SOT Preliminary Science Plan

SOT Preliminary Science Plan

Tom BergerLMSAL

SOT 17 MeetingNOAJApril 17-20, 2006

Solar-B Top Level Science GoalsA. Understand the origin and dynamics of the Solar magnetic Field

1. Large-scale structure and dynamics of active regions.2. The mechanisms of sunspot formation, dynamics, and decay.3. Small-scale magnetic fields: global vs. local or “fast” dynamo action.

B. Understand the modulation of Solar irradiance and luminosity by the magnetic field1. Active region irradiance contributions: sunspot& facular contrast as f(). 2. Photospheric network irradiance contributions.3. Physics of small-scale magnetic element irradiance.4. Chromospheric irradiance variations over the solar cycle.

C. Discover the source of heating of the upper atmosphere1. Coronal heating mechanisms: photospheric/chromospheric drivers.2. Spicules, jets, microflares.3. MHD waves and atmospheric seismology.4. Connectivity of photospheric magnetic structures to coronal loops.

D. Identify the physical mechanisms behind flares and coronal mass ejections. 1. Photospheric magnetic field evolution during flares.2. Prominence/filament formation.3. CME initiation and evolution.4. Photospheric and chromospheric response to transients (particles and waves).

SOT/FPP Science ProgramsA.1. Large-scale active region structure and dynamics

A.1.1. Active region evolution: the “flux history” of active regions AR_FLUXA.1.2. Active region surface flowfields AR_FLOWA.1.3. Active region sub-surface flowfields AR_SUBFA.1.4. Active region decay mechanisms AR_DCAYA.1.5. Active region helicity, currents, non-potential fields AR_HELI

A.2. Sunspot formation, dynamics, and decayA.2.1. Sunspot formation mechanisms SS_FORMA.2.2. Sunspot decay mechanisms SS_DCAYA.2.3. Sunspot penumbral structure, flows SS_PNUMA.2.4. Sunspot light-bridge and internal convective structures SS_CONVA.2.5. Sunspot wave frequencies and phases SS_WAVEA.2.6. Sunspot moving magnetic features SS_MMFS

A.3. Small-scale magnetic field structuresA.3.1. Small-scale field generation mechanisms SF_GENRA.3.2. Small-scale field interactions with convection SF_CONVA.3.3. Small-scale field thermodynamics SF_THRMA.3.4. Internetwork and weak fields SF_WEAKA.3.5. Ephemeral region origins and flowfield interactions SF_EPHM

SOT/FPP Science Programs

B. Solar IrradianceB.1 Active region irradiance budget SI_ACTVB.2. Photospheric network irradiance SI_PNETB.3. Physics of small-scale magnetic structure irradiance SI_PHYSB.4. Chromospheric irradiance variability SI_CHRM

C. Coronal HeatingC.1. Photospheric and chromospheric mechanisms CH_MECHC.2. Spicules, jets, and microflares CH_SPICC.3. MHD waves and atmospheric acoustics CH_MHDWC.4. Connectivity of the corona to the photosphere & chromosp. CH_PCON

D. Flares and Transient EventsD.1. Photospheric magnetic field changes during flares FT_PHOTD.2. Prominence & Filament activation FT_PROMD.3. CME initiation FT_CMESD.4. Photospheric & chromospheric impacts (particles & waves) FT_PART

A.1.1. Active Region Evolution: the “flux history” of active regionsScientific ObjectiveTo 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 -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?

RequirementsSynoptic 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 ProgramTarget: 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– H 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.

Sample SOT/FPP Science Program

XRT: AR DEM Program DEM6 filter set Full resolution 60 sec cadence EIS: He II 256 for H align TR lines Raster over SOT field

Sample SOT/FPP Science ProgramA.1.3. Active Region Subsurface Flows

Scientific ObjectiveTo 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?

RequirementsExtended “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 ProgramTarget: 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.

Sample SOT/FPP Science ProgramA.3.4. Internetwork (IN) and weak magnetic fields

Scientific ObjectiveTo 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?

RequirementsQuiet 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 ProgramTarget: 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.

Sample SOT/FPP Science ProgramB.1. Active Region Irradiance Budget

Scientific ObjectiveTo 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.

RequirementsObservation 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 ProgramTarget: 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– H 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.

Sample SOT/FPP Science ProgramC.2. Coronal Heating: spicules, jets

Scientific ObjectiveTo 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?

RequirementsObservations 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 ProgramTarget: 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– H 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.

Program vs. Observables Matrix

ProgramBFI NFI SP

388 396 430 450 550 668 517 525 557 589 630 656 NM FM DM DP

AR_FLUX F D V LC X

AR_FLOW F D IQUV X

AR_SUBF F D V X

AR_DCAY

AR_HELI

SS_FORM

SS_DCAY

SS_PNUM

SS_CONV

SS_WAVE

SS_MMFS

SF_GENR

SF_CONV F F F V X

SF_THRM

SF_WEAK F F F D V LC X

SF_EPHM

SI_ACTV F F F F V LS X

SI_PNET

SI_PHYS F F F F F F D IQUV LS X

SI_CHRM F F V F

Program vs. Observables Matrix (cont.)

