*********************************************************************************** STUDY TITLE: SOLAR MICROFLARES AND NETWORK DYNAMICS - RELEVANCE FOR CORONAL HEATING STUDY TEAM : J. Rybak (choc@astro.sk), P. Gomory, A. Veronig, M. Temmer, S. Stoiser based on "text template for submission of proposed studies for solar-b/eis" (version: MSSL, 2006 Feb 08) *********************************************************************************** Science Case: This proposal merges together attempts to observe two kinds of solar structures - solar microflares and supergranular network - which are planned to be investigated to address common open questions on their relevance for the heating and dynamics of the solar corona. Due to their small sizes and fast dynamics microflares need analysis demanding high spatial resolution observations combined with good temporal cadence. Our objective is to analyse the dynamics and plasma evolution during microflares by studying the chromospheric response to electron beam and/or conductive heating together with the transition region and coronal response combined with X-ray spectral analysis. The comparison of these observational data with theoretical predictions in the frame of electron-beam-driven and conductively driven chromospheric evaporation for individual microflares can help us to better understand: a) whether non-thermal electrons are present in microflares which hints at magnetic reconnection as the underlying physical process, b) how much plasma is brought into the corona by microflares, c) which process dominates the mass transport, d) how much energy which is available for the heating of the corona is deposited during microflares. Supergranular network is clearly related to the heating of the corona as well. On the other hand its close relation to the underlying layers is obvious today. Photospheric and chromospheric layers are planned to be investigated to identify the most probable physical mechanisms responsible for the energy transfer and dynamics of the solar corona above the chromospheric network. Our previous results indicate presence of downward propagating waves in/above the chromospheric network. These results led to the assumption that reconnection of the magnetic field lines should be the dominant mechanism to heat the solar corona above the particular chromospheric network. In contrast, findings of other authors show evidence of propagating intensity oscillations spreading out from the photosphere to the corona and therefore prefer alternative heating mechanism of the corona. To clarify these findings new measurements are necessary for better identification of the heating mechanism. We expect that time series of the speckle-reconstructed DOT filtergrams taken simultaneously with the Hinode/EIS spectra and the supporting Hinode/SOT and XRT data will provide an excellent material to study the properties of the mentioned targets. More details: campaign web page: http://www.astro.sk/~choc/open/07_dot/07_dot.html ******************************************************************************* Predicted count rates: Active region/Quiet sun - 10s. Note: we expect higher count rates than counts obtained for the quiet sun listed below when observing the network emission. Wavelength c/p Ion Total counts for exposure (per pixel) active region / quiet sun 192.82* c Ca XVII 572 / 0 195.12* c Fe XII 4240 / 138 256.32* c He II 247 / 47 185.21 p Fe VIII 275.35 p Si VII 117 / 12 184.54 p Fe X 235 / 13 196.54 p Fe XIII 336 / 4 284.16 p Fe XV 1266 / 6 192.04 p Fe XXIV 138 / 202.04 p Fe XIII 730 / 17 203.83 p Fe XIII 458 / 8 ******************************************************************************* STUDY-SPECIFIC INFORMATION: ******************************************************************************* A. Study Title (max. 100 characters): Solar microflares and network dynamics - relevance for coronal heating B. Study Description/Acronym (max. 20 characters, no spaces): Microflares+network C. Ordering of rasters (by acronym) in the study (with no. of repeats) : 1. Context_calib_jr ( 3 times) - 3x8m31s (25.m in total) 2. Obs_sit_stare_jr (12 times) - 12x28m3s (5.61h in total) slit placed to the X-center of the previous raster 3. Context_calib_jr ( 3 times) - 3x8m31s (25.m in total) raster positioned around the previous slit position Total time: 8h28m:38s (Data volume: 1110892kb, data rate: 47.6622kbps ******************************************************************************* A study is comprised of one or more rasters (each raster can be either "scanning" or "sit'n'stare") Copy and replicate the following raster-specific information template as necessary for the number of rasters in your proposed study. ******************************************************************************* RASTER-SPECIFIC INFORMATION ******************************************************************************* 1. Raster Description/Acronym: