Title : Characterizing the Energetics and Dynamics of the Quiet Sun Authors: B. De Pontieu, A. De Wijn, S. McIntosh [LEAD], K. Reardon Other Correspondents: M. Carlsson, W. Curdt, G. Cauzzi, E. DeLuca, B. Fleck, S. Gregory, J.B. Gurman, V. Hansteen, L. Harra, C. Henney, S. Jefferies, B. Lites, M.P. Miralles, K. Reeves, T.D. Tarbell, S. Tomczyk, A. Vourlidas, P.R. Young, D. Williams Update History First Draft (19 November 2007) Third Draft (24 November 2007) Fourth Draft (26 November 2007) Fifth Draft (31 January 2008) Sixth Draft (2 April 2008) [Modified SUMER, Hinode/SOT, IBIS - Removed MOTH, COMP] Participating Instruments and Observatories Space Based: SOHO/CDS, SOHO/EIT, and possibly SUMER -- campaign contact S. McIntosh [SOHO Coordination] SOHO/UVCS -- campaign contact M.P. Miralles SOHO/MDI -- campaign contact S. Gregory STEREO/SECCHI/EUVI -- campaign contact A. Vourlidas [STEREO Coordination] Hinode/XRT -- campaign contact K. Reeves Hinode/SOT -- campaign contact A. De Wijn [Hinode Coordination] Hinode/EIS -- campaign contact D. Williams TRACE -- campaign contact T. Winter [TRACE Coordination] Ground based: NSO/IBIS -- campaign contact K. Reardon [NSO Coordination] NSO/SPINOR -- campaign contact A. Norton Scientific Objective Our global objective is to make a detailed study of the response of the quiet solar chromosphere, transition region and corona to the constantly evolving photospheric magnetic field - these joint observations will show that there is no place in the solar atmosphere that is magnetically or dynamically quiet. With these observations we hope to gain reasonable estimates of the energy flux through the chromosphere and lower transition region. Further, this study will allow to study the structural elements [spicules, fibrils, mottles, etc] of the chromosphere and transition region, assess the relevance/importance of magneto-atmospheric [MA] wave energy versus direct magnetic energy release in the atmosphere below temperatures at which thermal conduction becomes significant. Further, we can use these observations to investigate MA mode generation, coupling and conversion as a result of photospheric motions and their interplay with magnetic structures. To reach the global objective we will need to make detailed measurements of the targeted magnetic environment, monitor the multitude of magneto-atmospheric waves and the radiative response of the plasma at multiple "heights" threading the atmosphere. We will perform the observations [detailed below] at chosen target locations during the WHI QS period. ---------------------------------------------------- Scientific Justification We will exploit recently revitalized interest in the quiet solar chromosphere (and transition region) that has been motivated, among other things, by the unprecedented observations of Hinode, showing that this region is far from quiet. The chromosphere and transition region are where (in general) the hydrodynamic and magnetic forces vie for dominance, forming the "magnetic transition region" between high and low beta plasmas. Much of what we hope to achieve in the proposed observing campaign relates to understanding the flow of mass and energy into and through this interface. Our goal is to fully characterize this region, fully aware that understanding the symbiotic interplay of magnetic field, MA wave and plasma motions (each driven by the relentless magneto-convection of the solar interior) is critical to achieving this goal. To perform this task we will use some of the finest observational tools available to measure [vector and line-of sight] magnetic fields in the photosphere and chromosphere at high spatial resolution, simultaneous Doppler motions of the plasma at multiple "heights" and obtain full spectroscopic information at spatial resolutions less than or equal to 1 arcsecond in scale. In our principal field of view, covering several supergranules, we will see a multitude of phenomena [spicules, jets, shocks, mottles, surges, macrospicules, blinkers, etc] all of which are gradually being tied to the forcing of magneto-convection and forced magnetic reconnection. This study may, in some way, serve to unify and "clean-up" the literature on these topics. Our observing program will combine disk center and limb observations. Each, as we have found with Hinode, will provide excellent context and insight into the other. When observing a limb target we will attempt to get better measurements of the Alfvenic energy flux through the quiet atmosphere and address their potential for heating the solar corona [as well driving the fast/slow wind] likely to be a hot topic of debate requiring