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SOT Preliminary Science Plan

SOT Preliminary Science Plan. Tom Berger LMSAL SOT 17 Meeting NOAJ April 17-20, 2006. Solar-B Top Level Science Goals. Understand the origin and dynamics of the Solar magnetic Field Large-scale structure and dynamics of active regions.

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SOT Preliminary Science Plan

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  1. SOT Preliminary Science Plan Tom Berger LMSAL SOT 17 Meeting NOAJ April 17-20, 2006

  2. Solar-B Top Level Science Goals • Understand the origin and dynamics of the Solar magnetic Field • Large-scale structure and dynamics of active regions. • The mechanisms of sunspot formation, dynamics, and decay. • Small-scale magnetic fields: global vs. local or “fast” dynamo action. • Understand the modulation of Solar irradiance and luminosity by the magnetic field • Active region irradiance contributions: sunspot& facular contrast as f(m). • Photospheric network irradiance contributions. • Physics of small-scale magnetic element irradiance. • Chromospheric irradiance variations over the solar cycle. • Discover the source of heating of the upper atmosphere • Coronal heating mechanisms: photospheric/chromospheric drivers. • Spicules, jets, microflares. • MHD waves and atmospheric seismology. • Connectivity of photospheric magnetic structures to coronal loops. • Identify the physical mechanisms behind flares and coronal mass ejections. • Photospheric magnetic field evolution during flares. • Prominence/filament formation. • CME initiation and evolution. • Photospheric and chromospheric response to transients (particles and waves).

  3. SOT/FPP Science Programs A.1. Large-scale active region structure and dynamics A.1.1. Active region evolution: the “flux history” of active regions AR_FLUX A.1.2. Active region surface flowfields AR_FLOW A.1.3. Active region sub-surface flowfields AR_SUBF A.1.4. Active region decay mechanisms AR_DCAY A.1.5. Active region helicity, currents, non-potential fields AR_HELI A.2. Sunspot formation, dynamics, and decay A.2.1. Sunspot formation mechanisms SS_FORM A.2.2. Sunspot decay mechanisms SS_DCAY A.2.3. Sunspot penumbral structure, flows SS_PNUM A.2.4. Sunspot light-bridge and internal convective structures SS_CONV A.2.5. Sunspot wave frequencies and phases SS_WAVE A.2.6. Sunspot moving magnetic features SS_MMFS A.3. Small-scale magnetic field structures A.3.1. Small-scale field generation mechanisms SF_GENR A.3.2. Small-scale field interactions with convection SF_CONV A.3.3. Small-scale field thermodynamics SF_THRM A.3.4. Internetwork and weak fields SF_WEAK A.3.5. Ephemeral region origins and flowfield interactions SF_EPHM

  4. SOT/FPP Science Programs B. Solar Irradiance B.1 Active region irradiance budget SI_ACTV B.2. Photospheric network irradiance SI_PNET B.3. Physics of small-scale magnetic structure irradiance SI_PHYS B.4. Chromospheric irradiance variability SI_CHRM C. Coronal Heating C.1. Photospheric and chromospheric mechanisms CH_MECH C.2. Spicules, jets, and microflares CH_SPIC C.3. MHD waves and atmospheric acoustics CH_MHDW C.4. Connectivity of the corona to the photosphere & chromosp. CH_PCON D. Flares and Transient Events D.1. Photospheric magnetic field changes during flares FT_PHOT D.2. Prominence & Filament activation FT_PROM D.3. CME initiation FT_CMES D.4. Photospheric & chromospheric impacts (particles & waves) FT_PART

