JOP Title: Linking the Corona to the solar wind at Ulysses Targeted Campaign #1, Whole Heliosphere Interval (WHI), first week (20-26 Mar 2008) Authors: G. Poletto (Lead), A. Breen, M. Bisi, R. Fallows, P.K. Manoharan, C. Marque', S. W. McIntosh, S. Plunkett, K. Reeves, A. Sterling, S.T. Suess, M. Tokumaru Other Correspondents: L. Abbo, W. Curdt, M. Kojima, G. Maris, M. P. Miralles, K. Munakata. Update History First Draft (26 Nov 2007) Participating instruments and observatories Targeted Space Based: SOHO/UVCS - campaign contact G. Poletto, Y.-K. Ko SOHO/LASCO - extra pB maps under consideration Hinode/XRT/EIS -- campaign contact A. Sterling Hinode/SOT -- campaign contact S. Mcintosh TRACE -- campaign contact K. Reeves Ground based: EISCAT -- campaign contact A. Breen Ooty -- campaign contact P. K. Manoharan IPS 327MHz station, Nagoya -- campaign contact M. Tokumaru HSO/CoMP -- campaign contact S. McIntosh Synoptic Nancay Radioheliograph -- campaign contact C. Marque', A. Kerdraon SOHO/LASCO-C2/C3 -- S. Plunkett SOHO/EIT -- TBD STEREO/SECCHI/EUVI/COR1/COR2/HI -- campaign contact S. Plunkett Ulysses/SWOOPS/SWICS -- campaign contact S. Suess Global Muon Detector Monitor -- contact person K. Munakata Scientific Objectives Our main scientific objective is to derive the solar wind speed profile from coordinated SOHO/UVCS and radio scintillation data, over a wide range of heliocentric distances (2 to 50 R_sun), with the terminal wind speed being given by in situ Ulysses data. The goal of this study is twofold: on one side, we will provide the solar community with a composite wind speed vs. heliocentric distance profile based on measurements which refer to the same plasma parcels measured by different experiments at different distances - thanks to the SOHO-Sun-Ulysses quadrature configuration. While this is "per se" a valid objective, the wind profile we will come up to will serve as a benchmark input for the construction of a reference solar minimum heliosphere, as described later in this document. A further objective we aim to as a by-product of the campaign observations is to get a better understanding of polar plumes morphology and physical conditions, with special emphasis to their temporal variation, practically unknown so far. The role of plumes in solar wind is still to be ascertained, hence, although we will build a wind profile averaged over the plume/interplume plasma in our main objective, we also plan to contribute to a better understanding of the solar wind by investigating polar plumes. Observations from COMP will provide measurements of alfvenic plasma motions and pos magnetic field diagnostics from the limb to 1.4 solar radii in the 10747 and 10830 lines. These measurements will help characterize the magnetic structures present, their inclination and the multitude of wave motions present - essential to understanding the roots of the fast solar wind. These goals are based on the following IHY Coordinated Investigation Programs (CIPs): 7: SOHO-Ulysses coordinated studies during the two quadratures and the alignment of 2007-2008 43: SMEI and IPS 3D heliospheric analysis comparison with Ulysses... 69: Rapid solar wind and its impact on the geomagnetic variability 11: Three-dimensional view of the inner heliosphere... 5: State of the LISM at the Heliospheric Boundary and Inside Scientific Justification The interpretation of the solar wind speed profile from its very source to large distances has still to cope with a number of open problems such as fully explaining the transition from fast to slow wind, bringing together observations close to the Sun and observations at distances of several to tens of AU, constructing the wind 3D structure over the whole heliosphere. In order to start dealing with these issues, it is crucial to get a data set to be used as a baseline to define a reference heliosphere. To this end, years 2007/2008 - the time interval defined as the International Heliophysical Year - offer an ideal situation, because of the presence of a whole fleet of spacecraft at different heliocentric distances. Also, we point out that during the WHI interval we are in a SOHO-Sun-Ulysses quadrature configuration, i.e., in a geometry that allows plasma parcels observed with remote instrumentation to be observed in due time by "in situ" experiments. Coordinated observations can be made by SOHO/HINODE/ACE/WIND/STEREO/Ulysses while the solar wind speed at the Termination Shock (TS) will be observed by Voyager 2, at present in the pre-shock regions of the TS. These data will be complemented by ENAs (Energetic Neutral Atoms) observations made by IBEX (Interstellar Boundary Explorer, to be launched in 2008) that are directly related to the solar wind which originates in the corona in 2007/2008. The JOP data are acquired in the framework of this project. A test campaign has been