The geomagnetic field was at unsettled to active levels on March 24 under the influence of slowly weakening effects associated with CH1351. Solar wind speed at SOHO ranged between 506 and 668 km/sec (-55 km/sec compared to the previous day). What is likely the March 22 CME was observed arriving at ACE at 05:52 UT on March 25. The high latitude magnetometer at Andenes was at unsettled to major storm levels. The above 10 MeV proton flux was at background levels all day.
Solar flux density measured at 20h UT on 2.8 GHz was 128.3 - decreasing 1.5 over the previous solar rotation.
The 365 day average solar flux at 1 AU was 144.62 (183 days ago). The 81 day average solar flux at 1 AU was 133.7 (41 days ago, this is 40.9% of the total SC25 solar flux range from the max 81 day average peak on September 4, 2024 at 227.3 and an average 81 day flux of 69 at solar minimum). SC25 365d peak: 195.9 on October 13, 2024.
The Potsdam WDC planetary A index was 17 (STAR Ap - based on the average of three hour interval ap indices: 17.0). Three hour interval K indices: 34343333 (planetary), 34343332 (Boulder), 44433466 (Andenes).
The background x-ray flux is at the class B8 level (GOES 19).
At the time of counting spots (see image time), spots were observed in 9 active regions using 2K resolution (SN: 184) and in 8 active regions using 1K resolution (SN: 131) SDO/HMI images.
AR 14397 [N14W13] decayed slowly and quietly.
AR 14398 [S17W12] decayed slowly and was mostly quiet. C1 flares:
C1.0 @ 21:10 UT
AR 14399 [S16E40] decayed slowly and quietly.
AR 14400 [S12W52] decayed slowly and was mostly quiet.
AR 14401 [N25E37] developed further and has polarity intermixing. A
minor M class flare is possible.
AR 14402 [N19E48] decayed in the leading spot section and was mostly
quiet.
Spotted regions not observed (or interpreted
differently) by SWPC/USAF:
AR S11950 [N07E12] decayed slowly and quietly.
New AR S11952 [N16E80] rotated partly into view and produced the
largest flare of the day.
New AR S11953 [S24E22] was observed with tiny spots in an old
plage area.
C1.0 flares at 22:53 and 23:13 UT had their origin behind the northeast limb.
C2+ flares
| Magnitude | Peak time (UT) | Location | Source | Recorded by | Comment |
| C7.2 | 17:54 | S11952 | GOES18 | LDE | |
| C2.8 | 18:42 | 14400 | GOES18 | ||
| C2.3 | 21:56 | 14401 | GOES18 | ||
| C2.1 | 00:03 | 14400 | GOES18 | flare began at 23:52 UT |
March 23-24: No obviously Earth directed CMEs were observed in
available coronagraph imagery.
March 22: A partial halo CME was observed after a large filament
eruption in the southeastern quadrant. The eruption started at aproximately
15:45 UT to the south of AR 14398. The CME likely reached Earth after 06h UT
on March 25.
[Coronal
hole history (since October 2002)]
[Compare today's report to the situation one solar rotation ago:
28 days ago
27 days ago
26 days ago]
A recurrent trans equatorial negative polarity coronal hole (CH1351) was Earth facing on March 19-22. A recurrent northern hemisphere positive polarity coronal hole (CH1352) will likely rotate across the central meridian on March 25-26.
The geomagnetic field is expected to be at quiet to active levels on March 25-26 due to effects associated with CH1351 and the March 22 CME. Quiet to unsettled conditions are likely on March 27. Effects associated with CH1352 could cause quiet to minor storm levels on March 28-29.
| Coronal holes (1) | Coronal mass ejections (2) | M and X class flares (3) |
1) Effects from a coronal hole could
reach Earth within the next 5 days. When the high speed stream has arrived
the color changes to green.
2) Effects from a CME are likely to be observed at Earth within 96 hours.
3) There is a possibility of either M or X class flares within the next 48 hours.
Green: 0-30% probability, Yellow: 30-70% probability, Red: 70-100% probability.
(Click on image for 2K resolution).
4K resolution.
Compare to the previous day's image. 0.5K image
When available the active region map has a coronal hole polarity overlay where red (pink) is negative and blue is positive.
