Topic

Objective

Solar Condition / Rank

XRT Type

Exposure time

Cadence

Filters in inner loop

XRT FOV

Duration

Description

SOT Support

EIS Support (see attachment)

Ground Support

Space Support

Stress buildup

To determine where and how free energy is stored in the corona.

AR preflare: Highest

Topology

1 sec/ 4sec/ 8 sec; AEC

45 sec

2

512x512

5 days

High resolution; 2-3 filters; moderate FOV; high/moderate cadence; 24 hours continuous

Program 1c

Program 1a

H-alpha

EUV imaging (TRACE, SDO)

Flows/Longitudinal waves; MHD waves

To determine whether waves are seen in coronal active regions.

AR/FL : High

Dynamic

4 sec; Fixed

1 min

1

1024x1024

5 days

High cadence; 1 filter at a time; 2hours continuous; low compression rate; For flaring AR use pre-flare buffer to take high cadence 1-filter data.

Program 1b

Program 1a

EUV imaging (TRACE, SDO)

MHD wave heating

To determine the role of waves in transporting energy and momentum to the corona.

AR: High

Dynamic

1 sec; AEC

10 sec/ 1 min

1

512x512

3 days

High cadence; highest angular resolution; 1 filter at a time; fixed exposures; 2 hours continuous; lossless; prefer non-flaring AR; for later runs, include 2 filters for T & EM

Program 1c

Program 1a

EUV imaging (TRACE, SDO)

Loop Life Cycle

To determine how coronal loops appear and disappear.

AR: Medium

Energetics

8 sec; AEC

1 min

3

512x512

6 days

3-4 filters; 24 hours continuous

Program 1e

Context + 2b

Large fov magnetograms

EUV imaging (TRACE, SDO)

Loop Thermal Structure

To establish the basic observables, T and ne, of coronal loops.

AR: High

Energetics

8 sec; AEC

1 min

5

512x512

6 days

5-7 filters; 24 hours continuous

Program 1e

Program 1b

Large fov magnetograms

EUV imaging (TRACE, SDO)

Jet initiation

To establish the conditions under which coronal jets are produced.

AR: Medium

Energetics

4 sec; AEC

45 sec

2

512x512

6 days

High cadence; high resolution; 2-3 filters; 2-3 hours (burst mode) 1-2 times per day; center FOV on western edge of AR

Program 1c

Context + 2b

EUV imaging (TRACE, SDO)

AR-AR interconnection

To determine the nature of interactions between structures in different Ars.

AR emerging: High

Energetics

4 sec/ 45 sec; AEC

1 min

2

512x512

4 days

2 filters; long & short exposures; high resolution; moderate cadence; moderate FOV; 3 day continuous

Program 1c

Context + 2b

Large fov magnetograms

EUV imaging (TRACE, SDO)

Jet Life Cycle

To track the evolution of coronal jets over their full observable lifetime.

AR Emerging: Medium

Dynamic

1 sec/ 4sec/ 8 sec,AEC

15 sec

2

512x512

4 days

High cadence; 2-3 filters; 2-3 hours (burst mode) 1-2 times per day

Program 1c

Program 2b

EUV imaging (TRACE, SDO)

Filament Activation

To establish the conditions under which filaments and prominences become active in the corona.

AR/QS: Low

Topology

8 sec/ 45 sec; Fixed

1 min

2

768x768

3 days

2 filters; long & short exposures; 24 hr continuous

Program 3

Context + 3

Large fov magnetograms; large fov H-alpha

EUV imaging (TRACE, SDO)

Separatrix Heating

To locate active separatrices in the corona.

AR/QS: Low

Topology

8 sec/ 45 sec; AEC

1 min

2

512x512

12 hours

2 filters; long & short exposures; 12 hr continuous

Program 1c

Context + 2a

Large fov magnetograms

EUV imaging (TRACE, SDO); Stereo

Nano-Flares

To measure the power spectrum of the smallest detectable flare events in the corona.

AR: Low

Energetics

8 sec; AEC

1 min

3

512x512

3 days

3 filters; 24 hours continuous

Program 1e

Context + 2a

Large fov magnetograms

EUV imaging (TRACE, SDO)

LASCO-XRT Downflow simultaneity

To locate and determine the properties of postflare downflows in the upper branches of flare reconnection sites.

CH/AR/Flare-post: High

Topology

45 sec; Fixed

1 min

2

1024x1024

3 days

1-2 filters; long exposures; region near limb (CMD > 45 degrees); large FOV; moderate cadence

Program 3

Context

Coronagrams

EUV imaging (TRACE, SDO); Stereo; LASCO

Filament structure

To determine the topology of coronal structures in and around filaments.