  5. Sample SOT/FPP Science Program A.1.1. Active Region Evolution: the “flux history” of active regions Scientific Objective To measure the distribution of magnetic flux over time for an ensemble of active regions. To determine the magnetic topologies that manifest themselves in the surface evolution; can we distinguish W-loops, U-loops, and horizontal flux tubes in the emergence process? Are there regular patterns to helicity, e.g. does it show hemispheric or solar cycle variation? Requirements Synoptic observation of several active regions per year over the course of the solar cycle. Requires at least some active regions to be observed during their initial emergence. Active regions must be tracked for as long as possible as they traverse the disk.Vector magnetic field maps as well as surface flow and Doppler velocity maps must be made with high spatial resolution with cadence varying from rapid (1 minute or less) during the initial emergence to moderate (2—5 minutes) during the mature and decaying phases. Observing Program Target: Multiple active regions including some emerging regions. FOV: Minimum 2K x 2K (164” x 164” in NFI), 4K x 2K for larger ARs to capture surrounding plage. Duration: 7—14 days continuous tracking of AR. Cadence: Emergence phase: high: 1 minute Mature/decay phase: moderate 2—5 minutes. FPP observables: NFI • Fe I 630.2 nm Stokes shuttered IQUV, 1x1 binning • Fe I 557.6 nm Dopplergram, 2x2 binning • Ha 656.3 nm line scam: -700 mÅ, LC, +700 mÅ, 2x2 binning BFI • Gband 430.5 nm, 1x1 binning SP • Normal map mode, full spatial resolution, 160 x 160 arcsecond scan widths depending on active region size. Mosaic maps if needed. • Repeat scans every 4—6 hours. XRT: AR DEM Program DEM6 filter set Full resolution 60 sec cadence EIS:He II 256 for Ha align TR lines Raster over SOT field

  6. Sample SOT/FPP Science Program A.1.3. Active Region Subsurface Flows Scientific Objective To measure the horizontal flows at a range of depths beneath active regions. Can we detect the 50 m/sec inflow around active regions recently measured with MDI local helioseismology and ring-diagram analysis? Do sunspots have systematic and scale varying downflows below the photosphere? Do moving magnetic features show a correlated velocity signature as a function of depth? Requirements Extended “staring” at an active region near disk center. Duration is 4 days minimum. Cadence can be moderate (2—3 minutes) but must be extremely regular for the duration of the observations. Uninterrupted pointing and smooth solar rotation compensation are required for the duration. Observing Program Target: Multiple active regions as close to disk center as possible. FOV: 2K x 2K (164” x 164” in NFI). Duration: 0.5 days continuous tracking of AR. Cadence: 1 minute. FPP observables: NFI • Fe I 557.6 nm Dopplergram, 2x2 binning • Fe I 630.2 nm Stokes V magnetogram, 2x2 binning BFI • Blue continuum 450.5 nm, 1x1 binning SP • None.

  7. Sample SOT/FPP Science Program A.3.4. Internetwork (IN) and weak magnetic fields Scientific Objective To measure the distribution of magnetic field, both in terms of flux density and field strength, outside of active regions with a resolution of 0.3”. Can we detect a latitudinal or solar cycle variation in this distribution? What is the distribution of size scales in the IN? What is the evolutionary history of IN flux? Can we detect the operation of a local/fast dynamo in the upper convection zone? Requirements Quiet Sun tracking with initial position at disk center. Spatial resolution as high as possible, highest possible polarimetric S/N in order to detect and measure magnetic elements with B < 100 G. FOV must encompass a supergranule area, at least partially. Duration of tracking on the order of 10 hours. Observing Program Target: Disk center Quiet Sun. FOV: 1K x 1K (80” x 80” in NFI). Duration: 10—15 hours. Cadence: moderate 2—5 minutes. FPP observables: NFI • Fe I 630.2 nm Stokes-V Magnetogram, 1x 1 binning • 16” mask shutterless Stokes IQUV • Fe I 557.6 nm Dopplergram, 1 x 1 binning BFI • Gband 430.5 nm, 1x1 binning • Ca II H-line 396.8 nm, 1x 1 binning SP • Deep magnetogram mode, window to 512 pixels along slit, 16” scan width, lossless compression.

  8. Sample SOT/FPP Science Program B.1. Active Region Irradiance Budget Scientific Objective To measure the continuum and spectral line contrast of active region sunspots, pores, micropores, and magnetic elements as a function of magnetic field strength at a range of disk positions, from extreme limb to disk center. To determine the horizontal and vertical flow patterns associated with AR faculae. To measure the brightness temperatures of AR components and compare them to quiet Sun values. Requirements Observation of a number of active regions at as many locations on the disk as possible with high spatial but moderate to low temporal resolution. Cotemporal observations of quiet Sun regions at the same line-of-sight angle as any active region observations (for QS reference contrast measurements). High photometric precision is required in the continuum filtergrams. Observing Program Target: Multiple active regions at various disk positions. FOV: 2K x 2K (164” x 164” in NFI). Duration: 4 hours. Cadence: 2—5 minutes. FPP observables: NFI • Fe I 557.6 nm Dopplergram, 2x2 binning • Fe I 630.2 nm shuttered Stokes IQUV, 2x2 binning • Fe I 630 nm continuum filtergram, 1 x 1 binning • Ha 656.3 nm line scam: -700 mÅ, LC, +700 mÅ, 2x2 binning BFI • Blue continuum 450.5 nm, 1x1 binning • Green continuum 555.0 nm, 1x1 binning • Red continuum 668.4 nm, 1x1 binning SP • Normal map mode, 164” scan width.

