Updated: Sept. 1, 2000 ------------------------ JOP127: High-cadence CME tracking through the corona and interplanetary medium Supported by SOHO-LASCO, EISCAT, Ulysses-SWOOPS/HiScale, Nagoya-Toyakawa, Nancay, Ootacamund, MICA, HASTA, HAO-MKIV, TRACE, SOHO-UVCS, Puschino, Others(?) Authors: G Lawrence (LASCO), A Breen (EISCAT), J Tappin (Ulysses) Supported by: M Kojima (Nagoya), M Pick (Nancay), G Stenborg (MICA), G Bagala (HASTA), S Ananthakrishnan (Ootacamund), A Lecinski (HAO), K Schriver (TRACE), J Raymond (UVCS), I Chashei (Puschino), (Others)(?) Version: (0) June 2000 (draft) (1) July 2000 Background: One of the outstanding problems of space physics is the mechanism (or mechanisms) responsible for heating the solar corona and accelerating the solar wind. It appears likely that the mechanisms involved are different in the fast, low density solar wind above coronal holes (and on open field lines) and the slow, dense and highly variable wind observed above coronal streamers. Co-ordinated measurements of radio scattering (Interplanetary Scintillation) and the drift velocities of features seen in coronagraph images have shown that that fast solar wind has reached at least 400-500 km/s by 4 solar radii (R) and has reached its cruising speed of 750-800 km/s by 10-15 R (Grall et al., 1996; Breen et al., 2000a), while the slow wind has a velocity of 100 km/s or less at 4 R, shows significant acceleration from 6-10 R outwards and only reaches its cruising speed of 300-400 km/s by 25-35 R (Sheeley et al., 1997, Breen et al., 2000b). These results suggest that the energy accelerating the slow wind may be deposited at greater heliocentric distances than is the case in the fast wind. The proposed programme of observations uses IPS observations from EISCAT (931 MHz, 14-100 R) and Toyakawa (327 MHz, 30-250 R), together with high-cadence optical measurements from LASCO C2 and C3, Nancay radioheliograph data, EUV imaging from TRACE, green-line imaging from MICA and white-light images from the MLSO Mk.4 coronagraph and in-situ measuremets from Ulysses as it approaches its southern polar pass. Together these will provide unprecidented coverage of the corona and solar wind from the lower corona to beyond 400 R. As well as giving bulk flow speeds, the IPS measurements from MERLIN and EISCAT will provide upper limits on the Alfven wave flux in the solar wind between 4 and 100 R (Canals et al., 2000). This dataset will be crucial in testing the predictions of wave-heating models of solar wind acceration. The LASCO measurements wil act as an important constraint to the interpretation of the IPS measurement, as they provide an independent measure of bulk flow speed covering an overlapping range of distances. The proposed programme of observations are also ideally suited to studying the propagation and velocity profile of coronal mass ejections from their origin to beyond 400 R. A second objective is to compile a dataset of very high cadence LASCO images. This will complement a previous (Jan '96) high (~3 min) cadence dataset, and allow a comparison of the fastest dynamic coronal features and processes at solar minimum and maximum. Furthermore, the earlier dataset had limited spatial coverage (C3 only, 3.8-15 R). The proposed campaign would extent the range to 2-30 R, by utilising the full C2 and C3 fields of view. We anticipate a C2 image cadence of ~6 mins, and a C3 cadence of ~15 mins. Observing schedule: The IPS sources are most favourable in the Sept 6-16 period, by which time the present EISCAT systems upgrade will be complete. The LASCO high campaign envisaged requires SUMER and EIT to be switched off. To maximise the volume of full-resolution LASCO data we propose a schedule that coincides with the EIT CCD bakeout over the weekend of Sept 8-11 A trial run is proposed for Sept 4-6 in which SOHO-LASCO and EIT would be running synoptic programs. The other instruments would aim for their optimal cadences. Instrument programs: LASCO: high-cadence program of 6 x C2 and 4 x C3 full-FoV, full-res images per hour UVCS: UVCS will support JOP 127 on one to three of the days of September 8-11, 2000. The observing plan will be CME Watch at 4 Ro. The choice of the PAs will be based on 1) a bright streamer, 2) an interplanetary observation relatively close to the Sun, 3) several interplanetary targets with similar position angles. Instrument configuration: Roll: TBD Mirror: 4.0 Ro Occulter: 1.5 mm overocculting OVI slit width: 150 um OVI grating position: 168208 Major lines included in the mask: OVI 1032, OVI 1037, Lyman Alpha 1216, Lyman Beta 1025, Si XII 520, C III 977, N III 991&989, O V] 1218, [O V] 1213, Mg X 609 Mask binning: 3-pixel (21 arcsec) spatial, 2-pixel spectral Exposure cadence: 120 sec UV and VL (no pB) UVCS contact person: John Raymond (jraymond@cfa.harvard.edu) EISCAT: between 9 and 12 sources targeted per day for up to 90 minutes, giving almost continuous coverage from about 04:30 to 14:30, at a variety of position angles relative to the solar central meridian. Ulysses: synoptic programs, monitoring the 2AU solar wind for density, speed and composition signatures Nagoya: between 50 and 60 sources per day, giving coverage during EISCAT night Nancay: full-disk images every 10s at 435, 410, 327, 236, 164 MHz Ootacamund: campaign mode, to be finalised MICA: high-cadence mode of 1 x full-FoV, full-res white light image every ~90s, plus 1x iron-line image for calibration and pointing HASTA: high-cadence patrol mode, with high-speed mode disabled, giving 1 x full-disk H-alpha image per minute HAO: synoptic program, including calibration images TRACE: ~4 iron-line images per hour, to determine MICA pointing and identify onset times (to be arranged from JOP 126 support) UVCS long series of short exposures at either 2 or 4 solar radii at a single position angle dictated by the IPS sources and streamers, plus synoptic observations Puschino: campaign mode, to be finalised Others: TBC/TBD Contacts: Gareth Lawrence (LASCO, Univ. Birmingham) grl@star.sr.bham.ac.uk Andy Breen (EISCAT, Univ. Wales, Aberystwyth) azb@aber.ac.uk James Tappin (Ulysses, Univ. Birmingham) sjt@star.sr.bham.ac.uk Other contact details to be added. Please contact GRL in first instance. Please contact GRL in first instance. Masoyoshi Kojima (Nagoya), kojima@stelab.nagoya-u.ac.jp Monique Pick (Nancay), pick@obspm.fr Guillermo Stenborg (MICA), stenborg@linmpi.mpg.de Gabriela Bagala (HASTA), gbagala@cds.plasma.mpe-garching.mpg.de Subradyam Ananthakrishnan (Ootacamund), ananth@ncra.tifr.res.in Alice Lecinski (HAO), alice@slug.hao.ucar.edu Karel Schriver (TRACE), schryver@lmsal.com John Raymond (UVCS), raymond@cfa.harvard.edu Igor Chashey (Puschino), chashey@prao.psn.ru (Others)(?)