Data for all officially numbered solar regions according to the Solar Region Summary provided by NOAA/SWPC, all other regions are numbered sequentially as they emerge using the STAR spot number. Comments are my own, as is the STAR spot count (spots observed at or inside a few hours before midnight) and data for regions not numbered by SWPC or where SWPC has observed no spots. SWPC active region numbers in the table below and in the active region map above are the historic SWPC/USAF numbers. SWPC data considered to be not sufficiently precise (location, area, classification) are colored red.
| Active region | SWPC date numbered STAR detected |
Spot count | Location at midnight | Area | Classification | SDO / HMI 4K continuum image with magnetic polarity overlays |
Comment | ||||
|---|---|---|---|---|---|---|---|---|---|---|---|
| SWPC/ USAF |
STAR | SWPC | STAR | Current | Previous | ||||||
| 2K | 1K | ||||||||||
| 14392 | 2026.03.11 2026.03.11 |
2 | S17W90 | 0090 | CAO |
 |
was AR S11922 area: 0220 rotated out of view |
||||
| 14395 | 2026.03.14 2026.03.14 |
S06W87 |
was AR S11929 location: S05W78 |
||||||||
| 14396 | 2026.03.15 2026.03.15 |
N20W71 |
was AR S11932 location: N20W63 |
||||||||
| S11933 | 2026.03.17 | S26W21 | |||||||||
| 14397 | 2026.03.17 2026.03.18 |
5 | 7 | 4 | N15W12 | 0010 | BXO | CRO |
 |
 |
was AR S11934 area: 0020 location: N14W13 |
| S11935 | 2026.03.18 | S22W29 | |||||||||
| 14400 | 2026.03.19 2026.03.22 |
5 | 11 | 6 | S14W52 | 0080 | DAO | DRI |
 |
 |
was AR S11937 beta-gamma area: 0060 location: S12W52 |
| 14398 | 2026.03.20 2026.03.21 |
10 | 16 | 8 | S17W12 | 0040 | DAO | DRI |
 |
 |
was AR S11938 area: 0060 |
| S11940 | 2026.03.20 | S07W40 | |||||||||
| 14399 | 2026.03.21 2026.03.21 |
4 | 10 | 3 | S18E42 | 0170 | CAO | CKO |
 |
 |
was AR S11941 area: 0260 |
| 14401 | 2026.03.21 2026.03.22 |
15 | 33 | 23 | N25E38 | 0210 | EAI | EKI |
 |
 |
was AR S11942 area: 0500 location: N25E37 |
| 14402 | 2026.03.21 2026.03.22 |
2 | 8 | 5 | N17E45 | 0150 | DSO | DAO |
 |
 |
was AR S11943 area: 0230 location: N19E48 |
| S11944 | 2026.03.21 | S42W31 | |||||||||
| S11947 | 2026.03.22 | S18W41 | |||||||||
| S11950 | 2026.03.23 | 5 | 1 | N07E12 | 0007 | BXO |
 |
 |
|||
| S11951 | 2026.03.23 | S18W22 |
 |
||||||||
| S11952 | 2026.03.24 | 1 | 1 | N16E80 | 0230 | HAX |
 |
||||
| S11953 | 2026.03.24 | 3 | S24E22 | 0005 | AXX |
 |
|||||
| Total spot count: | 43 | 94 | 51 | ||||||||
| Sunspot number: | 113 | 184 | 131 | (total spot count + 10 * number of spotted regions) | |||||||
| Weighted SN: | 73 | 133 | 90 | (Sum of total spot count + classification weighting for each AR. Classification weighting: X=0, R=3, A/S=5, H/K=10) | |||||||
| Relative sunspot number (Wolf number): | 124 | 101 | 105 | ||||||||
| Month | Average solar flux | International sunspot number (WDC-SILSO) |
Smoothed sunspot number (4) | Average
ap (3) |
|
|---|---|---|---|---|---|
| Measured | 1 AU | ||||
| 2024.05 | 187.7 | 191.9 | 172.1 | 149.1 (+4.6) | 23.56 (SC25 peak) |
| 2024.08 | 246.1 (SC25 peak) |
252.2 | 216.0 (SC25 peak) | 156.8 (+1.8) | 15.96 |
| 2024.10 | 221.0 | 219.6 | 165.8 | 160.9 (+1.5) (SC25 solar max) | 18.99 |
