HMI Science Data Measurements.
The data observing sequences that are used as input for
analyses are described here as a number of observation types. The Observation Types that support the
various science objectives are shown in the HMI_Objectives-Data_table. The Observation Types are
described here.
NOTE THESE
PAGES ARE STILL UNDER REVIEW
Observation Type HS-1
Global HS synoptic uses typically 72-day intervals. Repeated intervals are needed to follow solar variations with changes in solar activity. Loss of a few intervals in a three year span would still yield important results to extend the SOHO/MDI results into the next cycle. If GONG continues into the SDO mission years these observations have a somewhat lower priority since higher-noise but still very useful data can be obtained with GONG. In the past seven years GONG has (in 36-day intervals) coverage in the range of 70 to 85% (of the minutes). MDI has typically 96-97% coverage except of course for the large gaps. For low-degree (less than l=120) modes we believe most of the noise difference results from coverage completeness. We believe that coverage less than ninety something percent results in noticeable noise, probably the limit is about 90. We believe that solar noise is such that the noise in the frequency fits with coverage between about 95% and 100% is indistinguishable. Thus 95% is a good place to be sure that we are limited by solar noise rather than noise from data gaps. Where there are gaps we have found that random times of random sizes is least damaging. Gap filling methods can recover most of the signal when the gap is less than 10% of the surrounding spans of more complete data.
Observation Type Table Entry
|
Type |
Observing Sequence Needed |
Observables |
Planned Span of Observations |
Planned Number of Observations (percent coverage) |
Minimum Span of Observations |
Minimum Number of Observations (percent coverage) |
Minimum Image resolution |
Notes |
|
HS-1 |
OS-1 |
fd_V, fd_Ic |
5-years |
25 (100%) |
3-years |
12 (80%) |
2” |
Global structure and rotation |
Observing Sequence Type Table Entry
|
Observing Sequence Type |
Nominal Interval |
Completeness in interval |
Max harmless gap |
Optimum Gap distribution |
Notes |
|
OS-1 |
72d |
95% |
90s |
random |
|
Observation Type HS-2
Global Scale Local Method Helioseismology. HS-2. This type of observation supports measurement of deep-in-the-Sun flows and possibly fields. The method uses time-distance techniques to probe the conditions in the vicinity of the tachocline and bottom of the convection zone. This is about 200Mm deep. The end-points of acoustic rays that turn at this depth are about 700Mm apart, i.e. about a solar radius. This means that only a narrow range of longitude or latitude from disk center can be probed. With end points about 60 degrees apart and limiting data to about 75 degrees from disk center (0.96R where projection factor is about 4) the distance from disk center at the turning point is at most about 45 degrees. A “point” could then be tracked for 90 degrees or about 6 days. Doppler noise near the limb may restrict the range to +-60 degrees (0.87R, factor of 2 in projection) giving a 60 degree or 4 day maximum observing sequence. Experiments have shown useful S/N for one day sequences .Due to the wavelength of waves at the tachocline (c. 70Mm) the maximum resolution achievable is about 10 degrees. Thus about 5 resolution elements are detectable for each day-long sequence and 36 elements covers a rotation. This means the minimum requirement is 8 one-day sequences per month with at most 4-day gaps.
