The geomagnetic field was at quiet to unsettled levels. Solar wind speed at SOHO ranged between 378 and 506 km/sec, averaging 440 km/sec (+17 km/sec compared to the previous day). A weak CME appears to have reached SOLAR-1 at 02:24 UT on September 14, at that time a sudden increase in solar wind speed, density and the total IMF field was recorded. The high latitude magnetometer at Andenes was at quiet to active levels. The above 10 MeV proton flux was at background levels all day.
Solar flux density measured at 17h UT on 2.8 GHz was 106.9 - decreasing 17.5 over the previous solar rotation. The measurement at 20h UT was flare enhanced (caused by a long duration filament eruption in the southwest quadrant peaking at 19:45 UT), and will therefore be replaced by the measurement at 17h UT.
The 365 day average solar flux at 1 AU was 135.68 (183 days ago). The 81 day average solar flux at 1 AU was 130.3 (41 days ago, this is 38.7% 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 6 (STAR Ap - based on the average of three hour interval ap indices: 5.8). Three hour interval K indices: 12222111 (planetary), 12332312 (Boulder), 34312211 (Andenes).
The background x-ray flux is at the class B3 level (GOES 19).
At the time of counting spots (see image time), spots were observed in 10 active regions using 2K resolution (SN: 149) and in 9 active regions using 1K resolution (SN: 114) SDO/HMI images.
AR 14524 [N12W66] decayed slowly and quietly.
AR 14525 [N11W53] decayed slowly and quietly and could soon become
spotless again.
AR 14527 [N03W45] was quiet with sings that the large penumbra could
be fragmenting into smaller penumbrae.
AR 14528 [S11W29] was quiet and stable.
AR 14529 [N12W28] has many tiny spots and was quiet.
AR 14530 [N20W58] decayed slowly and quietly.
Spotted regions not observed (or interpreted
differently) by SWPC/USAF:
AR S12353 [N11W48] decayed slowly and quietly
and could soon become spotless.
AR S12356 [N06W07] was quiet and stable.
AR S12360 [S11E16] was quiet and stable.
New AR S12361 [S10E50] emerged with tiny spots.
A long duration C1.4 event peaked at 19:45 UT during a filament eruption in the southwest quadrant. A faint partial halo CME was observed after this event.
C2+ flares
| Magnitude | Peak time (UT) | Location | Source | Recorded by | Comment |
September 11-12: No obviously Earth directed CMEs were observed in
available coronagraph imagery.
September 13: A faint partial halo CME was observed after a filament
eruption in the southwest quadrant peaking at 19:45 UT. The CME may have
Earth directed components and could reach Earth on September 16 or 17.
[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 negative polarity southern hemisphere coronal hole (CH1398) will be Earth facing on September 10-14. A recurrent negative polarity northern hemisphere coronal hole (CH1399) will rotate across the central meridian on September 12-14.
The geomagnetic field is expected to be at quiet to minor storm levels on September 13-17 due to effects associated with CH1398 and CH1399.