| 2024.12 | 197.3 | 191.2 | 154.6 | 151.2 (-6.0) | 8.42 |
| 2025.01 | 190.3 | 184.2 | 137.0 | 146.2 (-5.0) | 13.17 |
| 2025.02 | 184.2 | 179.7 | 155.7 | 139.8 (-6.4) | 14.42 |
| 2025.03 | 163.7 | 162.1 | 134.2 | 135.9 (-3.9) | 15.96 |
| 2025.04 | 162.5 | 163.6 | 141.4 | 133.3 (-2.6) | 17.62 |
| 2025.05 | 135.3 | 138.3 | 78.5 | 128.6 (-4.7) | 17.26 |
| 2025.06 | 131.3 | 135.4 | 114.6 | 124.7 (-3.9) | 21.43 |
| 2025.07 | 137.8 | 142.3 | 125.9 | 122.4 (-2.3) | 11.80 |
| 2025.08 | 154.9 | 158.7 | 133.7 | 118.2 (-4.2) | 9.97 |
| 2025.09 | 154.4 | 156.0 | 129.7 | (113.5 projected, -4.7) | 14.02 |
| 2025.10 | 139.5 | 138.6 | 114.6 | (110.0 projected, -3.5) | 15.64 |
| 2025.11 | 140.3 | 137.3 | 91.7 | (108.3 projected, -1.7) | 21.01 |
| 2025.12 | 160.8 | 155.8 | 124.0 | (107.1 projected, -1.2) | 13.35 |
| 2026.01 | 148.7 | 144.0 | 112.6 | (103.2 projected, -3.9) | 22.47 |
| 2026.02 | 136.4 | 133.1 | 78.2 | (98.9 projected, -4.2) | 12.88 |
| 2026.03 | 125.0 (1) | 61.3 (2A) / 79.2 (2B) / 88.3 (2C) ISN
month to date average: 80 |
(94.3 projected, -4.6) | (17.1) | |
| 2026.04 | (90.4 projected, -3.9) | ||||
| 2026.05 | (89.2 projected, -1.2) | ||||
| 2026.06 | (87.1 projected, -2.1) | ||||
| 2026.07 | (82.7 projected, -4.4) | ||||
| 2026.08 | (80.5 projected, -2.2) | ||||
1) Running average based on the daily 20:00 UTC observed solar flux value
at 2800 MHz and any corrections applied to that measurement.
2A) Current impact on the monthly sunspot number based on the Boulder
(NOAA/SWPC) sunspot number (accumulated daily sunspots / month days).
2B) Boulder SN current month average to date.
2C) STAR SDO 1K Wolf number 27 day average.
3) Running average based on the quicklook and definitive Potsdam WDC ap
indices. Values in red
are based on the definitive international
GFZ Potsdam WDC ap
indices.
4) Source: WDC-SILSO, Royal Observatory
Of Belgium, Brussels
Solar activity appears to have exited the solar max phase as of February
2026 with a strong decrease in the number of sunspots observed. The northern
polar field has weakened considerably over the last months, and although
there is a chance the the field could recover over the next 1-2 years, there
is an increasing chance that solar cycle 26 will be very weak. The southern
polar field is not impressive either, however, a southern polar coronal hole
has formed early in 2026 and appears to be growing.
All 365 day smoothed sunspot numbers reached a maximum on October 11-12, 2024.
This became the peak of SC25 (365 day smoothed peaks: STAR 1K: 236.1, STAR 2K: 364.3, NOAA SN: 156.0, ISN: 163.9),
while the 365d
smoothed solar flux peaked on October 13, 2024, just 1.7% below the SC23
peak, and 62.6% above the SC24 peak.
--------------------------------------------------------------------------------------
This report has been prepared by Jan Alvestad. It is based on the analysis of data from whichever sources are available at the time the report is prepared. All time references are to Universal Time. Comments and suggestions are always welcome.
SDO images are courtesy of NASA/SDO and the AIA, EVE, and HMI science teams.