  9. Sample SOT/FPP Science Program C.2. Coronal Heating: spicules, jets Scientific Objective To measure horizontal and vertical velocity and magnetic field patterns in both the photosphere and chromosphere of spicules, larger jets, and microflares. Can we detect opposite polarity cancellation at the location of spicules? How are spicules related to the surface flowfield? Can we detect the existence of acoustic shocks in spicules? Are spicules found primarily along non-vertical magnetic flux tubes? Requirements Observations of spicules both at the limb and on the disk (where they are referred to as “mottles”). Both quiet network spicules and AR spicules (sometimes referred to as “fibrils”) are required in order to explore the full range of magnetic flux density values. Observing Program Target: Multiple active regions as close to disk center as possible. FOV: 1K x 1K (80” x 80” in NFI). Duration: 4—6 hours. Cadence: high 30—40 seconds. FPP observables: NFI • Mg Ib 517.3 nm Magnetogram, 2 x 2 binning • Fe I 557.6 nm Dopplergram, 1x 1 binning • Fe I 630.2 nm Magnetogram, 1x 1 binning • Ha 656.3 nm line scan: -700 mÅ, -350 mÅ, +350 mÅ, 1x 1 binning BFI • Gband 430.5 nm, 1x1 binning • Ca II H-line 396.8 nm, 1x 1 binning SP • Normal map mode, 80” scan width.

  10. Program vs. Observables Matrix

  11. Program vs. Observables Matrix (cont.) KEY: F: Filtergram D: Dopplergram V: Stokes V magnetogram IQUV: Stokes vector magnetogram LC: Line center LS: Line scan NM: Normal map FM: Fast map DM: Dynamics Mode DP: Deep magnetogram

  12. Initial Science Operations Outline • Period of 4 months following Performance Verification (PV) phase • 2006/Early 2007: close to solar minimum • Targeting priorities • Track any active region on the disk • When no AR on disk • Disk center QS studies • Irradiance scans • Prominence limb scans • Targets of Opportunity • Flaring regions • Active filaments • Priority “minimum success” data • Vector magnetic map of AR • G-band movie of AR + granulation • Ha movies of AR • Ca II H-line movie of AR • Flare capture AR on Sun? No Disk Center QS Programs Yes AR Tracking Programs Irradiance Scans Prominence/Polar Scans Enough AR Data? Yes No

  13. AR Tracking Programs • Emerging Active Region • Target: center on emerging flux region • Duration: 2 days FG SP 1K x 1K FOV 80” x 80” map NFI 80” x 80” Ca II H 396.8 (1x1) 3 min/cycle? G-band 430.5 (1 x 1) Fast Map Mode 3.2 sec/slit 0.32” step Blue Cont. 450.5 (1 x 1) 15 min/map Fe I 630.2 Shutterless Stokes IQUV (1 x 1) Fe I 557.6 Dopplergram (2 x 2) Ha 656.3 Line Scan (2 x 2) (-350, LC, +350)

  14. AR Tracking Programs 2. Mature/Decaying AR • Target: center on AR centroid • Duration: 7-14 days 4K x 2K FOV NFI 320” x 160” FG Ca II H 396.8 (1x1) SP 164” x 164” map G-band 430.5 (1 x 1) Blue Cont. 450.5 (1 x 1) 10 min/cycle? Green Cont. 550.0 (1 x 1) Normal Map Mode 4.8 sec/slit 0.16” step Red Cont. 668.4 (1 x 1) Fe I 630.2 Stokes V Magnetogram (2 x 2) Fe I 557.6 Dopplergram (2 x 2) 83 min/map Na D 589.6 Dopplergram (2 x 2) Mg Ib 517.3 Stokes V Magnetogram (2 x 2) Ha 656.3 Line Scan (1 x 1) (-350, LC, +350)

