JOP194 Activity in Filaments and Filament Cavities Authors S Gibson, H. Gilbert, P.S McIntosh, B.J. Thompson, D. Berghmans, D. Biesecker, J. Burkepile, G de Toma, R. Harrison, R. Liu, G. Kilper, T. Kucera, A. Sterling, E.Robbrecht, D. Webb, A. Zhukov Update History Version 1.0 (27 June 2007) Participating instruments and observatories Targetted: Space Based SOHO/CDS, EIT, and possibly, in future campaigns, SUMER -- campaign contact T. Kucera SOHO/UVCS - campaign contact J. Raymond, K. Ko Hinode/EIS -- campaign contact A. Sterling, D. Williams Hinode/XRT -- campaign contact K. Reeves Hinode/SOT -- campaign contact S. Mcintosh TRACE -- campaign contact K. Reeves Ground based Comfirmed for Aug. 2007 Campaign: COMP -- campaign contact S. Tomczyk HELIO -- S. Martin Possible for Aug. 2007 or future campaigns: SOLARC -- campaign contact H. Lin ProMag -- campaign contact R. Casini MWA -- campaign contact J. Kasper Synoptic Mode: SOHO/LASCO-C2/C3 STEREO/SECCHI/EUVI/COR1/COR2/HI (may also run special high cadence observations) STEREO/IMPACT STEREO/PLASTIC PROBA2/SWAP GOES/SXI H-alpha (BBSO, ISOON, MLSO...) Nancay radioheliograph SMEI RHESSI Scientific Objectives We will study filaments, filament channels, and filament cavities with the following goals: To understand the time dependent, three dimensional density, temperature, and magnetic structure of filaments and filament channels and cavities; To study how filaments form; To study filament activation in the chromosphere and CMEs in the corona to better understand how this process works and how it is related to CMEs. Note that for the first campaign (August 8-18) we plan to target filaments associated with well-established, longitudinally extended filament channel (e.g. a Polar Crown Filament (PCF)). This will improve the chances of good cavity observations, and allow us to concentrate on a large-scale, long-lived structure. If the observed structures erupt we will Study the evolution of the cavity during eruption Map the EUV signatures (dimmings, filaments, expanding loops, EIT waves) into the coronal structures as represented by the coronagraphs, with the goal of understanding more clearly the structure and manifestations of CMEs in the low corona. These goals are based on the following IHY Coordinated Investigation Programs (CIPs): Scientific Justification The new observations from STEREO and Hinode combined with existing resources of SOHO, TRACE, ground based observatories, and modeling efforts should provide new understanding of the structure and dynamics of filaments, filaments cavities, and eruptive events. In this campaign we are pulling together this wide range of resources to understand the filament and its environment in three dimensions and a wide range of temperatures. The observations are flexible enough that we can obtain useful information about an eruptive or non-eruptive filament, whichever occurs. Operational Considerations The chief ground based support is from Hawaii, so our prime observing time is the Mauna Loa prime viewing time 18:00-22:00 UT, although observations may be taken 16:30 - 02:30 UT. Most day we will request observing during the 18:00-22:00 UT time period. There are up to 3 variants on of the observing programs - Observing programs for filaments on the disk - Observing programs of targets on the limb - Long exposure programs for streamers. These are only different from other limb observations for EIS and CDS. The last ones would be either added (as possible) on a few days when a very good cavity target was present, either before the regular observations or replacing them if it was thought very unlikely the would be an eruption. The choice of programs will be announced by the campaign coordinator, and any extra observing time will be worked out with the EIS and CDS planners. Target will be selected a designated campaign target selector each day. A team member in Japan will have final ability to change the target. We hope to be able to follow a target for a number of days in a row. The target pointing will be based on the Hinode pointing. See this web page for more information: http://web.hao.ucar.edu/~sgibson/CIP21/topcampaign.html We request EIT shutterless observations when possible, which will require real time operations. Detailed Observing Sequences per Instrument SOHO/EIT: When possible (we estimate 1 or 2 times during the course of the campaign) we would like to run in EIT shutterless mode at 304 A (10'x10' field of view). At other times we would like high cadence EIT sub fields in 304 or 195 A, 8'x8' field of view SOHO/CDS Cavity Observations on the Limb: EJECT_V3/v18 (16 min rasters in He