UVCS MISSION LOG ---------------- Date: 05 October 2005 ----- Last revision: 17 November 2005 (Wu) -------------- File Name: 2005.10.06.a.log ---------- Compiled by: M. Uzzo, R .Wu ------------ UVCS Activity: JOP 175 Observation of Extended Filaments at the -------------- Limb for 06 - 07 October 2005 Load JOP 175 Observation of Extended Filaments at the Limb for 07 October 2005 SOHO Activity: -------------- EOF Staff: J. Raymond: Lead Scientist ---------- R. Wu: Commander M. Uzzo: Planner Y.-K. Ko Command file: 05.10.05.21:32:00.cmd.log 05.10.06.16:50:00.cmd.log Activity: --------- 1) Extended Filaments at the Limb Sequence: 05.09_StrObs.tcl, sw = 1 SCI_SPEC: From JOP Description found at the following URL: http://soho.nascom.nasa.gov/soc/JOPs/jop175.txt Note: Some information may be obsolete. Draft received 19 February 2004. SOC added UVCS details & POC 23 February 2004. SCIENTIFIC GOALS: (1) To relate the magnetic field morphology of an erupting filament to the structure observed as the white-light CME; (2) Does the fluxrope exist prior to the eruption? REQUESTED OBSERVATIONS: Target-of-opportunity. Long, non-active region, filament during West limb transit (e.g., polar crown, although any extended filament will suffice) -EIT (304A in CME watch mode, full-frame) -TRACE (195A CME watch mode, framed as 02Jun1998 EIT example) -LASCO synoptic mode -UVCS (C III, O VI and Ly beta) Others? POINTS-OF-CONTACT: St. Cyr, Schrijver, Gurman, J. Raymond SCIENTIFIC RATIONALE: Attached is a partial frame EIT 195 image from the June 2, 1998 eruption of the south polar crown filament eruption. Plunkett et al (2000, SolPhys, 194,371-391) described this event and demonstrated that the "cusp" or concave-out shape above the filament was visible for many hours in EIT before the eruption. The cusp appears to be the concave-outward portion of the form we call a fluxrope in LASCO CMEs. We are aware of a few more of these pre-eruption shapes above filaments, but the EIT temporal resolution (and the geometry?) is typically not sufficient to determine when the cusp appears above the prominence. OBS_PROG: Primary: Sub Obj: SCI_OBJ: Primary: Sub Obj: OBJ: Streamer CMP_NAME: JOP 175, Extended Filaments at the Limb, LASCO; EIT; UVCS; TRACE(S/C) CMP_NUM: 7135 Duration: start: 2005.10.06.10:37 end: 2005.10.07.04:55 ONUMs = 21786 (320 exps) 21787 (80 exps) 21788 (80 exps) 21789 (8 exps) 21790 (40 exps) Instrument configuration: - Pointing: Sun center - Spacecraft Roll: 0 Degrees - Roll: 48 Degrees (27510) - Mirror/Occulter: 1.75 Ro 1.5 mm overocculting - LYA Slit: 50 um - OVI Slit: 150, 50 um - LYA GRTPOS: 100000 - OVI GRTPOS: 232100, 86600, 67500, 164600, 223500 - OVI MCP Voltage: 200 - OVI mask: OVI_str_164_225 in slot 6 msk_000303_OVI in slot 3 Fits Files: q05.10.06.10:36:27.ovi.dat q05.10.06.21:38:46.ovi.dat q05.10.07.00:26:14.ovi.dat q05.10.07.03:13:39.ovi.dat q05.10.07.03:31:21.ovi.dat 2) Extended Filaments at the Limb Sequence: 05.09_StrObs.tcl, sw = 1 SCI_SPEC: From JOP Description found at the following URL: http://soho.nascom.nasa.gov/soc/JOPs/jop175.txt Note: Some information may be obsolete. Draft received 19 February 2004. SOC added UVCS details & POC 23 February 2004. SCIENTIFIC GOALS: (1) To relate the magnetic field morphology of an erupting filament to the structure observed as the white-light CME; (2) Does the fluxrope exist prior to the eruption? REQUESTED OBSERVATIONS: Target-of-opportunity. Long, non-active region, filament during West limb transit (e.g., polar crown, although any extended filament will suffice) -EIT (304A in CME watch mode, full-frame) -TRACE (195A CME watch mode, framed as 02Jun1998 EIT example) -LASCO synoptic mode -UVCS (C III, O VI and Ly beta) Others? POINTS-OF-CONTACT: St. Cyr, Schrijver, Gurman, J. Raymond SCIENTIFIC RATIONALE: Attached is a partial frame EIT 195 image from the June 2, 1998 eruption of the south polar crown filament eruption. Plunkett et al (2000, SolPhys, 194,371-391) described this event and demonstrated that the "cusp" or concave-out shape above the filament was visible for many hours in EIT before the eruption. The cusp appears to be the concave-outward portion of the form we call a fluxrope in LASCO CMEs. We are aware of a few more of these pre-eruption shapes above filaments, but the EIT temporal resolution (and the geometry?) is typically not sufficient to determine when the cusp appears above the prominence. OBS_PROG: Primary: Sub Obj: SCI_OBJ: Primary: Sub Obj: OBJ: Streamer CMP_NAME: JOP 175, Extended Filaments at the Limb, LASCO; EIT; UVCS; TRACE(S/C) CMP_NUM: 7135 Duration: start: 2005.10.07.04:57 end: 2005.10.07.23:14 ONUMs = 21791 (319 exps) 21792 (80 exps) 21793 (80 exps) 21794 (8 exps) 21795 (40 exps) Instrument configuration: - Pointing: Sun center - Spacecraft Roll: 0 Degrees - Roll: 48 Degrees (27510) - Mirror/Occulter: 1.75 Ro 1.5 mm overocculting - LYA Slit: 50 um - OVI Slit: 150, 50 um - LYA GRTPOS: 100000 - OVI GRTPOS: 232100, 86600, 67500, 164600, 223500 - OVI MCP Voltage: 200 - OVI mask: OVI_str_164_225 in slot 6 msk_000303_OVI in slot 3 Fits Files: q05.10.07.04:56:09.ovi.dat q05.10.07.15:58:28.ovi.dat q05.10.07.18:45:56.ovi.dat q05.10.07.21:33:21.ovi.dat q05.10.07.21:51:03.ovi.dat