KEY: F: FiltergramD: DopplergramV: Stokes V magnetogramIQUV: Stokes vector magnetogramLC: Line centerLS: Line scan

NM: Normal mapFM: Fast mapDM: Dynamics ModeDP: Deep magnetogram

ProgramBFI NFI SP

388 396 430 450 550 668 517 525 557 589 630 656 NM FM DM DP

CH_MECH

CH_SPIC F F D V LS X

CH_MHDW F F V D D V LS X

CH_PCON F F F V V IQUV LS X

FL_PHOT

FL_PROM F D IQUV LS X

FL_CMES

FL_PART

• Period of 4 months following Performance Verification (PV) phase

• 2006/Early 2007: close to solar minimum

• Targeting priorities1. Track any active region on the disk2. When no AR on disk

• Disk center QS studies• Irradiance scans• Prominence limb scans

3. Targets of Opportunity• Flaring regions• Active filaments

• Priority “minimum success” data– Vector magnetic map of AR– G-band movie of AR + granulation– H movies of AR– Ca II H-line movie of AR– Flare capture

Initial Science Operations Outline

AR on Sun?

Yes

No

Disk Center QSPrograms

Irradiance Scans

AR TrackingPrograms

Prominence/Polar Scans

Enough AR Data?

No

Yes

AR Tracking Programs

1. Emerging Active Region– Target: center on emerging flux region– Duration: 2 days

Ca II H 396.8 (1x1)

G-band 430.5 (1 x 1)

Blue Cont. 450.5 (1 x 1)

Fe I 630.2 Shutterless Stokes IQUV (1 x 1)

Fe I 557.6 Dopplergram (2 x 2)

H 656.3 Line Scan (2 x 2)(-350, LC, +350)

FG 1K x 1K FOV SP

Fast Map Mode3.2 sec/slit0.32” step

80” x 80” map

15 min/map

3 min/cycle?

NFI 80” x 80”

AR Tracking Programs2. Mature/Decaying AR

– Target: center on AR centroid– Duration: 7-14 days

Ca II H 396.8 (1x1)

G-band 430.5 (1 x 1)

Blue Cont. 450.5 (1 x 1)

Fe I 630.2 Stokes V Magnetogram (2 x 2)


H 656.3 Line Scan (1 x 1)(-350, LC, +350)

FG

4K x 2K FOV

SP

Normal Map Mode4.8 sec/slit0.16” step

164” x 164” map

83 min/map

10 min/cycle?Green Cont. 550.0 (1 x 1)

Red Cont. 668.4 (1 x 1)

Na D 589.6 Dopplergram (2 x 2)

Mg Ib 517.3 Stokes V Magnetogram (2 x 2)

NFI 320” x 160”


3. Flaring Active Region– Target: center on -spot or emerging flux region– Duration: triggered or ~1 day

Ca II H 396.8 (1x1)

G-band 430.5 (1 x 1)

Blue Cont. 450.5 (1 x 1)

Fe I 630.2 Stokes V Magnetogram (1x1)


H 656.3 Line Center (1 x 1)

FG 512 x 512 FOV SP

Dynamics Mode1.6 sec/slit0.16” step

16” x 32” map

3 min/map

30 sec/cycle?

NFI 40” x 40”


4. Active Region subsurface flows– Target: center on AR centroid near disk center– Duration: 1 day


FG 2K x 2K FOV SP


164” x 164” map

83 min/map

1 min/cycleFixed cadence

NFI 160” x 160”

Fe I 557.6 Continuum (1 x 1)

Quiet Sun Observing Programs

1. Quiet Network Flux Dynamics– Target: center on supergranular network– Duration: 2 days

G-band 430.5 (1 x 1)

Blue Cont. 450.5 (1 x 1)

Fe I 630.2 Shutterless IQUV (1 x 1)


FG512K x 1K FOV

SP


16” x 60” map

8 min/map

1 min/cycle?


NFI 40” x 80” Ca II H 396.8 (1x1)

Quiet Sun Observing Programs

2. Internetwork Flux– Target: center of supergranule– Duration: 1 day

G-band 430.5 (1 x 1)

Blue Cont. 450.5 (1 x 1)



FG1K x 1K FOV

SP

Deep Magnetogram Mode12.8 sec/slit0.16” step

16” x 80” map

15 min/map

1 min/cycle?


NFI 80” x 80” Ca II H 396.8 (1x1)

Irradiance Scan Programs1. 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)

Blue Cont. 450.5 (1 x 1)


FG4K x 2K FOV

SP


164” x 164” map

83 min/map

7 min/cycle?

Green Cont. 550.0 (1 x 1)

Red Cont. 668.4 (1 x 1)

H 656.3 Line Scan (2 x 2)(-350, LC, +350)

Ca II H 396.8 (1x1)

NFI 320” x 160”

Irradiance Scan Programs1. 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)

Blue Cont. 450.5 (1 x 1)


FG4K x 2K FOV

SP


164” x 164” map

83 min/map

3 min/cycle?

Green Cont. 550.0 (1 x 1)

Red Cont. 668.4 (1 x 1)

H 656.3 Line Scan (2 x 2)(-350, LC, +350)

Ca II H 396.8 (1x1)

NFI 320” x 160”

Prominence Observing Programs

1. Prominence at the limb– Target: see title…– Duration: 4 hours

Blue Cont. 450.5 (1 x 1)

Fe I 630.2 Shuttered Stokes IQUV (1x1)

H 656.3 Line Scan (1 x 1)(-700, -350, LC, +350, +700)

FG 1K x 1K FOV SP

Fast Map Mode3.2 sec/slit0.32” step

164” x 164” map

30 min/map

40 sec/cycle?

NFI 80” x 80”

Documents

SOT Preliminary Science Plan