*********************************************************************************** STUDY TITLE: Physical mechanisms driving solar microflares and network dynamic fibrils - relevance for coronal heating and mass supply STUDY TEAM : J. Rybak (choc@astro.sk), P. Gomory, A. Veronig, M. Temmer, S. Stoiser. J. Koza, A. Kucera based on "text template for submission of proposed studies for solar-b/eis" (version: MSSL, 2006 Feb 08 + study submission requirements & Study Description Template) *********************************************************************************** Science Case: This proposal merges together attempts to observe two kinds of solar structures - solar microflares and network dynamic fibrils - 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 answer several open questions regarding microflares and the coronal heating. Network dynamic fibrils (DFs) display in the chromosphere repetitive mass loading by acoustic shocks driven by the global oscillations in the underlying photosphere. This scenario assumes that considerable power of photospheric 5-min oscillations is concentrated at the bases of inclined magnetic fluxtubes giving rise to the chromospheric DFs. Using H alpha filtergrams obtained by the Dutch Open Telescope we have shown that the DFs exhibit also significant variations in orientation, which are faster for shorter DFs. Recently, downflows and upflows occurring at the base and tops of mottles, respectively, were reported. To explain this dynamic structure the magnetic reconnection as a potential driver of mottles was suggested. As an extension of the works mentioned above, in this proposal we aim at identification of the center-to-limb variation of kinematic properties of dynamic fibrils and also center-to-limb variation of terminal wavelength shift of visibility of the fibrils and mottles in the H alpha line profile. Thus, the spectral observations of chromosphere with the best, spatial and spectral resolution, are needed. More details: campaign page: http://www.astro.sk/~choc/open/08_dot/08_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 / 47 186.88 p Fe XII (the spectral window selected to cover also 186.00 Fe VIII line) 263.76 p Fe XXIII ******************************************************************************* STUDY-SPECIFIC INFORMATION/DESCRIPTION: ******************************************************************************* STUDY TITLE: Solar microflares and network dynamic fibrils - relevance for coronal heating and mass supply TARGET/POINTING: 1/ quit sun at the disk center or alternatively 2/ an AR (or its remnants) near the disk center EXPOSURE TIME: 10s SLIT: 2" COMPRESSION: JPEG90 Number of studies: 2 1/ Study dot+eis:mic_fib_con: scanning, step size: 2", FOV: 44"x120" 2/ Study dot+eis:mic_fib_sit: sit-and-stare, FOV: 2"x120" USE/INSTRUCTIONS TO PLANNERS: STUDY NAME RASTER NAME dot+eis:mic_fib_con: consisting of only one raster Context_calib_jr_08 dot+eis:mic_fib_sit: consisting of only one raster Obs_sit_stare_jr_08 C. Ordering of the studies (with no. of repeats) : STUDY RASTER Repetition Time Total time 1. dot+eis:mic_fib_con Context_calib_jr_08 1 times 4m50s - number of study repetitions: 3, total time: 14m30s 2. dot+eis:mic_fib_sit Obs_sit_stare_jr_08 1 times - 10m - number of study repetitions: 11, total time: 1h50m - slit placed to the X-center of the previous rasters 3. dot+eis:mic_fib_con Context_calib_jr_08 1 times 4m50s - number of study repetitions: 3, total time: 14m30s - raster positioned at the previous slit position There could be an interruption between the previous and following study allowing any instrument specific upload of tables, etc. 4. dot+eis:mic_fib_con Context_calib_jr_08 1 times 4m50s - number of study repetitions: 3, total time: 14m30s 5. dot+eis:mic_fib_sit Obs_sit_stare_jr_08 1 times - 10m - number of study repetitions: 11, total time: 1h50m - slit placed to the X-center of the previous rasters 6. dot+eis:mic_fib_con Context_calib_jr_08 1 times 4m50s - number of study repetitions: 3, total time: 14m30s - raster positioned at the previous slit position Total time: 2 x 2h19m (Data volume: 2 x 51.23 MBits) PREFERRED OBSERVING TIME SLOT (~DOT/LaPalma): ~09 - ~13 UT PREFERRED POINTING (~DOT/LaPalma): if disk center: then to have x=0 at 10UT while compensating for solar rotation SCHEDULING OF THE PROGRAM: Program is prepared according new study Submission requirements. The planner is free to change number of repetitions of the study 2. and 5. in the ordering of studies above in order to allow an optimum interruption of the program due to instrument specific uploads, etc. Nevertheless we would extremely welcome if our program can be run in the preferred observing time slot (09-13UT). ******************************************************************************* 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_08 ------------------------------------------------------------------------------ 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 32 log T=6.1 4240 256.32* c He II 32 log T=4.9 247 186.88 p Fe XII 40 log T=6.1 (186.00 Fe VIII log T=5.6 inside Fe XII 186.88 window) 263.76 p Fe XXIII 32 log T=7.1 (*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: 120 (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): 40 steps -> 41 slit positions 5.2 Fine mirror step size (in arcseconds): 2 ------------------------------------------------------------------------------ 6. Compensation for Differential Solar Rotation: Yes (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): 287 7.5 Anticipated data volume, if known (in kilobits, not kilobytes): 1830 kb 7.6 Anticipated mean data rate, if known (in kilobits per second): 5870 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: 1 (i.e. number of times to execute before the next raster) ------------------------------------------------------------------------------ 9. Compression 9.1 Compression type: JPEG90 (choose one of "DPCM", "JPEG1", "JPEG2" or "None") ------------------------------------------------------------------------------ 9.2 Desired Compression factor: (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_08 ------------------------------------------------------------------------------ 2. Line list (please append desired lines to the following list if necessary): 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 / 47 186.88 p Fe XII (the spectral window selected to cover also 186.00 Fe VIII line) 263.76 p Fe XXIII (*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: 120 (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): 48 OR 5.4 Duration of sit'n'stare (in seconds): 480 (Note: Entering either parameter will automatically allow the planner to calculate the other.) ------------------------------------------------------------------------------ 6. Compensation for Differential Solar Rotation: Yes (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): 480 7.5 Anticipated data volume, if known (in kilobits, not kilobytes): 3659 kb 7.6 Anticipated mean data rate, if known (in kilobits per second): 5870 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: 1 (i.e. number of times to execute before the next raster) ------------------------------------------------------------------------------ 9. Compression 9.1 Compression type: JPEG90 (choose one of "DPCM", "JPEG1", "JPEG2" or "None") ------------------------------------------------------------------------------ 9.2 Desired Compression factor: (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: __________________ ******************************************************************************** ******************************************************************************* Study dot+eis:mic_fib_con: Study dot+eis:mic_fib_con: Study dot+eis:mic_fib_con: Study dot+eis:mic_fib_con: Study dot+eis:mic_fib_con: