The geomagnetic field was at quiet levels on March 31. Solar wind speed at ACE ranged between 356 and 515 km/sec. A weak solar wind shock was observed at ACE at 10:12 UT, most likely caused by the X1 flare on March 28. The high latitude magnetometer at Andenes recorded quiet to unsettled levels. The above 10 MeV proton flux reached event level briefly when the above solar wind shock was recorded. Later in the day proton levels increased further and was at 77 pfu at the end of the day. Early on April 1 levels increased further and 147 pfu was recorded at 04:20 UT.
Solar flux density measured at 20h UT on 2.8 GHz was 171.9 - increasing 11.4 over the previous solar rotation. (Centered 1 year average SF at 1 AU - 183 days ago: 194.35. In comparison SC24 peaked on June 28, 2014 at 145.50 while SC23 peaked on February 23, 2002 at 198.15. Current SC25 peak: 194.78 on September 18, 2024 (subtracting a baseline solar flux level of 65, this is +61.22% compared to the SC24 peak and -2.53% compared to the SC23 peak). The Potsdam WDC planetary A index was 5 (STAR Ap - based on the mean of three hour interval ap indices: 4.9). Three hour interval K indices: 12221111 (planetary), 12232421 (Boulder), 11122331 (Andenes).
The background x-ray flux is at the class C2 level (GOES 18).
At the time of counting spots (see image time), spots were observed in 13 active regions using 2K resolution (SN: 344) and in 9 active regions using 1K resolution (SN: 197) SDO/HMI images.
AR 14043 [N14W27] decayed slowly and was mostly
quiet. C1 flares: C1.8 @ 16:57, C1.9 @ 19:10 UT
AR 14044 [N20W04] decayed slowly and quietly.
AR 14045 [S14E23] decayed slowly and quietly.
AR 14046 [N05E31] decayed slowly and was mostly quiet. C1 flares:
C1.9 @ 14:03 UT
AR 14047 [S15W50] decayed slowly and quietly.
AR 14048 [S15E53] developed further gaining spots and area. The
region has major flare potential. C1 flares: C1.8 @ 13:53, C1.6 @ 14:46,
C1.6 @ 15:36, C1.8 @ 15:43, C1.9 @ 15:50, C1.9 @ 19:39, C1.7 @ 21:42 UT
New AR 14049 [S30E28] emerged on March 29 and was numbered 2 days
later by SWPC as the region developed further. C1 flares: C1.5 @ 06:53
Spotted regions not observed (or interpreted
differently) by SWPC/USAF:
S10933 [S15W16] was quiet and stable.
S10941 [S00W02] was quiet and stable.
S10946 [S03E00] was quiet and stable.
S10948 [N21E26] was quiet and stable.
New region S10949 [S18E13] emerged with tiny
spots.
New region S10950 [N05E09] emerged with a tiny spot.
C2+ flares
| Magnitude | Peak time (UT) | Location | Source | Recorded by | Comment |
| C6.5 | 00:06 | 14048 | GOES16 | ||
| C5.5 | 00:41 | 14048 | GOES16 | ||
| C3.4 | 00:57 | 14048 | GOES16 | ||
| C3.9 | 01:13 | 14048 | GOES16 | ||
| C2.9 | 01:50 | 14048 | GOES16 | ||
| C3.1 | 02:14 | 14048 | GOES16 | ||
| C8.9 | 02:35 | 14048 | GOES16 | ||
| C4.6 | 02:59 | 14048 | GOES16 | ||
| C5.8 | 03:17 | 14048 | GOES16 | ||
| C6.5 | 03:30 | 14048 | GOES16 | ||
| C5.3 | 03:40 | 14048 | GOES16 | ||
| C7.6 | 03:52 | 14046 | GOES16 | ||
| C2.9 | 04:37 | 14048 | GOES18 | ||
| C4.7 | 05:08 | 14048 | GOES18 | ||
| C3.7 | 05:15 | 14048 | GOES18 | ||
| C2.6 | 07:28 | 14048 | GOES16 | ||
| C2.4 | 07:41 | 14048 | GOES16 | ||
| C2.4 | 09:28 | 14048 | GOES16 | ||
| C3.1 | 10:07 | 14048 | GOES16 | ||
| M1.2 | 10:24 | 14048 | GOES16 | ||
| C4.4 | 12:08 | N04E41 | 14046 | GOES16 | |
| C2.5 | 12:40 | 14048 | GOES16 | ||
| C2.2 | 14:13 | S16E63 | 14048 | GOES16 | |
| C2.4 | 16:15 | 14048 | GOES16 | ||
| C4.4 | 16:37 | 14048 | GOES16 | ||
| C3.5 | 17:22 | 14048 | GOES16 | ||
| C4.1 | 17:42 | 14048 | GOES16 | ||
| C6.0 | 17:50 | S17E62 | 14048 | GOES16 | |
| C2.0 | 19:16 | 14043 | GOES16 | ||
| C2.0 | 20:25 | 14048 | GOES16 | ||
| C2.0 | 20:35 | 14048 | GOES16 | ||
| C2.7 | 20:50 | 14046 | GOES16 | ||
| C3.3 | 20:57 | 14046 | GOES16 | ||
| C2.6 | 21:48 | 14048 | GOES16 | ||
| C2.0 | 22:34 | 14049 | GOES16 | ||
| C2.0 | 22:44 | 14049 | GOES16 | ||
| C2.2 | 23:04 | 14048 | GOES16 | ||
| C3.3 | 23:45 | 14048 | GOES16 | ||
| C3.2 | 23:57 | 14048 | GOES16 |
March 29-31: No obviously Earth directed CMEs.
[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 (CH1281) will rotate across the central meridian on April 1.
Long distance low and medium frequency (below 2 MHz) propagation along paths north of due west over upper middle and high latitudes is poor. Propagation on long distance northeast-southwest paths is poor.
The geomagnetic field is expected to be at mostly quiet levels on April 1-3. A high speed stream associated with CH1281 could cause unsettled to minor storm levels on April 4-5.
| 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 | ||||||||||
| 14038 | 2025.03.20 2025.03.21 |
S15W78 |
was AR S10912 location: S13W73 |
||||||||
| 14039 | 2025.03.20 2025.03.21 |
N09W76 |
 |
was AR S10914 location: N11W67 |
|||||||
| 14040 | 2025.03.21 2025.03.22 |
S08W66 |
 |
was AR S10915 location: S08W55 |
|||||||
| 14041 | 2025.03.21 2025.03.22 |
N18W54 |
 |
was AR S10916 location: N20W56 |
|||||||
| 14042 | 2025.03.22 | S12W58 | the trailing spots of AR 14040 | ||||||||
| 14043 | 2025.03.23 2025.03.25 |
13 | 37 | 22 | N14W27 | 0120 | EAI | EAI |
 |
 |
was AR S10921 |
| S10926 | 2025.03.25 | N04W34 | |||||||||
| S10927 | 2025.03.25 | N16W39 | |||||||||
| 14044 | 2025.03.26 2025.03.27 |
9 | 20 | 9 | N20W04 | 0040 | DAO | DAO |
 |
 |
was AR S10929 area: 0080 |
| S10931 | 2025.03.26 | S23W05 | |||||||||
| 14045 | 2025.03.27 2025.03.27 |
4 | 21 | 11 | S15E23 | 0010 | AXX | BXO |
 |
 |
was AR S10932 location: S14E23 area: 0050 |
| S10933 | 2025.03.27 | 11 | 4 | S15W16 | 0020 | AXX |
 |
 |
|||
| 14046 | 2025.03.27 2025.03.28 |
9 | 16 | 8 | N05E31 | 0260 | DHO | CKO |
 |
 |
beta-gamma was AR S10935 area: 0480 |
| S10936 | 2025.03.27 | N19W40 |
 |
||||||||
| S10937 | 2025.03.27 | N08W49 | |||||||||
| 14047 | 2025.03.28 2025.03.28 |
10 | 15 | 9 | S16W50 | 0060 | DAO | DAO |
 |
 |
was AR S10939 area: 0090 |
| 14048 | 2025.03.28 2025.03.29 |
32 | 56 | 32 | S16E53 | 0440 | EKC | EKC |
 |
 |
beta-gamma was AR S10940 location: S15E53 area: 1410 |
| S10941 | 2025.03.28 | 2 | S00W02 | 0003 | BXO |
 |
|
||||
| S10942 | 2025.03.29 | N27E24 | |||||||||
| 14049 | 2025.03.29 2025.03.31 |
4 | 17 | 9 | S31E27 | 0020 | CRO | DRI |
 |
 |
beta-gamma was AR S10943 area: 0080 |
| S10944 | 2025.03.29 | S01W33 |
 |
||||||||
| S10946 | 2025.03.29 | 1 | S03E00 | 0001 | AXX |
 |
 |
||||
| S10948 | 2025.03.30 | 2 | N21E26 | 0002 | BXO |
 |
 |
||||
| S10949 | 2025.03.31 | 5 | 3 | S18E13 | 0020 | HRX |
 |
||||
| S10950 | 2025.03.31 | 1 | N05E09 | 0001 | AXX |
 |
|||||
| Total spot count: | 81 | 204 | 107 | ||||||||
| Sunspot number: | 151 | 344 | 197 | (total spot count + 10 * number of spotted regions) | |||||||
| Weighted SN: | 119 | 245 | 148 | (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): | 166 | 189 | 158 | ||||||||
| Month | Average solar flux | International sunspot number (WDC-SILSO) |
Smoothed sunspot number (4) | Average
ap (3) |
|
