Tracked Active Region Patches for MDI and HMI

Tracked Active Region Patches for MDI and HMI
Poster
#123.52
AAS
SPD
2014
Michael Turmon (JPL/Caltech); J. Todd Hoeksema, Monica Bobra (Stanford University)
Synoptic 2001 M-TARPs (lines mark month boundaries)
Summary
Methodology: Finding Active Regions
We are developing complementary tracked active region (AR) data
products from HMI and MDI images, indexed by region number and
by time. They are intended for subsetting individual ARs, for space
weather research, and to facilitate synoptic statistical studies of ARs.
HMI product
HARP = HMI Active Region Patch
Uses 720s (12m) HMI LOS magnetograms + intensitygrams
2300 regions and growing from 2010.05–present
Released on JSOC in 2011 as hmi.Mharp_720s
Also available: near-real-time, vector, & space weather products
• 
Together, the two data products cover May 1996 to the present, and
should eventually span two solar cycles.
We first compute a full-disk activity mask given input
magnetogram and intensity images taking spherical geometry
into account (Turmon et al. 2010).
• 
• 
MDI activity model relates to
HMI model by scaling by ~1.40
(Liu et al. 2012).
• 
Sample HMI mask (right)
shows typical
mask appearance.
• 
• 
Mask:
zoom
• 
• 
Kernel
at Limb
Kernel at
Disk Center
•  The tracked patch is often not a contiguous region. Use the bitmap
to determine what is part of the TARP.
•  Below: HARP 3457 (NOAA 11912) with a merge (between B and
HARPs:
Region(E)
Patches
C)HMI
andActive
breakup
causing a non-contiguous HARP shape.
Convolved with Template
Identified Groups
Some HMI HARPs enclose more activity within one
correspond to differently-numbered MDI TARPs).
HMI HARP 92 + MDI TARP 14113 at 2010.07.25 19:12:00 TAI
MDI TARP Pixels = 8601, MDI Active Pixels = 1320
HMI HARP 226 + MDI TARP 14242 at 2010.10.26 19:12:00 TAI
MDI TARP Pixels = 7192, MDI Active Pixels = 1193
50
150
A
B
C
D
E
2013.12.01
00:00 TAI
2013.12.04
00:00 TAI
2013.12.05
00:00 TAI
2013.12.09
00:00 TAI
2013.12.14
00:00 TAI
Ndef = 0
Ndef = 35638
N/A
Nnrt = 22919
100
200
300
400
500
600
700
800
900
1000
6.2. Movies
In the HARP, outside M-TARP
1100
150
HMI HARP 211 + MDI TARP 14226 at 2010.10.15 00:00:00 TAI
MDI TARP Pixels = 9358, MDI Active Pixels = 776
20
350
400
450
MDI−HMI Match OK
100
200
• 
No MDI or HMI match
300
400
500
600
700
800
900
1000
100
1100
200
300
400
500
2.5
2
1.5
1
0.5
5
x 10
HMI HARP 115 + MDI TARP 14136 at 2010.08.09 20:48:00 TAI
MDI TARP Pixels = 10125, MDI Active Pixels = 810
AREA: HMI HARP 86 + MDI TARP 14105
with HEK
6
150
200
2100
2101
2102
2103
250
200
250
Carrington Rotation Number
350
300
400
350
Some extra HARPs are found due to enhanced spatial/temporal
resolution of HMI. With current settings, some extra M-TARPs are
found due to grouping (see also next panel).
400
500
450
100
200
300
400
500
600
700
200
300
400
500
600
700
800
500
100
HMI HARP 185 + MDI TARP 14198 at 2010.09.23 20:48:00 TAI
MDI TARP Pixels = 8542, MDI Active Pixels = 762
200
300
400
500
600
22
20
x 10
800
900
NPIX: HMI HARP 187 + MDI TARP 14205
4
2
100
150
100
150
150
200
200
200
250
250
250
10.03
350
400
350
200
300
400
500
600
700
800
References
100
200
300
400
500
600
700
800
900
1000
09.26
MTOT: HMI HARP 187 + MDI TARP 14205
100
200
300
400
500
600
700
800
900
10.03
AREA ACR: HMI HARP 187 + MDI TARP 14205
10.03
5
x 10
10.03
MNET: HMI HARP 187 + MDI TARP 14205
5
0
10.03
−5
MMEAN: HMI HARP 187 + MDI TARP 14205
350
300
100
09.26
x 10
09.26
1000
800
600
400
200
09.26
10.03
LAT FWT: HMI HARP 187 + MDI TARP 14205
21.5
21
20.5
20
19.5
60
40
20
0
−20
300
NACR: HMI HARP 187 + MDI TARP 14205
1
09.26
300
x 10
0.5
4000
14
12
10
8
6
4
2
50
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
1.5
6
HMI HARP 175 + MDI TARP 14187 at 2010.09.17 14:24:00 TAI
MDI TARP Pixels = 12522, MDI Active Pixels = 1412
100
Improve MDI data product before an expected August 2014 release:
•  Better suppression of extraneous patches due to energetic particles.