made May 7 to 13, 2007, joining SOHO/UVCS and radio scintillation measurements. Operational Considerations The geometry of the Ulysses quadrature dictates where data need to be acquired: east limb, Northern hemisphere, 70 degree latitude. Detailed Observing Sequences per Instrument (will be revised later, based on input from instrument teams): SOHO/UVCS The slit of UVCS will be set normal to the solar radius to Ulysses. Data will be taken in the Ly-alpha line, at a number of altitudes ranging from about 1.7 to about 5 solar radii. Radio scintillation data: Different instrumentation take part in the campaign: - Ooty Radio Telescope operating at 327 MHz: will make solar wind estimates (using the Interplanetary Scintillation (IPS) technique) for the whole campaign period. - STELab 327MHz multi-station IPS system: will start observing on April 1st, so it will not take data during the Targeted Campaign Week. Nevertheless, from April 1st data will be acquired daily from 22h and 7h UT. The distribution of the solar wind speed for radial distance between 0.1 and 1 AU will be derived over a Carrington rotation. Hence, if the target coronal hole is a stationary feature STELab will still provide relevant data. The wind map provided by STELab covers the entire range of heliographic longitude and latitude, and the speed estimate is given with a 1 deg by 1 deg pixel resolution. - EISCAT-MERLIN: unfortunately there are no sources to infer good information with EISCAT-MERLIN baselines during WHI. The situation is somehow analogous to that of STELab, but during the previous Carrington rotation a number of observations will be made at the East limb. More precisely: 20080223 Dist Lat limb sites 1330 1430 2225-049 18.6 63.1 E KT 1330 1430 2232+117 78.6 51.9 E CK 1430 1530 2212+018 44.7 69.9 E JS 20080224 1330 1430 2232+117 77.1 53.6 E CK 1345 1445 2225-049 17.3 72.6 E KT 1430 1530 2212+018 44.4 70.7 E JS Observations can be made later with the 0137+331 source, extending from 50 N at 85Rs on 20080415 through to past the end (or beginning earlier, at lower latitudes) - say to 64N at 79Rs on 20080427, East limb, thus "bordering" data taken during the WHI. SOHO/EIT/LASCO/SUMER: EIT maps support the plume campaign with images of plumes. LASCO pB observations are crucial to the primary focus of the campaign, because they offer a means to estimate coronal densities along the radial to Ulysses, at the positions where UVCS acquires data (contributing to a better interpretation of UVCS outflow speed measurements. SUMER operations are foreseen most likely during the last WHI week. In this case we have no SUMER support during the campaign, but SUMER may be able to support earlier campaigns. The issue is under discussion. STEREO/SECCHI STEREO/SECCHI/EUVI and/or COR1: STEREO SECCHI normal synoptic data are sufficient for our primary focus. Further action is pending, to support the secondary plume issue. TRACE Observing Plan In order to observe plume morphology high cadence Observations at 171 A (30 - 35 s) are needed, with 284, 1600, 1216 in contest. It will be better to observe with a full FOV (512" X 512"), but this can be discussed later on. Pointing will be chosen to match UVCS observations. TRACE will go into eclipse season starting April 10; this does not affect the campaign, if, as planned, will be run early during the WHI. Hinode/XRT Observing Plan Filters: Al/poly, Ti/Poly filters appear adequate to image soft X-ray plume plasma. Occasionally thin/Be images may be taken to check on the presence of hotter material, possibly with longer exposures (~50 s). EIS contribution TBD. Hinode/SOT Observing Plan SP: detailed vector spectropolarimetry of the polar region - 400"X100" spectropolarimetric maps of polar region in Fe I 6301/6302 NFI: two sequences to characterize the photospheric magnetic field and lower chromospheric expansion. - Fe I 6302.5 Ang. photospheric magnetograms at 10-20s cadence - Na I 5890.6 Ang. chromospheric magnetograms at 10-20s cadence Ground based instrumentation NSO Observing Plan: If the Targeted campaign # 1 will be held in the first week of the WHI, we plan to use the usual SOLIS synoptic maps. Should the campaign be postponed we may search for a more active NSO participation. Nancay Radioheliograph Daily observations from 8:30 to 15:30 UT; five frequencies between 150 and 450 MHz; spatial resolution ~ 1 arcmin; FOV: full Sun. Global Muon Detector Monitor Observations of high-energy cosmic rays with the Global Muon Detector Network. HSO/Coronal Multi-channel Polarimeter [CoMP] - CoMP spectroscopically observes a full-disk FOV out to 1.4 Rsun. Fe XII 10747 - 10s cadence full corona - wave studies He I 10830 - 10s cadence full corona - wave studies - detail of near-limb alfvenic motions. Deep exposure spectropolarimetric POS magnetic field strength, azimuth and line width measurements.