AR/QS: Medium

Energetics

32 sec; AEC

1 min

3

512x512

2 days

3-4 filters; 24 hour continuous

Program 2a

Hot & cool line vel; Context+Program 3

Large fov magnetograms; large fov H-alpha

EUV imaging (TRACE, SDO); Stereo

XBP Topology

To find the topological structure of X-ray bright points.

QS: Medium

Topology

1 sec/ 45 sec; AEC

1 min

1

512x512

2 days

1 filter at a time; long and short exposures; 10 hours per filter;

Program 2a

Slot images; coordinate lines with XRT filter changes; Context + 1b + 2a

He 10830; H-alpha

EUV imaging (TRACE, SDO)

XBP Thermal Structure

To determine the coronal T and ne of X-ray bright points.

QS: High

Energetics

8 sec; AEC

1 min

4

512x512

2 days

4-6 filters; 24 hour continuous

Program 2a

Program 2b

He 10830; H-alpha

EUV imaging (TRACE, SDO)

XBP Life Cycle

To track the evolution of XBP over their full observable lifetime.

QS: Medium

Energetics

32 sec; AEC

3 min

3

512x512

2 days

3-4 filters; 24 hour continuous

Program 2a

Cool context

He 10830; H-alpha

EUV imaging (TRACE, SDO)

Magnetic carpet

To determine the observable properties of the small-scale B.

QS/CH/ Polar CH: Low

Topology

16 sec/45 sec; AEC

2 min

1

512x512

2 days

Thin filter, long and short exposures; moderate cadence; 24 hours;

Program 1e

Context

He 10830

EUV imaging (TRACE, SDO)

Coronal Hole Boundary

To measure the locations and evolution of coronal hole boundary structures.

CH: Medium

Dynamic

32 sec; Fixed

2 min

1

1024x512

6 days

Moderate cadence; 1-2 filters; 24 hours continuous;

Program 1e

Context + 1b

Large fov magnetograms; He 10830;

Polar Plume Jets

To track the evolution of polar plumes and related jets over their full observable lifetime.

CH Polar: Low

Dynamic

32 sec; Fixed

45 sec

1

1024x512

3 days

High cadence; 1 filter at a time; 2hours continuous; low compression rate

Program 1e

Program 1d (cool line list)

Large fov magnetograms; He 10830;

EUV imaging (TRACE, SDO)

Flare Onset

To find the locations and basic observable properties of flare initiation sites in the corona.

FL: High

Dynamic

0.1 sec; Fixed?

10 sec

1

1024x1024

24 hours total

1-2 filters; high cadence; use flare buffer

Program 3

Context + 1b

Large fov magnetograms; large fov H-alpha

EUV imaging (TRACE, SDO); Stereo

Flare Topology

To determine the coronal configuration(s) that lead to flares.

FL: Highest

Topology

1 sec/ 4sec/ 8 sec; Fixed

30 sec

2

1024x1024

24 hours total

2-3 filters; long & short exposures; use flare buffer

Program 3

Context + 1b

Large fov magnetograms; large fov H-alpha

EUV imaging (TRACE, SDO); Stereo

CME Acceleration

To measure the eruption speeds of CMEs as they first develop and leave the solar surface.

FL Limb: Highest

Dynamic

0.1 sec; Fixed

10 sec

2

2048x2048

24 hours total

2 filters; high cadence; use flare buffer

Program 3

Context + 3

Large fov magnetograms; large fov H-alpha

EUV imaging (TRACE, SDO); Stereo

Current Sheet Inflows

To locate and measure the properties of inflows in flare current sheets in the corona related to flares.

FL Limb: High

Dynamic

32 sec; Fixed

45 sec

1

2048x2048

24 hours total

1 filter; high cadence; flare response; long exp

Program 3

Context + 3

Large fov magnetograms; large fov H-alpha

EUV imaging (TRACE, SDO); Stereo

Supra-arcade downflows

To locate and measure the properties of supra-arcade downflows in flares.

FL Limb: Medium

Dynamic

0.1 sec; Fixed

10 sec

1

1024x1024

48 hours total

High cadence; 1 filter; 2 hours continuous; large FOV; moderate resolution; CMD > 45 degrees

Program 1c

Context + 1b

EUV imaging (TRACE, SDO)

Arcade fan formation/oscillation

To determine how and when fans form and measure their oscillations.

FL Limb: Medium

Energetics

0.1 sec; Fixed

10 sec

2

1024x1024

48 hours total

High cadence; 2 filters; large FOV; moderate resolution

Program 1c

Context + 1b

EUV imaging (TRACE, SDO)