Context_calib_jr ------------------------------------------------------------------------------ 2. Line list (please append desired lines to the following list if necessary): Wavelength Type Window Name Width (angstroms) (pixels) 192.82* c Ca XVII 32 log T=6.7 572 195.12* c Fe XII 48 log T=6.1 4240 256.32* c He II 48 log T=4.9 247 185.21 p Fe VIII 24 log T=5.6 275.35 p Si VII 32 log T=5.8 117 184.54 p Fe X 32 log T=6.0 235 196.54 p Fe XIII 32 log T=6.2 336 284.16 p Fe XV 32 log T=6.3 1266 192.04 p Fe XXIV 32 log T=7.2 138 202.04 p Fe XIII 32 log T=6.2 730 203.83 p Fe XIII 32 log T=6.2 458 (*The first three lines are core ("c") lines for each raster and must be included. There is some question, however, about the viability of Ca XVII 192.82. Whether its inclusion is to be compulsory in all studies is yet to be decided. Add any additional desired lines to the following list. The list of programme ("p") lines, expected to be seen by EIS, is online at: http://www.mssl.ucl.ac.uk/www_solar/solarB/faq_lines.html Note that window widths must be a mutiple of 8, but can be different for each desired window. A guideline window width of 32 pixels is suggested as this is equivalent to +/- 400 kilometres per second, in velocity space, at 270 angstroms, or +/- 560 kilometres per second at 190 angstroms.) ------------------------------------------------------------------------------ 3. Slit/Slot Width (in arcseconds): 2" (choose one of 1", 2", 40", or 250") ------------------------------------------------------------------------------ 4. Window height in pixels: 304 (Note that this is the height for all windows. It must be a multiple of 8, up to a maximum of 512 pixels.) ------------------------------------------------------------------------------ 5. Raster Type: Scanning (choose "Scanning" or "Sit'n'Stare") (This determines which of the following group of parameters you must choose -- answer either 5.1 and 5.2 for a scanning raster, or 5.3 or 5.4 for sit'n'stare) --------------------- For a scanning raster: --------------------- 5.1 Number of fine mirror steps (i.e. positions): 41 5.2 Fine mirror step size (in arcseconds): 2 ------------------------------------------------------------------------------ 6. Compensation for Differential Solar Rotation: No (choose either Yes or No) ------------------------------------------------------------------------------ 7. Exposure Options ---------------------- For set exposure times: (answer questions 7.1 to 7.6) ---------------------- 7.1 Number of exposures per step: 1 (Minimum=1, maximum=8. Note that for each position, or "step", several different exposure times can be set, so that -- for example -- a 1-second exposure might be followed by a 10-second exposure before moving the fine mirror to another position on the Sun. This parameter can be used with both sit'n'stare and scanning rasters.) 7.2 Exposure time(s) (in seconds, separated by commas): 10 7.3 Corresponding delay after each exposure (in milliseconds): 0 (This delay term may be useful for slowing down the rate at which data are taken, i.e. specifying a cadence other than the fastest which EIS can attain for this raster). 7.4 Duration of raster (in seconds): 511 7.5 Anticipated data volume, if known (in kilobits, not kilobytes): 22409 kb 7.6 Anticipated mean data rate, if known (in kilobits per second): 47.7606 kbps (note that a time-averaged rate of 45 kilobits per second, averaged over the duration of the study, is the guideline upper limit for uncompressed studies.) ---------------------------------------------- For when Automatic Exposure Control is enabled: (answer question 7.7) ---------------------------------------------- (Note: 1 - that prediction of data rates is unlikely to be easy with AEC enabled; 2 - AEC is not envisioned for use with the 1" or 2" slits.) 7.7 Length of time run-time for AEC-controlled exposures: _________ (This will override the duration specified in Section 5.4, above) ------------------------------------------------------------------------------ 8. No. of repeats of this raster: 3 (i.e. number of times to execute before the next raster) ------------------------------------------------------------------------------ 9. Compression 9.1 Compression type: DPCM (choose one of "DPCM", "JPEG1", "JPEG2" or "None") ------------------------------------------------------------------------------ 9.2 Desired Compression factor: ~2.5 (leave blank if the answer to 9.1 is "None") (Note: choosing "50%" would mean a reduction in telemetry size of a factor of 2. Current testing indicates that a compression factor of 2 with JPEG(?) compression still accurately reproduces line widths and heights, with only slightly reduced precision.) ------------------------------------------------------------------------------ 10. Event triggers 10.1 This study can be interrupted by: a) a) No triggering (study is run as scheduled) b) EIS Event Trigger c) EIS Internal Flare Trigger d) XRT Flare Trigger Please choose: (a) (Note: 1 - A trigger is most likely to be desired if you are hunting for a flare or bright event with EIS, and you have a raster type which you would like to take over in the event of this trigger occurring. 