| 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 | ||||||||||
| 14521 | 2026.08.30 2026.08.31 |
1 | 3 | N09W93 | 0020 | HSX | BXO |
 |
 |
was AR S12327 area: 0010 location: N11W80 |
|
| 14523 | 2026.08.31 | N10W84 | interpretational mistake by SWPC/USAF. Obviously the trailing spots of AR 14521 | ||||||||
| 14524 | 2026.09.02 2026.09.02 |
1 | 2 | 1 | N12W54 | 0020 | HRX | HRX |
 |
 |
was AR S12334 location: N12W52 |
| 14526 | 2026.09.03 2026.09.04 |
S02W44 |
was AR S12338 location: S02W22 |
||||||||
| 14527 | 2026.09.03 2026.09.04 |
3 | 10 | 3 | N04W33 | 0200 | HSX | CKO |
 |
 |
was AR S12339 area: 0320 location: N03W32 |
| 14525 | 2026.09.03 2026.09.04 |
1 | 6 | 1 | N11W38 | 0010 | AXX | CRO |
 |
was AR S12340 location: N11W40 |
|
| S12344 | 2026.09.04 | S18W37 | |||||||||
| S12345 | 2026.09.04 | S12W34 | |||||||||
| 14529 | 2026.09.05 2026.09.06 |
3 | 13 | 7 | N12W18 | 0060 | CAO | HRX |
 |
 |
was AR S12346 area: 0030 location: N12W15 |
| 14528 | 2026.09.05 2026.09.06 |
1 | 9 | 3 | S11W17 | 0100 | HSX | CSO |
 |
 |
area: 0230 location: S11W15 |
| 14530 | 2026.09.06 | 7 | 8 | 4 | N19W49 | 0030 | DAO | CRO |
 |
 |
was AR S12350 location: N19W47 |
| S12353 | 2026.09.09 | 8 | 3 | N11W34 | 0030 | BXO |
 |
 |
ref. AR 12525 | ||
| S12354 | 2026.09.09 | S10E09 | |||||||||
| S12355 | 2026.09.09 | S22W36 |
 |
||||||||
| S12356 | 2026.09.10 | 6 | 1 | N07E05 | 0010 | BXO |
 |
||||
| S12357 | 2026.09.12 | 1 | 1 | N04E27 | 0005 | HRX |
 |
||||
| S12358 | 2026.09.12 | 5 | S27E31 | 0007 | BXO |
 |
|||||
| S12359 | 2026.09.12 | 2 | N18E55 | 0003 | AXX |
 |
|||||
| S12360 | 2026.09.12 | 4 | S11E35 | 0005 | AXX |
 |
|||||
| Total spot count: | 17 | 77 | 24 | ||||||||
| Sunspot number: | 87 | 207 | 114 | (total spot count + 10 * number of spotted regions) | |||||||
| Weighted SN: | 45 | 107 | 54 | (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): | 96 | 114 | 91 | ||||||||
| 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 |
| 2025.06 | 131.3 | 135.4 | 114.6 | 124.7 (-3.9) | 21.43 |
| 2025.07 | 137.8 | 142.3 | 125.9 | 122.5 (-2.2) | 11.80 |
| 2025.08 | 154.9 | 158.7 | 133.7 | 118.4 (-4.1) | 9.97 |
| 2025.09 | 154.4 | 156.0 | 129.7 | 113.1 (-5.3) | 14.02 |
| 2025.10 | 139.5 | 138.6 | 114.6 | 108.5 (-4.6) | 15.64 |
| 2025.11 | 140.3 | 137.3 | 91.7 | 106.9 (-1.6) | 21.01 |
| 2025.12 | 160.8 | 155.8 | 124.0 | 107.0 (-0.1) | 13.35 |
| 2026.01 | 148.7 | 144.0 | 115.0 | 104.2 (-2.8) | 22.47 |
| 2026.02 | 136.4 | 133.1 | 77.4 | 99.8 (-4.4) | 12.88 |
| 2026.03 | 131.0 | 129.7 | 86.6 | (94.7 projected, -5.1) | 15.44 |
| 2026.04 | 120.0 | 120.9 | 79.3 | (90.8 projected, -3.9) | 12.10 |
| 2026.05 | 125.4 | 128.2 | 101.4 | (89.6 projected, -1.2) | 9.80 |
| 2026.06 | 137.9 | 142.2 | 94.3 | (87.4 projected, -2.2) | 9.57 |
| 2026.07 | 134.7 | 139.0 | 78.1 | (82.9 projected, -4.5) | 10.16 |
| 2026.08 | 116.1 | 119.0 | 76.0 | (80.7 projected, -2.2) | 8.67 |
| 2026.09 | 108.5 (1) | 32.2 (2A) / 80.6 (2B) / 88.1 (2C) | (79.8 projected, -0.9) | (8.8) | |
| 2026.10 | (77.7 projected, -2.1) | ||||
| 2026.11 | (74.9 projected, -2.8) | ||||
| 2026.12 | (71.7 projected, -3.2) | ||||
| 2027.01 | (69.3 projected, -2.4) | ||||
| 2027.02 | (67.5 projected, -1.8) | ||||
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.