•  Improved correspondence of MDI TARPs to HMI HARPs.
•  Identify sunspots within the activity mask.
Planned enhancements of HARP product: synoptic maps; gap filling.
For more on related space weather products, see Bobra et al. 2014.
50
HMI HARP 187 + MDI TARP 14205 at 2010.09.29 08:00:00 TAI
MDI TARP Pixels = 8866, MDI Active Pixels = 1329
700
50
Status and Plans
LAT FWT: HMI HARP 86 + MDI TARP 14105
2000
100
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
24
6000
50
These results are consistent with the good MDI/HMI agreement
found by Liu et al. (2012), especially for high LOS B.
−1
AREA: HMI HARP 187 + MDI TARP 14205
500
450
0
MMEAN: HMI HARP 86 + MDI TARP 14105
09.26
450
350
MNET: HMI HARP 86 + MDI TARP 14105
1
4
250
300
400
6
The definitive HARP processing groups each identified region according to its
complete life history, including its growth and interactions with other regions.
This omniscient view means that each definitive HARP is self-consistent and
HMI HARP
and MDI
TARP 14205with use cases like
has the most accurate calibration,
but it187
is also
incompatible
forecasting. We developed an analogous near-real-time (NRT) data product that
uses only retrospective data, and therefore can be computed immediately upon
receipt of data. However, because of the inferior quality of the NRT data (detailed
below), we do not recommend use of the NRT HARPs except for forecasting,
Ripple:
development of forecasting tools, and similar purposes.
In particular, if definitive
Hoeksema
al. be preferred, and if it does not
data exists for a given time range, it is vastlyet2014
to
yet exist due to processing lag, it is almost certainly better to wait for it to
appear.
MJT: Move some of the below paragraph to ”extent determination” above
We briefly describe the interaction of region time history with HARP geometry. The geometry of each definitive HARP is determined only after the
corresponding region has left the visible disk, or dissipated while being observed
on the disk. So, as explained in sec. 5.1,[email protected]
the rectangular bounding box of a [email protected]
tive HARP on the CCD encloses the fixed
heliographic region that encompasses
14
12
10
8
6
4
2
300
NACR: HMI HARP 86 + MDI TARP 14105
AREA ACR: HMI HARP 86 + MDI TARP 14105
x 10
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
150
2099
MTOT: HMI HARP 86 + MDI TARP 14105
0
100
150
0.070%
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
50
200
=
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
x 10
x 10
1200
1000
800
600
400
200
5
100
100
0.047%
4
2.5
2
1.5
1
0.5
7. NRT versus Definitive HARPs
50
−40
NPIX: HMI HARP 86 + MDI TARP 14105
15
HMI HARP 86 + MDI TARP 14105 at 2010.07.14 22:24:00 TAI
MDI TARP Pixels = 15672, MDI Active Pixels = 1646
HMI HARP 104 + MDI TARP 14127 at 2010.08.02 04:48:00 TAI
MDI TARP Pixels = 8138, MDI Active Pixels = 813
50
=
10000
8000
6000
4000
2000
100
−30
0.036%
10
600
More typically, as below, the HARP and the M-TARP coincide well.
−20
=
07.10 07.11 07.12 07.13 07.14 07.15 07.16 07.17 07.18 07.19 07.20
Active in HARP & M-TARP
400
HARP (HMI)
35.7%
and Stills
Active in HARP, not in M-TARP
6.4. Integration
350
300
MDI TARP
Ndef = 20055
HMI HARP 86 and MDI TARP 14105
Active in M-TARP, not in HARP
300
250
10
Ndef = 167634
6.3. Relationship to SHARPs
250
150
200
=
HARP & M-TARP coincide
200
50
100
Ndef = 75500
Nnrt = 75473
Nnrt = 167556
Nnrt = 20041
For each HARP/M-TARP
at each
time, we compute:
In the M-TARP, outside HARP
250
300
MDI vs. HMI Summary Statistics
NPIX
#pixels
in HARP
NACR
= #active
NPIX)
Figure 6. Definitive
and =
NRT
HARPs
versus time.
The top
row of pixels
images(≤
shows
definitive
= HARP
(µH) are:AREA
ACRemergence),
= active area
(≤ AREA)
HARPs; bottom rowAREA
is NRT
HARPs.area
Columns
A (before
B (before
merge),
HARP (blue blobs below
C (after merge), D (largest
E (decay).