detailed measurement. Our observing suite will be complimented at the limb by include observations from CoMP and SOHO/UVCS - these observations have the potential go a long way to addressing the balance between low-frequency driven MHD turbulence and high-frequency [ion-cyclotron] waves in the acceleration of the solar wind. Our team is comprised of experts in the realm of chromospheric, transition region and coronal dynamics, observation and simulation. These observations offer a truly unique opportunity to make a significant breakthrough in understanding the "basal" energetic processes effecting the Sun and Heliosphere. Recent Related/Relevant Publications of Core Science Team: Carlsson, M., et al. 2007, "Can High Frequency Acoustic Waves Heat the Quiet Sun Chromosphere?" in press PASJ special Hinode "first light" Issue. Cauzzi, G., et al., 2007, "The solar chromosphere at high resolution with IBIS. I. New insights from the Ca II 854.2 nm line", A&A (in press) De Pontieu, B., et al., 2007, "High Resolution Observations and Modeling of Dynamic Fibrils", ApJ, 655, 624 De Pontieu, B., et al., 2007, "A Tale Of Two Spicules: The Impact of Spicules on the Magnetic Chromosphere", in press PASJ special Hinode "first light" Issue. De Pontieu, B., et al., 2007, "Chromospheric Alfvenic Waves strong enough to Power the Solar Wind". In press Science [December 7 2007] de Wijn, A.G. & De Pontieu, B., 2006, "Dynamic fibrils in H and CIV", A&A, 460, 309 Hansteen, V., et al., 2006, "Dynamic Fibrils Are Driven by Magnetoacoustic Shocks", ApJ, 647, L73 Hansteen, V., et al., 2007, "On connecting the dynamics of the chromosphere and transition region with Hinode SOT and EIS" in press PASJ special Hinode "first light" Issue. Jefferies, S.M., et al., 2006, "Magnetoacoustic Portals and the Basal Heating of the Solar Chromosphere", ApJ, 648, L151 McIntosh, S.W., De Pontieu, B. & Tarbell, T.D., 2008, "Reappraising Transition Region Line Widths in light of Recent Alfvén Wave Discoveries", in press ApJL McIntosh, S.W., et al., 2007, "Observations Supporting the Role of Magnetoconvection in Energy Supply to the Quiescent Solar Atmosphere", ApJ, 654, 650 McIntosh, S.W. & Jefferies, S.M., 2006, "Observing the Modification of the Acoustic Cutoff Frequency by Field Inclination Angle", ApJ, 647, L77 Rouppe van der Voort, L.H.M., 2007, "Magnetoacoustic Shocks as a Driver of Quiet-Sun Mottles", ApJ, 660, 169 Tomczyk, S., et al. 2007, "Alfvén Waves in the Solar Corona", Science, 317, 1192 Vecchio, A., et al., 2007, "Solar Atmospheric Oscillations and the Chromospheric Magnetic Topology", A&A, 461, L1 ---------------------------------------------------- Operational Considerations The ground based observations critical to this study are based in SW Mainland US. At NSO/SP the prime seeing time is 14:00-18:00 UT. Observing targets will be chosen to maximize scientific return and for their diagnostic differences. For example, we hope to spend at least one day characterizing the limb of the quiet atmosphere for comparison to disk center measurements of extended structure [spicules] in the chromosphere and transition region - the limb target will also permit Alfven wave studies combining Hinode [SOT, EIS], SOHO [UVCS/SUMER] & COMP. A team member in Japan [De Wijn] will have final ability to change the target and will be based on the Hinode pointing of that day. Observations just above the limb with SUMER may require interactive confirmation of the slit position, which will depend on observer and telemetry availability. ***************************************************** Detailed Observing Sequences per Instrument (may need revision later, based on input from instrument teams). SOHO/EIT: We would like to request CME_watch data be acquired in 304 for the QS week. SOHO/CDS: (QUICK/v6: 26x150 raster with 2x240 slit) Complimentary lines to SUMER, those spanning the same temperature range and filling the temperature gap between OV and NeVIII. Need CDS to raster estimated SUMER position (+/-13 arcseconds) whence post-analysis will ensure cross-correlation between the individual observations at each timestep. Spectral lines : OIII (559.56); OV (629.74); NeVI (562.80); HeI (584.33); MgIX (368.06); He II (303.78; in second order) SOHO/UVCS: Limb Target Only UVCS will observe at 1.7 Rsun, obtaining line profiles for Ly beta, Ly gamma, C III 977, O VI 1032, O VI 1037 and Si XII 520 with a 124 second cadence. SOHO/SUMER: SUMER will observe in two wavelength ranges and will perform a small set of observations for each pointing and range: (1) A full detector readout at the initial pointing with the long slit. For wavelength calibration. (2) A 