667 ra_pm_unct: 0.000067 dec_pm_val: -1.4200 dec_pm_unct: 0.0010 an_prlx_val: 0.1730 comment_1: DM3.5E STAR fluxnum_1: 1 fluxval_1: V = 9.12 ! targnum: 5 name_1: GL752B name_2: VB10 descr_1: A,141 pos_1: RA-OFF = +3S +/- 1S, pos_2: DEC-OFF = -72" +/- 3", pos_3: FROM 4 equinox: 1950.00 pm_or_par: N pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_unct: 0.001000 dec_pm_unct: 0.0010 comment_1: DM8E STAR fluxnum_1: 1 fluxval_1: V = 17.38 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: DME targname: # config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1427 num_exp: # time_per_exp: 272S priority: # param_1: STEP-PATT=5 req_1: NON-INT comment_1: EXPOSURE SEQUENCE GIVING comment_2: 4.5 MIN TIME RESOLUTION ! linenum: 13.000 targname: GL752B-OFFSET config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S priority: 1 param_1: SEARCH-SIZE=5 param_2: FAINT=200 req_1: ONBOARD ACQ FOR 14; req_2: CYCLE 4/ 13-17; req_3: GROUP 13-17 NO GAP; req_4: SEQ 13-17 comment_1: STEP TIME = 1 SEC comment_2: FAINT REVISED 20-MAY-1991 ! linenum: 14.000 targname: GL752B-OFFSET config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 73.6S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 15.5-17; comment_1: STEP-TIME=1.6SEC comment_2: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 15.500 targname: GL752B-OFFSET config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1304 num_exp: 2 time_per_exp: 327S priority: 2 param_1: STEP-PATT=5 ! linenum: 15.600 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1574 num_exp: 2 time_per_exp: 300S priority: ^ param_1: ^ ! linenum: 17.000 sequence_1: USE sequence_2: DME targname: GL752B num_exp: 13 time_per_exp: X1 priority: 1 ! ! end of exposure logsheet ! No scan data records found