The
same =
portion
the solar disk is shown
MTOT =extent),
∑HARP abs(B
MNET
∑HARP of
BLOS
LOS)
in each upper/lowerMMEAN
image pair.
Bottom rows are pixel
counts= (within
the red latitude
shape) at the
= MTOT/NPIX
LAT FWT
flux-weighted
Color Key
given time, and the Below,
final row
the percent
di↵erence.
HARPs
correspond
MDIispixel
counts scaled
up byThese
4x4; MDI
flux scaled
down to
by NOAA
1.40
AR 11912, whose center is shown as a blue cross.
to account for known MDI-HMI calibration (Liu et al. 2012).
Outside the HARP & M-TARP
50
200
30
Latitude (deg.)
Solve linear assignment
problem to match A up to B:
For the 2010 overlap, we overlaid the nine largest MDI TARPs over the HMIN/A
HARPs, projecting the MDI TARPs into the HMI coordinates by image WCS.
100
2098
A
B
•  Coping with the consequences of merges adds complexity to the
implementation. This complexity is hidden in the final data product.
MDI TARP vs. HMI HARP Region Boundaries
Centroid of MDI-TARPs and HMI HARPs
Synoptic: May 2010 – October 2010
2097
After
•  Tracks are first identified using past and current data. Thus,
growing regions may merge in later appearances.
100
2096
Before
2002 Sep. 02, 11:11 TAI
We used the ~140 ARs in the May–October 2010 overlap to check
correspondence between MDI TARPs and HMI HARPs.
Comparing location and size, we found 130 matching regions (in
green) and ~15 misses (in gray) of each type (TARP present but no
HARP, and v/v).
−10
Compute the overlap area
D(a,b) between extrapolated
track (via latitude-dependent
motion) and new region.
Merging Tracks and Complex ARs
We use a matched filter approach
with an elongated Gaussian kernel of
FWHM ~50x25Mm (~40x20 MDI pixels)
at disk center.
MDI Mask
MDI vs. HMI Region Correspondence
0
• 
where P is a permutation matrix giving the B-to-A mapping.
Group pixel-scale activity from
masks into NOAA AR-scale regions
Sponsored by NASA’s Heliophysics HDEE Program and SDO.
40
Chain single regions together to make a track.
• 
Mask:
2011/02/14 12:00
Active Region Grouping
Large spatially-coherent regions are identified within line-of-sight
(LOS) magnetograms and intensitygrams, and tracked from image to
image, accounting for merges as regions grow. The data series
provide all geometric and heliographic information needed to locate
active patches in HMI, MDI and other solar data sets. For each
numbered AR, the data series defines at each time step a rectangular
CCD cut-out, and it provides a mask within the cut-out indicating the
active pixels within a regular, smoothly-evolving blob. Summary
keywords such as areas and integrated fluxes are included for each
appearance of the region.
• 
Bayesian approach trades off pixel-by-pixel agreement of the
mask to the data against spatial coherence of labels (a prior).
Mask Model and Example
MDI product
MDI-TARP = MDI Tracked Active Region Patch
Uses 96m MDI LOS magnetograms + intensitygrams
6200 regions from 1996.05–2010.10
Complete (see authors); 2014 release in MDI Resident Archive
Methodology: Active Region Tracking
09.26
J. T. Hoeksema et al., “The HMI Vector Magnetic Field Pipeline: Overview and Performance,” Solar Phys., March, 2014.
M. Bobra et al., “The HMI ... Pipeline: SHARPs – Space-weather HMI active region patches,” Solar Phys., April, 2014.
M. Turmon, J. T. Hoeksema, X. Sun, M. Bobra, “HARPs – Tracked active region patch data product from SDO/HMI,”
2012 AGU fall meeting, and “TARPs: Tracked Active Region Patches from SoHO/MDI,” 2013 AGU fall meeting.
M. Turmon, H. Jones, J. Pap, O. Malanushenko, “Statistical feature recognition for multidimensional solar imagery”,
Solar Phys., 262(2), 2010.
Y. Liu, J. T. Hoeksema, P. H. Scherrer, et al., “Comparison of line-of-sight magnetograms taken by SDO/HMI and SOHO/
MDI,” Solar Phys., 279(1), 2012.
H. Jones, G. Chapman, K. Harvey, J. Pap, D. Preminger, M. Turmon, S. Walton, “A comparison of feature
classification...”, Solar Phys., 248(2), 2007.
10.03
09.26
10.03
[email protected]
National Aeronautics
and Space Administration
Jet Propulsion Laboratory
California Institute of Technology
Pasadena, California
Copyright 2014. All rights reserved.
SOLA: harp-v0.tex; 12 May 2014; 10:06; p. 11