2 - If a trigger is able to interrupt this study, the corresponding raster, the study from which that raster comes, and the length of time for this raster to run after the trigger occurs, must all be supplied. This study can be either from the official database, or submitted by e-mail just like other studies.) ---------------------- For EIS Event Trigger: ---------------------- 10.2 Window to be monitored: ________ (Note: the window MUST be from the line list entered in Section 2.) 10.3 Description/Acronym of study to be run in response: ____________________ 10.4 ID Number or Description/Acronym of raster (from response study) to be run: ____________________ (Note: you must only choose one raster to be run from this study, although it repeated exactly as it would be run in that study.) 10.5 Repoint in X (Yes or No): _______ 10.6 Repoint in Y (Yes or No): _______ 10.7 X Threshold: __________ 10.8 Y Threshold: __________ 10.9 X Min. Limit: __________ 10.10 Y Min. Limit: __________ ------------------------------- For EIS Internal Flare Trigger: ------------------------------- 10.11 Window to be monitored: ________ (Note: the window MUST be from the line list entered in Section 2.) 10.12 Description/Acronym of study to be run in response to EIS Flare Trigger: ____________________ 10.13 Description/Acronym of raster (from response study) to be run: ____________________ 10.14 Repoint in X to: __________ (choose either "Flare Peak X" or "Flare Centre X") 10.14 Repoint in Y to: __________ (choose either "Flare Peak Y" or "Flare Centre Y") ---------------------- For XRT Flare Trigger: ---------------------- 10.15 Description/Acronym of study to be run in response to XRT Flare Trigger: ____________________ 10.16 Check that XRT is in EIS Field of View? (Yes or No): ____ 10.17 Description/Acronym of "filler study", to be run between end of response study and end of XRT Flare Trigger mode: __________________ ******************************************************************************* ******************************************************************************* ******************************************************************************* RASTER-SPECIFIC INFORMATION ******************************************************************************* 1. Raster Description/Acronym: Obs_sit_stare_jr ------------------------------------------------------------------------------ 2. Line list (please append desired lines to the following list if necessary): Wavelength Type Window Name Width (angstroms) (pixels) 192.82* c Ca XVII 32 log T=6.7 195.12* c Fe XII 48 log T=6.1 256.32* c He II 48 log T=4.9 185.21 p Fe VIII 24 log T=5.6 275.35 p Si VII 32 log T=5.8 184.54 p Fe X 32 log T=6.0 196.54 p Fe XIII 32 log T=6.2 284.16 p Fe XV 32 log T=6.3 192.04 p Fe XXIV 32 log T=7.2 202.04 p Fe XIII 32 log T=6.2 203.83 p Fe XIII 32 log T=6.2 (*The first three lines are core ("c") lines for each raster and must be included. There is some question, however, about the viability of Ca XVII 192.82. Whether its inclusion is to be compulsory in all studies is yet to be decided. Add any additional desired lines to the following list. The list of programme ("p") lines, expected to be seen by EIS, is online at: http://www.mssl.ucl.ac.uk/www_solar/solarB/faq_lines.html Note that window widths must be a mutiple of 8, but can be different for each desired window. A guideline window width of 32 pixels is suggested as this is equivalent to +/- 400 kilometres per second, in velocity space, at 270 angstroms, or +/- 560 kilometres per second at 190 angstroms.) ------------------------------------------------------------------------------ 3. Slit/Slot Width (in arcseconds): 2" (choose one of 1", 2", 40", or 250") ------------------------------------------------------------------------------ 4. Window height in pixels: 304 (Note that this is the height for all windows. It must be a multiple of 8, up to a maximum of 512 pixels.) ------------------------------------------------------------------------------ 5. Raster Type: Sit'n'Stare (choose "Scanning" or "Sit'n'Stare") (This determines which of the following group of parameters you must choose -- answer either 5.1 and 5.2 for a scanning raster, or 5.3 or 5.4 for sit'n'stare) ------------------------ For a sit'n'stare raster: ------------------------ 5.3 No. of Exposures (if known): 135_________ OR 5.4 Duration of sit'n'stare (in seconds): 1683_____ (Note: Entering either parameter will automatically allow the planner to calculate the other.) ------------------------------------------------------------------------------ 6. Compensation for Differential Solar Rotation: No (choose either Yes or No) ------------------------------------------------------------------------------ 7. Exposure Options ---------------------- For set exposure times: (answer questions 7.1 to 7.6) ---------------------- 7.1 Number of exposures per step: 1 (Minimum=1, maximum=8. Note that for each position, or "step", several different exposure times can be set, so that -- for example -- a 1-second exposure might be followed by a 10-second exposure before moving the fine mirror to another position on the Sun. This parameter can be used with both sit'n'stare and scanning rasters.) 