! $Id: 5306,v 13.1 1994/11/16 19:54:04 pepsa Exp $ coverpage: title_1: MEASUREMENTS OF PROTON BEAMS IN STELLAR FLARES : CYCLE4 MEDIUM sci_cat: COOL STARS sci_subcat: ACTIVE STARS proposal_for: GO pi_fname: BRUCE pi_mi: E pi_lname: WOODGATE pi_inst: NASA GODDARD/LASP pi_country: USA pi_phone: (301) 286-5401 hours_pri: 9.49 num_pri: 1 hrs: Y time_crit: Y off_fname: STEPHEN off_lname: HOLT off_title: DIR. OF SPACE SCI. off_inst: 2856 off_addr_1: CODE 600 off_addr_2: GODDARD SPACE FLIGHT CENTER 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 to observe the H Lyman Alpha profile of the flare line_2: star YZ CMI using the GHRS in the rapid readout mode to line_3: search for evidence of proton beams in stellar flares. Following our line_4: successful detection of a proton beam on the flare star AU Mic during line_5: cycle 1 we now wish to determine how often this phenomenon occurs, line_6: whether proton beams are seen on cooler stars, what is the time history line_7: and emission profile of the beam and whether the proton beam is line_8: energetically dominant during the impulsive phase. ! ! end of abstract general_form_proposers: lname: WOODGATE fname: BRUCE inst: 2866 country: USA ! lname: CARPENTER fname: KENNETH inst: 2866 country: USA ! lname: ROBINSON fname: RICHARD inst: 1780 country: USA ! lname: BROSIUS fname: JEFFREY inst: 3480 country: USA ! lname: HOLMAN fname: GORDON inst: 2866 country: USA ! lname: LINSKY fname: JEFFREY inst: 1764 country: USA ! lname: DANKS fname: ANTHONY inst: 3480 country: USA ! lname: KUNDU fname: MUKUL inst: 2620 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will use the GHRS with the G160M grating and the rapid readout mode line_2: to observe the Lyman alpha wavelength region of the active flare star line_3: YZ CMi with a time resolution of 0.4 seconds. The time line_4: interval was chosen as the smallest time consistent with continuous line_5: data storage on the science tape recorder. The observations will cover line_6: the wavelength range from 1203 to 1240 A and have a spectral resolution line_7: of approximately 10,000. If the low resolution G140L mode becomes line_8: available after the servicing mission, then we plan to request a change line_9: to observe with this grating and the SSA. The lower resolution data line_10: will allow a spectra coverage from 1150 to 1435 Angstroms, which line_11: covers a wide range of strong diagnostic lines such as C III, C II, Si line_12: IV, N V, O V, Fe XII, Fe XXI, CI and OI. ! question: 4 section: 1 line_1: Theory predicts that downstreaming non-thermal protons accelerated line_2: during the stellar flare will charge exchange with ambient hydrogen and line_3: become excited, downstreaming hydrogen atoms. These then emit line_4: red-shifted radiation into the wings of the various hydrogen lines. line_5: While a signature of proton beams should appear in the lines of the line_6: Balmer series, it will be MUCH more detectable in the wing of the Lyman line_7: alpha line because (a) the majority of the photons are emitted at Lyman line_8: alpha and (b) the quiescent stellar background is more than 8 orders of line_9: magnitude larger at the Balmer line wavelengths than at Lyman alpha, so line_10: a faint signal is more easily detected. Furthermore, as line_11: shown by our earlier successful detection of proton beams, the events line_12: may last for only a matter of seconds, requiring rapid line_13: time sequences. The GHRS aboard the HST is the only instrument line_14: currently available which allows high time resolution at the Lyman line_15: alpha wavelengths. ! question: 5 section: 1 line_1: We request scheduling of the HST obsrvations to coordinate with line_2: observations of the star at other wavelengths. Many of the goals of line_3: this project require only the HST observations. However, one major line_4: objective of the program is to determine whether the proton beams are line_5: the energetically dominant transport mechanism. To answer this question line_6: it is necessary to determine the total energy within the flare by line_7: observing at several wavelength regions, particularly in the optical, line_8: EUV and X-rays. For this reason we will be applying for coordinated line_9: observing time from ROSAT and EUVE and a variety of groundbased optical line_10: and