120" x 300" context raster in N IV / Ne VIII with 2" increment and 30s exposure for context. [for limb observations the context raster will be removed] (3) Sit-and-stare in 5 windows with 25s caadence and solar rotation tracking on. Detector - Detector B Duration of each sequence: 205 min + 20 min memory dump Slit: 120"x1" slit (SUMER Slit #2 for timeseries); 120"x1" slit (SUMER Slit #2 for timeseries) Spectral Windows: 1) The 760-790 spectral range - OV (760.228); NIV (765.143); NeVIII (770.324), NeVIII (780.324); OIV(787.71) 2) The 1390-1410 spectral range - Si IV (1394, 1402); OIII /2(704); S I (1396), continuum (1391) SOHO/MDI: High Res FOV Observations [if possible for on-disk studies] Regular Full Disk Observations [magnetograms/dopplergrams at 60s] STEREO/SECCHI: EUVI normal synoptic data [304, 195, 284 - 10 mins, 171 - 1 minute]. Hinode/EIS: - 1 rasters of target region "HPW004_QS_RAST_120m" at start of sequence. - for one hour of each targeted run do "IUU_QS_SNS_001" sit and stare at the image center of SOT/XRT Hinode/SOT: SP: Fast Maps, repeating, 60"x60" 1.7 s/slit => ~600 s cadence, 2x2 binning => 0.3" px size (512*112 ccd px/slit) / (1.7 s/slit) / (2*2) = 8433 px/s Multiply by 4 for I, Q, U, V (8433 px/s *4) = 33732 px/s Compression : JPEG Q65 (2.1 b/px for I, Q, U &V) -> 70837 b/s - Number of steps in each map: 60"/0.3" = 200 (x2) - 4s (400*0.1) return time for the map to restart. Header: 1250 b/slit / (1.7 s/slit) / (2 slits/image) = 368 b/s Total Data Rate: 69.53 Kb/s NFI: Fe I 6301.5 IV, 61"x82", 16 s cadence or Mg B 5172.7 IV, 61"x82", 16 s cadence or Na I 5890.6 IV, 61"x82", 16 s cadence 2x2 binning => 0.16" resolution, shutterless : 2 * 384x1024 = 786432 px per image: (384*1024 ccd px/image) * 2 images / (16 s/image) / (2*2) = 12288 px/s JPEG Q65: 1.9 b/px for I, 2.2 b/px for V (12288 px/s) * ((1.9 + 2.2) b/px) = 50381 b/s Header: (1000 b/image) / (16 s/image) * (2 images) = 125 b/s Total data rate: 49.32 Kb/s Mg B 5172.7 DG, 57"x82", 16 s cadence or Na I 5890.6 DG, 57"x82", 16 s cadence 2x2 binning => 0.16" resolution per image: (704*1024 ccd px/image) / (16 s/image) / (2*2) = 11264 px/s JPEG Q65: 1.9 b/px for I (2 images in DG) (11264 px/s) * 2 images * (1.9) b/px) = 42803 b/s Header: (1000 b/image) / (16 s/image) * (2 images) = 125 b/s Total data rate: 41.93 Kb/s Mg B 5172.7 IVDG, 61"x82", 20 s cadence or Na I 5890.6 IVDG, 61"x82", 20 s cadence 2x2 binning => 0.16" resolution 2x2 binning => 0.16" resolution, shutterless : 2 * 384x1024 = 786432 px per image: (384*1024 ccd px/image) / (20 s/image) / (2*2) * (2 images) = 9830 px/s JPEG Q65: 1.9 b/px for I (2 images), 2.2 b/px for V (2 images) (9830 px/s) * ((1.9 + 1.9 + 2.2 + 2.2) b/px) = 80609 b/s Header: (1000 b/image) / (16 s/image) * (4 images) = 250 b/s Total data rate: 78.97 Kb/s BFI: Ca II H (3968.5 Ang), 50"x50", 16 s cadence 500 ms exposure, 2x2 binning => 0.1" px size (1024*1024 ccd px/image) / (16 s/image) / (2*2) = 16384 px/s JPEG Q75: 2.1 b/px 16384 px/s * 2.1 b/px = 34406 b/s Header: (600 b/image) / (16 s/image) = 38 b/s Total Data Rate: 33.64 Kb/s Hinode/XRT: Filters: Al/poly (8 sec exposure), Ti/Poly (16 sec exposure) Cadence: ~30 sec cadence FOV: 250"x250" centered on target region [capture aspects of global connectivity] Context: Al/poly (2048x2048, 2x2 binned), 5 thin Be (768"x384" 23sec) every ~30 minutes Note: In the case of an active region on the sun, the long exposures can be replaced by multiple short exposures. TRACE: Main wavelength: Alternating 1600/1700 TDT.any_frames [McIntosh "INO" Program] Cadence: ~ 12s FOV: 640x512 pixels (320"x256") centered on target region [capture aspects of global connectivity] Context : 171/195/WL taken at start and end of each hour-long sequence. NSO/IBIS: Combination of spectroscopic measurements with a 40"x80" FOV. Ca II 8542 - Line profile scans - Chromospheric dynamics Halpha 6563 - Line profile scans - Chromospheric dynamics Na I D - Line profile scans - Chromospheric dynamics - Calibration of Hinode/NFI Na Dopplergrams Total cadence: 20-28 sec for all three lines Rapid scans (repeated observations in one line with a 3-5 second cadence might also be obtained for studying rapid dynamics) Speckle imaging in CN or CH band * Ca II 8542 - spectropolarimetry - chromospheric/TR magnetic fields - this will be used if needed but reduces cadence to ~60s NSO/SPINOR: Simultaneous observation of the following in a 30"x30" field of view. Will coordinate observing periods with IBIS. Fe I 15648 (g=3) and 15652 (g=1.53) on FLIR (or new IR) camera Fe I 6301 (g=1.66) and 6302 (g=2.5) on ERNIE camera Fe II 4233 (g=2.8) on BERT camera O I 7774 on SARNOFF camera