7.2 Exposure time(s) (in seconds, separated by commas): 10 7.3 Corresponding delay after each exposure (in milliseconds): 0 (This delay term may be useful for slowing down the rate at which data are taken, i.e. specifying a cadence other than the fastest which EIS can attain for this raster). 7.4 Duration of raster (in seconds): 1683 7.5 Anticipated data volume, if known (in kilobits, not kilobytes): 80370 kb 7.6 Anticipated mean data rate, if known (in kilobits per second): 47.7606 kbps (note that a time-averaged rate of 45 kilobits per second, averaged over the duration of the study, is the guideline upper limit for uncompressed studies.) ---------------------------------------------- For when Automatic Exposure Control is enabled: (answer question 7.7) ---------------------------------------------- (Note: 1 - that prediction of data rates is unlikely to be easy with AEC enabled; 2 - AEC is not envisioned for use with the 1" or 2" slits.) 7.7 Length of time run-time for AEC-controlled exposures: _________ (This will override the duration specified in Section 5.4, above) ------------------------------------------------------------------------------ 8. No. of repeats of this raster: 12 (i.e. number of times to execute before the next raster) ------------------------------------------------------------------------------ 9. Compression 9.1 Compression type: DPCM (choose one of "DPCM", "JPEG1", "JPEG2" or "None") ------------------------------------------------------------------------------ 9.2 Desired Compression factor: ~2.5 (leave blank if the answer to 9.1 is "None") (Note: choosing "50%" would mean a reduction in telemetry size of a factor of 2. Current testing indicates that a compression factor of 2 with JPEG(?) compression still accurately reproduces line widths and heights, with only slightly reduced precision.) ------------------------------------------------------------------------------ 10. Event triggers 10.1 This study can be interrupted by: a) a) No triggering (study is run as scheduled) b) EIS Event Trigger c) EIS Internal Flare Trigger d) XRT Flare Trigger Please choose: (a) (Note: 1 - A trigger is most likely to be desired if you are hunting for a flare or bright event with EIS, and you have a raster type which you would like to take over in the event of this trigger occurring. 2 - If a trigger is able to interrupt this study, the corresponding raster, the study from which that raster comes, and the length of time for this raster to run after the trigger occurs, must all be supplied. This study can be either from the official database, or submitted by e-mail just like other studies.) ---------------------- For EIS Event Trigger: ---------------------- 10.2 Window to be monitored: ________ (Note: the window MUST be from the line list entered in Section 2.) 10.3 Description/Acronym of study to be run in response: ____________________ 10.4 ID Number or Description/Acronym of raster (from response study) to be run: ____________________ (Note: you must only choose one raster to be run from this study, although it repeated exactly as it would be run in that study.) 10.5 Repoint in X (Yes or No): _______ 10.6 Repoint in Y (Yes or No): _______ 10.7 X Threshold: __________ 10.8 Y Threshold: __________ 10.9 X Min. Limit: __________ 10.10 Y Min. Limit: __________ ------------------------------- For EIS Internal Flare Trigger: ------------------------------- 10.11 Window to be monitored: ________ (Note: the window MUST be from the line list entered in Section 2.) 10.12 Description/Acronym of study to be run in response to EIS Flare Trigger: ____________________ 10.13 Description/Acronym of raster (from response study) to be run: ____________________ 10.14 Repoint in X to: __________ (choose either "Flare Peak X" or "Flare Centre X") 10.14 Repoint in Y to: __________ (choose either "Flare Peak Y" or "Flare Centre Y") ---------------------- For XRT Flare Trigger: ---------------------- 10.15 Description/Acronym of study to be run in response to XRT Flare Trigger: ____________________ 10.16 Check that XRT is in EIS Field of View? (Yes or No): ____ 10.17 Description/Acronym of "filler study", to be run between end of response study and end of XRT Flare Trigger mode: __________________ ******************************************************************************** *******************************************************************************