|---|---|---|---|---|---|
| Measured | 1 AU | ||||
| 2014.02 | 170.3 (cycle peak) |
166.3 | 146.1 (SC24 peak) | 110.5 | 10.70 |
| 2014.04 | 143.9 | 144.8 | 112.5 | 116.4 (SC24 solar max) | 7.88 |
| 2017.09 | 91.3 | 92.3 | 43.6 | 18.2 (-1.3) | 18.22 (SC24 peak) |
| 2019.11 | 70.2 | 68.7 | 0.5 | 2.0 (-0.6) (Solar minimum using 365d smoothing: November 17, 2019) |
4.19 |
| 2019.12 | 70.8 | 68.6 | 1.6 | 1.8 (-0.2) (ISN 13 months smoothed solar minimum) |
3.22 |
| 2023.10 | 142.8 | 141.9 | 99.9 | 124.8 (+0.8) | 8.16 |
| 2023.11 | 153.5 | 150.2 | 107.1 | 127.9 (+3.1) | 12.20 |
| 2023.12 | 151.1 | 146.4 | 113.5 | 129.5 (+1.6) | 9.60 |
| 2024.01 | 164.6 | 159.3 | 126.0 | 131.2 (+1.7) | 5.46 |
| 2024.02 | 172.5 | 168.3 | 123.0 | 136.9 (+5.7) | 5.31 |
| 2024.03 | 154.4 | 152.9 | 103.7 | 141.4 (+4.5) | 11.03 |
| 2024.04 | 161.3 | 162.6 | 137.0 | 144.5 (+3.1) | 9.69 |
| 2024.05 | 187.7 | 191.9 | 172.1 | 149.1 (+4.6) | 23.56 (SC25 peak) |
| 2024.06 | 184.3 | 190.2 | 164.1 | 152.7 (+3.6) | 10.24 |
| 2024.07 | 196.6 | 203.0 | 196.8 | 154.9 (+2.3) | 7.13 |
| 2024.08 | 246.1 (cycle peak) |
252.2 | 216.0 (SC25 peak) | 156.7 (+1.8) | 15.96 |
| 2024.09 | 195.7 | 197.8 | 141.1 | 159.3 (+1.6) | 15.36 |
| 2024.10 | 221.0 | 219.6 | 166.4 | (160.2 projected, +0.9) | 18.99 |
| 2024.11 | 199.6 | 195.3 | 152.5 | (157.6 projected, -2.6) | 9.33 |
| 2024.12 | 197.3 | 191.2 | 154.5 | (153.8 projected, -3.8) | 8.42 |
| 2025.01 | 190.3 | 184.2 | 137.0 | (148.3 projected, -5.5) | 13.17 |
| 2025.02 | 184.2 | 179.7 | 154.7 | (139.8 projected, -8.5) | 14.42 |
| 2025.03 | 163.7 | 162.1 | 134.2 | (133.4 projected, -6.4) | 16.4 |
| 2025.04 | (1) | (2A/2B) / 165.1 (2C) | (128.8 projected, -4.6) | () | |
| 2025.05 | (123.5 projected, -5.3) | ||||
| 2025.06 | (118.6 projected, -4.9) | ||||
| 2025.07 | (114.5 projected, -4.1) | ||||
| 2025.08 | (109.8 projected, -4.7) | ||||
| 2025.09 | (105.5 projected, -4.3) | ||||
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
Sunspot activity has been on a slowly decreasing trend since September 2024 (using the average solar flux over 3 solar rotations as a proxy). Currently all 365 days smoothed indices are still indicating that a peak occurred on October 12 or 13, 2024. Should sunspot activity decrease even further then there is a possibility that the peak may have taken place in September 2024. Any peak outside of September-October 2024 appears unlikely. The 365 days average solar flux is likely to max out ~2% below the peak of solar cycle 23. The maximum 365d smoothed solar flux of SC23 and SC25 are similar, however, sunspot numbers were significantly lower during SC25 compared to SC23.
--------------------------------------------------------------------------------------
This report has been prepared by Jan Alvestad. It is based on the analysis of data from whatever 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.