|
Type |
Observing Sequence Needed |
Observables |
Planned Span of Observations |
Planned Number of Observations (percent coverage) |
Minimum Span of Observations |
Minimum Number of Observations (percent coverage) |
Minimum Image resolution |
Notes |
|
HS-2 |
OS-2 |
fd_V |
5-years |
1800 (98%) allows 5 lost days/yr |
3-years |
300 with max gap of 4 days (25%) |
2” |
Tachocline structure from time-distance |
Observing Sequence Type Table Entry
|
Observing Sequence Type |
Nominal Interval |
Completeness in interval |
Max harmless gap |
Optimum Gap distribution |
Notes |
|
OS-2 |
24h |
85% |
90s |
bunched |
|
Observation Type HS-3
Sub-Surface “Weather” – SSW. This type of observation supports both Time-Distance and Ring type analyses (as well as holographic techniques). The goal is to study the region from the surface to 30Mm in detail and watch global and AR scale flows as they evolve. Sequences of a day are tracked in data cubes of typically 15-degrees or 7.5 degrees (perhaps 5 degrees with HMI). The Sun’s disk is tiled with overlapping tracked cubes and flow analysis is performed on each cube. MDI has shown changes on day time scales with larger scales persistent for rotations (or years in case of zonal flows a.k.a. torsional oscillations). MDI has only allowed one 2-rotation sequence per year. This is not sufficient to determine the persistence or nature of evolution of active region scale or even radius-scale flows. We believe a minimum of three contiguous rotations at least once each six months would yield important data on these flows. We should sample over the full rising part of the cycle – i.e. from min to max. The base plan is for continual mapping. One important component of large scale solar flows are the meridional or poleward flows. They have typical amplitudes of several m/s. We should be able to detect real variations down to c. 1 m/s. To avoid leakage of the 2 km/s solar rotation signal into the meridional signal we must know the roll orientation to better than 2 arc-min.
|
Type |
Observing Sequence Needed |
Observables |
Planned Span of Observations |
Planned Number of Observations (percent coverage) |
Minimum Span of Observations |
Minimum Number of Observations (percent coverage) |
Minimum Image resolution |
Notes |
|
HS-3 |
OS-3 |
fd_V |
5-years |
20 (100%) |
Min to max |
6 – one 3-rotation sequence each 6 months |
2” |
Large scale subsurface “weather” |
Observing Sequence Type Table Entry
|
Observing Sequence Type |
Nominal Interval |
Completeness in interval |
Max harmless gap |
Optimum Gap distribution |
Notes |
|
OS-3 |
90d |
95% |
90s |
random |
|
Observation Type HS-4
Active Longitude Studies. This observation type will provide data for the examination of the source of active zones or longitudes or complexes of activity. We know a good deal statistically about the clumpiness of activity but do not know of any internal cause for such clumping. This study will use techniques nearly identical to HS-3 except that longer contiguous spans are required. We believe we need at least 4-rotation spans of synoptic maps of sub-surface flows. Both Ring and Time-Distance analyses will be applied. Time-Distance prefers clumped gaps and Rings prefer random gaps.
|
Type |
Observing Sequence Needed |
Observables |
Planned Span of Observations |
Planned Number of Observations (percent coverage) |
Minimum Span of Observations |
Minimum Number of Observations (percent coverage) |
Minimum Image resolution |
Notes |
|
HS-4 |
OS-4 |
fd_V |
5-years |
15 (100%) |
3-years |
5 four-rotation sequences (55%) |
2” |
Active Longitudes |
Observing Sequence Type Table Entry
|
Observing Sequence Type |
Nominal Interval |
Completeness in interval |
Max harmless gap |
Optimum Gap distribution |
Notes |
|
OS-4 |
120d |
95% |
90s |
random |
|
Observation Type HS-5
Active Region Studies. This observation type produces data to allow study of flows, thermal, and field structure beneath active regions. Both Time-Distance and Holographic methods will be used. Since the details in the near surface layers are important the highest resolution data will be needed. The wavelength of acoustic waves near the surface is about 2Mm and this sets a natural resolution target. Active regions have lifetimes of weeks to months. If data is used to about 0.93 R then a 1Mm pixel subtends 0.5”. This gives a 10-day span of coverage. 12-days coverage with 0.5” pixels corresponds to 2Mm pixels with data used out to 0.98R. We would hope to obtain clean data for 10-day spans with analyses extended to 12-day spans with allowances for lower resolution at the ends. This means we can observe 20-50% of the lifetime of many active regions with full coverage of many short lived small regions. With this coverage we should be able to determine the flow-evolution from prior to eruption to post-visibility for small, typical, and a few large regions. We estimate that a sample of 100 regions tracked for 12-days each will yield at least 10 large region segments and we consider this to be a minimum requirement for this study. The baseline plan calls for tracking all active regions with NOAA identification. 100 regions can be captured in about 2.5 years starting at minimum or in less than six months near a typical maximum of activity. Since Time-Distance methods will be used gaps should be clumped into as few sub-intervals as possible. Ring type analyses do not give enough resolution for these studies.
