Hi David, that sounds fine. I enclose two more squences, one which was missed from the previous list and a new one. Gerry. ======================================================== Relation between reconnection events and waves J.G. Doyle, E. O'Shea & D. Banerjee, ========================================================== We wish to study the relation between reconnection events and waves, enquiring whether it is possible that reconnection events are triggering the waves. We want to look in the highest resolution images for new loop structures inside a BP that could be associated to reconnection events and compare them to newly appeared oscillating wave-trains. High resolution magnetograms should be available to provide information about the magnetic flux changes. Propose to use EIT, XRT & the magnetogram. ********** EIS Study ********** Line list:ARM_2 LINE WAVELENGTH TEMP. He II 256.32 log T=4.7 Si VII 275.35 log T=5.8 Fe XII 195.13 log T=6.1 Fe XV 284.16 log T=6.3 CaXVII 192.82 log T=6.7 Observations: Slot observations: We propose to use the 40" slot to produce a movie images of the BP in a selected group of strong lines (ARM_2). A 60 pixel long slit window will be used to produce images of 40"x120" in size. Use an exposure time of 30s and repeat the observations 100 times to build up a movie of the developing bright point region. This will allow us to visually see the changes in the loop structures within the BP as they occur. It is expected that the observations will take >3000s. The slit is not to move from the BP during the observation through use of the solar tracking facility. During the observations, if the BP shows a sudden brightening it is proposed to use the event trigger to initiate a sequence of time series rasters using the 2" slit and the line list ARM_1. The sequence time series rasters below will then be run. Target: coronal hole / Bright point (BP) Line list: ARM_2 Exposure duration: 30s Slit/slot size: 40" Fine mirror step: 1" No. of xsteps: 0 Common window height (pixel): 60 Window width: 30(may need to be changed for these slot observations) No. of spectral windows: 5 No. of rasters: 100 Total duration: >3000s Solar feature tracking: On Time series raster: Use the 1" slit again with a 120 pixel long slit window targeted on the bright region in the coronal hole. Use the solar feature tracking to maintain the slit on the bright spot as the Sun rotates. Obtain 100 repeat rasters of the bright point, leading to a total duration of the sequence of >3000s (no incl. readout time etc.) Again use window widths of 30 pixels (may need to be amended depending on wavelength coverage required). Exposure duration of 30s. Target: coronal hole / Bright point (BP) Line list: ARM_1 Exposure duration: 30s Slit/slot size: 1" Fine mirror step: 1" No. of xsteps: 0 Common window height (pixel): 120 Window width: 30 No. of spectral windows: 19 No. of rasters: 100 Total duration: >3000s Solar feature tracking: On If no sudden brightening is observed (necessitating the use of the event trigger) the time series raster will be run immediately following those of the slot observations. For high resolution images of the BP it is considered to use overview rasters built up by moving the 2" slit in 60 steps in X. The sequence below will be run; Overview raster: Use 2" slit to raster 60 positions with the 120 pixel long slit window (producing a raster of 120"x240" assuming resolution of 2" per pixel in the y direction). Use a window with of 30 pixels for the 19 lines (and hence separate windows) chosen. The fine mirror step should be every 2 arcsec. Total no. of rasters is 1. Exposure duration of 30s Target: coronal hole / Bright point (BP) Line list: ARM_1 Exposure duration: 30s Slit/slot size: 2" Fine mirror step: 2" No. of xsteps: 60 Common window height (pixel): 120 Window width: 30 No. of spectral windows: 19 No. of rasters: 1 Total duration: >1800s Solar feature tracking: Off Further context images of the BP can be obtained by using the XRT telescope, with a study like the following; *********** XRT study *********** XRT mode: Quiet Use the XRT telescope to provide context images within its temperature range. Attempt to obtain time series of the bright points using a partial FOV and an exposure time of a few seconds (taking into account that we are observing a coronal hole). ********************** FFP magnetogram study ********************** While the 40" slot movie and the time series rasters are being obtained it is proposed that parallel observation with the FPP magnetogram are undertaken every 5 mins. In this way changes in the magnetic structure in the BP can be related to sudden brightenings and restructuring in the BP. Diagnostics of loop-like coronal structures Y. Taroyan & J.G.Doyle =========================================== We propose to use spectroscopic EIS time-series measurements with co-aligned XRT observations near the equatorial regions of the Sun to study coronal (active region) loop-like structures. The spectroscopic observations should be done in transition region and coronal lines. These are high cadence feature tracking-mode observations which should last for at least several hours. Our theoretical and numerical studies have predicted the presence of distinct mHz peaks in the power spectra of the line intensity and Doppler shift time-series. These peaks will allow us to better understand the multistrand structure of the loops, determine important physical parameters such as the average temperatures of these structures, the average energies involved in the small-scale heating processes and their distributions in time and space. ****************** EIS observations: ****************** Overview Raster: Use 2" slit to raster 60 positions with the 120 pixel long slit window (producing a raster of 120"x240" assuming resolution of 2" per pixel in the y direction). Use a window with of 30 pixels for the 19 lines (and hence separate windows) chosen. The fine mirror step should be every 2 arcsec. Total no. of rasters is 2, one before and one after the time series. Exposure duration of 30s Target: coronal hole / Bright point (BP) Line list: ARM_1 Exposure duration: 30s Slit/slot size: 2" Fine mirror step: 2" No. of xsteps: 60 Common window height (pixel): 120 Window width: 30 No. of spectral windows: 19 No. of rasters: 1 Total duration: >1800s Solar feature tracking: Off Time series rasters: Use the 2" slit of EIS with a 120 pixel long slit window targeted on a loop within an active region. Use the solar feature tracking to maintain the slit on the same location on the loop the Sun rotates. Take 3-4 time series rasters. In each observation obtain 200 repeat rasters of the loop, leading to a total duration of the sequence of >3000 x 4 s. Exposure duration of 15s. Use the line list ARM_1 with 19 separate wavelength windows of 30 pixels (may need to be amended depending on wavelength coverage required). Target: Active region disk centre, followed over subsequent days to the limb Line list: ARM_1 Exposure duration: 15s Slit/slot size: 2" Fine mirror step: 1" No. of xsteps: 0 Common window height (pixel): 120 Window width: 30 No. of spectral windows: 19 No. of rasters: 200 Total duration: >3000 x 4 s Solar feature tracking: On ********** XRT study *********** XRT mode: Active Use the XRT telescope to provide context images within its temperature range. Obtain time series of the loop using a partial FOV and an exposure time of a few seconds.