I, O V, Mg IX, Fe XVI, Si X) For limb targets run in three 4x4 arcmin mosaic forming a 4x12 arcmin field on west or east limb (see regular CDS "CME onset watch" program). On certain days we will request special longer exposure observations of the streamer cavity on the limb using STRE4W/v111 in a mosaic to cover the cavity and adjacent streamer. This should be coordinated with EIS GAD002_AR_RAST and/or QS_ATLAS_OFFLIMB observations of the same region. See the EIS listing for more discussion of scheduling. Filaments on Disk: Run EJECT_V3/v18 On disk mosaic if necessary to cover region of interest. The overall mosaics should have same pointing as the EIS study. SOHO/UVCS When the target is within 30 degrees of the limb, UVCS will observe at 1.7 Rsun, obtaining line intensities and profiles for Ly beta, Ly gamma, C III 977, O VI 1032, O VI 1037 and Si XII 520 with a 124 second cadence. SMEI SMEI will try to reserve the time period of campaign observations (1700-2000 UT minimum, 1650-0230 UT maximum) as "no=cal" during the campaign. Because of shuttering and background sources, views of either the solar east or west limb may be more favorable from SMEI for this campaign. SMEI may also coordinate campaign observations with STEREO/SECCHI instruments. STEREO/SECCHI STEREO/SECCHI/EUVI and/or COR1 hope to run in high time cadence mode during the time periods 1800-2200 UT. Otherwise they will take normal synoptic data. Hinode/EIS EIS will run different studies, depending on whether we are observing cavities or filaments. Cavities: Our main plan for observations if we have a good filament cavity at the limb is to choose from among these three basic programs: 1) A combination of the 2" slit study CMEO_SLIT_STUDY and the slot (40" wide slit) study CMEO_SLOT_STUDY. These studies are designed to observe CME eruptions and related phenomena. 2) A 4.5 hour raster which includes several different cool (TR) lines; this study is GAD002_AR_RAST, and would allow us to make deep spectrograms over a fairly large (about 300'') FOV. We hope to be able to determine physical properties of the cavity material, or at least of its bright boundary if we cannot detect the cavity material itself. 3) A spatially-sampling raster, using a 1" slit but with 10" steps. This would take about 45 min to complete and include full spectral information. This study is called QS_ATLAS_OFFLIMB. We would favor running (1) during the observing Focus Time Period in the hope of observing an eruption, since MLSO and SECCHI/COR1/EUVI (also involved in the campaign; see below), might be running high time-resolution observations. We would perhaps choose to run the longer rasters (3, and especially 2) during the observing Focus Time Period if our best guess says that an eruption is not eminent (e.g., due to lack of rise of the cavity over the previous days - Gibson et al. 2006; S. Martin 2006, private comm.), or we would request that the Hinode team consider running the longer rasters prior to the start of the campaign prime time if there is no conflicting observational target. The longer raster (2 and 3) would be run in conjunction with SOHO/CDS companion program Filaments: When a good cavity at the limb is not visible, then we will look at filaments or filament channels on the disk. We would run a selection of the previously-developed filament studies for these observations. Hinode/SOT On disk: SP: 1) Prior and after Observing Period Perform 1"x100"Xlength of channel spectropolarimetric maps in Fe I 6301/6302 2) During Observing Period perorm 1"X100"x100" repeated rastering of SP. BFI: Alternating at 10s cadence Ca II H (3968.5 Ang) full field (200"x100") of channel region CN I (3883.0 Ang) full field (200"x100") of channel region NFI: Choice of one - maybe we'll be able to tune by then and get both 10s Fe I 6302.5 Ang. magnetograms at 5s cadence (200"x100") H I 6562.8 Ang. line core at 5s cadence (200"x100") Off disk: BFI: Ca II H (3968.5 Ang) full field (200"x100") of prominence region, 5s cadence NFI: H I 6562.8 Ang. line core at 5s cadence (200"x100") Hinode/XRT Main Loop: Filters: Al/poly (8-16 sec exposure), Ti/Poly (16-23 sec exposure) Cadence: ~1.5 min for whole loop FOV: 768"x384" In the case of an active region on the sun, the long exposures can be replaced by multiple short exposures. Context: Al/poly (2048x2048, 2x2 binned), 5 thin Be (768"x384" 23 sec) every ~30 minutes TRACE Main wavelength: 171 Cadence: ~ 1min (could be longer if the target region is very quiet) FOV: 1024x1024 pixels (512"x152") Context : 1550/1600/1700/WL every ~ 20 min MLSO MLSO hopes to run high temporal cadence during campaign hours, 1800-2200 UT.