  15. AR Tracking Programs 3. Flaring Active Region • Target: center on d-spot or emerging flux region • Duration: triggered or ~1 day FG SP 512 x 512 FOV 16” x 32” map NFI 40” x 40” Ca II H 396.8 (1x1) G-band 430.5 (1 x 1) Dynamics Mode 1.6 sec/slit 0.16” step Blue Cont. 450.5 (1 x 1) 30 sec/cycle? Fe I 630.2 Stokes V Magnetogram (1x1) 3 min/map Fe I 557.6 Dopplergram (2 x 2) Ha 656.3 Line Center (1 x 1)

  16. AR Tracking Programs 4. Active Region subsurface flows • Target: center on AR centroid near disk center • Duration: 1 day FG SP 2K x 2K FOV 164” x 164” map NFI 160” x 160” Normal Map Mode 4.8 sec/slit 0.16” step 1 min/cycle Fixed cadence 83 min/map Fe I 557.6 Dopplergram (1 x 1) Fe I 557.6 Continuum (1 x 1)

  17. Quiet Sun Observing Programs 1. Quiet Network Flux Dynamics • Target: center on supergranular network • Duration: 2 days FG SP 16” x 60” map 512K x 1K FOV NFI 40” x 80” Ca II H 396.8 (1x1) G-band 430.5 (1 x 1) Normal Map Mode 4.8 sec/slit 0.16” step Blue Cont. 450.5 (1 x 1) 1 min/cycle? 8 min/map Fe I 630.2 Shutterless IQUV (1 x 1) Fe I 557.6 Dopplergram (1 x 1) Ha 656.3 Line Center (1 x 1)

  18. Quiet Sun Observing Programs 2. Internetwork Flux • Target: center of supergranule • Duration: 1 day FG SP 16” x 80” map 1K x 1K FOV NFI 80” x 80” Ca II H 396.8 (1x1) 1 min/cycle? G-band 430.5 (1 x 1) Deep Magnetogram Mode 12.8 sec/slit 0.16” step Blue Cont. 450.5 (1 x 1) 15 min/map Fe I 630.2 Stokes V Magnetogram (1 x 1) Fe I 557.6 Dopplergram (1 x 1) Ha 656.3 Line Center (1 x 1)

  19. Irradiance Scan Programs 1. Activity Belt Irradiance • Target: Activity belts (40°N – 40°S) from East limb to West limb • SC pointing mosaic • Duration: 2 hours (depends on SC pointing/stabilization rate) FG SP 164” x 164” map 4K x 2K FOV NFI 320” x 160” Blue Cont. 450.5 (1 x 1) Green Cont. 550.0 (1 x 1) Normal Map Mode 4.8 sec/slit 0.16” step Red Cont. 668.4 (1 x 1) 7 min/cycle? Ca II H 396.8 (1x1) 83 min/map Fe I 630.2 Stokes V Magnetogram (2 x 2) Ha 656.3 Line Scan (2 x 2) (-350, LC, +350)

  20. Irradiance Scan Programs 1. Polar Region Scans • Target: Polar regions (60—90°N & 60—90°S) from East limb to West limb • SC pointing mosaic • Duration: 2 hours (depends on SC pointing/stabilization rate) FG SP 164” x 164” map 4K x 2K FOV NFI 320” x 160” Blue Cont. 450.5 (1 x 1) Green Cont. 550.0 (1 x 1) Normal Map Mode 4.8 sec/slit 0.16” step Red Cont. 668.4 (1 x 1) 3 min/cycle? Ca II H 396.8 (1x1) 83 min/map Fe I 630.2 Stokes V Magnetogram (2 x 2) Ha 656.3 Line Scan (2 x 2) (-350, LC, +350)

  21. Prominence Observing Programs 1. Prominence at the limb • Target: see title… • Duration: 4 hours FG SP 1K x 1K FOV 164” x 164” map NFI 80” x 80” Blue Cont. 450.5 (1 x 1) Fast Map Mode 3.2 sec/slit 0.32” step 40 sec/cycle? Fe I 630.2 Shuttered Stokes IQUV (1x1) 30 min/map Ha 656.3 Line Scan (1 x 1) (-700, -350, LC, +350, +700)

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