|
Type |
Observing Sequence Needed |
Observables |
Planned Span of Observations |
Planned Number of Observations (percent coverage) |
Minimum Span of Observations |
Minimum Number of Observations (percent coverage) |
Minimum Image resolution |
Notes |
|
HS-5 |
OS-5 |
fd_V |
5-years |
100% |
2.5-years starting at min or 1 year at max |
100 regions |
2” |
Active Regions, Multiple regions concurrently |
Observing Sequence Type Table Entry
|
Observing Sequence Type |
Nominal Interval |
Completeness in interval |
Max harmless gap |
Optimum Gap distribution |
Notes |
|
OS-5 |
12d |
95% |
90s |
clumped |
|
Observation Type MAG-3
FACTS:
Nature of emerging magnetic flux: emerging of active regions; emerging magnetic flux within active
regions.
Observation of emerging magnetic flux: quickly emerge firstly (in the first 30 minutes), slow down in the coming 6 hours, and stop
after 10 hours; strong transverse component of magnetic field; downflows seen at footpints; flux
emerging within active regions often associated with flaring activity which is
limited to the procedure of emerging; whether emerging of active regions
causing eruption of nearby filaments depends on orientations of newly active regions
and background field (favor for reconnection).
Tasks: process of emergence
of magnetic flux within active regions; emerging of active regions (structure
of emerging magnetic field – Omega or U loops, energy buildup, and adjustment
of magnetic configuration by rotation, motion to follow Hale law with vector
and line-of-sight magnetograms, brightness and EUV images); structure of
emerging flux regions (structure & topology of magnetic field inferred and
computed by vector data, EUV observation, and coronal field extrapolation);
interaction of newly emerging flux and pre-existed field (both in small-scale
and large-scale) in order to understand its role for flare, eruption of
filaments, and/or CMEs; formation, structure, stability of filaments: (1) formation
(as short as 15 min, reappearance after eruption in one hour or less, test
scenarios of shear motion, reconnection, twisted-already before emerging by
using vector field data, brightness images and EUV images); (2) magnetic
configuration (structure & topology from vector field data & EUV data);(3)
stability (kink instability: buildup of twist by shear motion or by merging of
newly emerged, twisted-already fluxes, based on vector data, brightness &
EUV images).
REQUIREMENTS:
Samples: more than 5
examples for emerging of active regions, emerging flux regions within active
regions, emerging of active regions near filaments (within 20 degree).
Observations: vector
magnetic field (accuracy for transverse component and azimuth angle is of high priority;
10 min cadence; 2 arcsec resolution); line-of-sight
magnetograms (1 min cadence; 2 arcsec resolution; for
detecting emerging and evolution of magnetic flux such as motion, cancellation,
etc.); brightness images (1 min cadence for LCT); EUV (temporal, spatial
resolution is of priority, no worse than 10 min cadence, 2 arcsec
resolution to discern structure and behavior of emerging for magnetic flux,
longer than 1 hour duration); coronagraph images( temporal resolution is of
priority- no worse than 10 minutes for inner coronal images; longer than 1 hour
interval).
Calculation: coronal
magnetic extrapolation (10 minutes cadence); coronal and solar wind models (60
minutes cadence).
For other magnetic field observation types, see the “green” text in Magnetic_Objectives
These items will be incorporated into this document soon (