Title: Connection between photospheric vortex flows and transition region and coronal heating Authors: D.E. Innes, R. Attie, L. Gizon Instruments and POCs SOHO/SUMER: D.E. Innes SOHO/MDI: TBD HINODE/SOT: T. Berger HINODE/EIS: H. Hara HINODE/XRT: M. Weber TRACE: TBD STEREO: TBD Scientific Objectives: The aim of this proposal is to accumulate a data-bank of information on X-ray brightenings and their relationship to photospheric fields, so that we can make predictions on when and where eruptions will occur. This requires observations over several hours across different features (coronal holes, quiet Sun, small active regions) on the solar disk. Analysis of MDI and EUVI/STEREO data suggests that eruption and coronal brightenings are activated by twisting photospheric flows at supergranule junctions (Innes et al, A&A, 2008). We have several examples where vortices in photospheric flows, computed by tracking granules in MDI continuum images, seem to be dragging mixed polarity magnetic fields together. Subsequently small CME-like eruptions are seen from the same supergranule junction in EUVI images. With SOT/FG continuum images we are able to track the photospheric flows with much better resolution and, together with XRT, we are able to see smaller events in detail. The rate for small (5” and 15 min) X-ray events is 1-2 events per hour in the SOT field-of-view for the quiet Sun. To see the build-up phase of events we require at least 8 hours of observation, the turnover time of supergranulation. Operational Considerations: Both the Soho instruments SUMER and MDI (HR) are essential. SUMER because it provides high quality spectra showing the transition region dynamics, at least along the 300”x1” slit. MDI because it provides the line-of-sight magnetic field and Doppler velocity as well as continuum images for computing the photospheric flow across the full XRT field of view. In addition MDI images will be used to obtain sub-surface flows using local helioseismology techniques. We are asking for HR MDI and SUMER observations, to be taken together with FG/SOT , C-Poly/XRT and EIS for three 8 hour observations during the SUMER campaign in April. If possible there should be one run on each of the three features - quiet Sun, coronal hole and active region. As mentioned above EUVI/STEREO 171 images show small CME-like eruptions in the quiet Sun. The advantage of EUV over X-ray images is that one sees in addition to the coronal brightenings, the cold filament eruptions as darkenings against the bright background corona. Studies have so far only been done with an angles less than 20 degrees to the earth-sun line. In April the angle between the STEREO spacecraft and earth will be about 45 degrees. We would like to ask for high cadence 171 images to see events from this different perspective. Proposed Dates: 2009 Apr 14 -- Apr 30. Detailed Observing sequences: SOHO/SUMER - map connection to chromosphere, pick up transition region flows. Rasters in Si IV and continuum SOHO/MDI - High Res Hinode/SOT: Ca II, Blue continuum, magnetic field Hinode/EIS: slot He II, Si VII, X, Fe XII, XIV, XV Hinode/XRT: Hig cadence C-poly TRACE: 171 images with 1700 for co-alignment STEREO: High cadence 171 images