radio observatories. In particular, we hope to obtain moderate line_11: resolution spectroscopy of the flares at high time resolution by using line_12: the new GSFC MAMA photon counting detector in a time tagged mode, line_13: where the position and time of each photon is stored on Exabyte tape line_14: for later analysis. Mounted on a large telescope such as the 3.9m line_15: Anglo-Australian Telescope or the McDonald 2.6m, the MAMA will allow line_16: us to obtain spectra with a time resolution which is limited only by line_17: the counting statistics. ! question: 6 section: 1 line_1: NONE ! ! question: 8 section: 1 line_1: NONE ! question: 9 section: 1 line_1: Flare related GO and GTO observations: line_3: GO 2321 - Search for proton acceleration in flare stars - AU Mic line_4: 4214 - Rerun of part of 2321 (cycle 2) line_5: GTO 1158 - Coronal Flares line_7: Carpenter, Maran and Linsky have HST GTO programs which are not devoted line_8: to stellar flares. Limited space prevents us from listing these. line_10: High time resolution observations of the Lyman alpha line on the flare line_11: star AU Mic (GO 2321/4214) showed evidence for a significant increase line_12: in the red wing of the line during the peak of a flare event. There line_13: was no corresponding increase in the blue wing. This effect was first line_14: predicted by Orrall and Zirker in 1976 and results from the presence line_15: of a proton beam accelerated during the impulsive phase of the flare line_16: and streaming down through the atmosphere. The protons charge exchange line_17: with the ambient hydrogen atoms and then emit red-shifted Lyman alpha line_18: photons up to 10 A from line center. Preliminary calculations have line_19: shown that the detected beam may be responsible for transporting a line_20: significant amount of the flare energy. ! question: 10 section: 1 line_1: Software developed by the GHRS IDT and the proposers will be used in line_2: the reduction and analysis of these observations. A VAX cluster is line_3: available for data reduction and analysis at GSFC. ! !end of general form text general_form_address: lname: WOODGATE fname: BRUCE mi: E category: PI inst: 2866 addr_1: CODE 681 addr_2: GODDARD SPACE FLIGHT CENTER city: GREENBELT state: MD zip: 20771 country: USA phone: (301) 286-5401 telex: CHAMP::WOODGATE ! lname: ROBINSON fname: RICHARD mi: D category: CON inst: 1780 addr_1: CODE 681/CSC addr_2: GODDARD SPACE FLIGHT CENTER city: GREENBELT state: MD zip: 20771 country: USA phone: (301) 286-4530 telex: HRS::HRSROBINSON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: YZ-CMI descr_1: A, descr_2: 141,146, pos_1: RA=07H 44M 40.11S +/- 1", pos_2: DEC=+03D 33' 08.25" +/- 1" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.026000 dec_pm_val: -0.4700 an_prlx_val: 0.1650 an_prlx_unct: 0.0080 rv_or_z: V=18 comment_1: FLARE STAR fluxnum_1: 1 fluxval_1: V=11.2+/-1, TYPE=DM4.5E, ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: YZ-CMI config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25.0S fluxnum_1: 1 priority: 1 param_1: LOCATE=YES, param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=5 req_1: CYCLE 4 / 1.0-13.0 ; req_2: AT 21-DEC-94:14:00:00 +/- 11H ; req_3: ONBOARD ACQ FOR 3.0 ; req_4: SEQ 1-13 ; comment_1: STEP-TIME=1.0S , comment_2: EXPECT 500 COUNTS IN STEP TIME ! linenum: 3.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 comment_1: ONE TIME SEQUENCE PER ORBIT ! linenum: 4.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 5.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 6.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 7.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 8.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 9.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 10.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 41M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 11.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 40M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 12.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 35M priority: 1 param_1: SAMPLE-TIME=0.4 ! linenum: 13.000 targname: YZ-CMI config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1295 num_exp: 1 time_per_exp: 29M priority: 1 param_1: SAMPLE-TIME=0.4 ! ! end of exposure logsheet ! No scan data records found