The geomagnetic field was quiet to unsettled on March 25 under the lingering influence of a high speed stream from CH1069. The high latitude magnetometer at Andenes recorded quiet to active levels.
Solar flux density measured at 20h UT on 2.8 GHz was 112 - increasing 15.5 over the previous solar rotation. (Centered 1 year average SF at 1 AU - 183 days ago: 89.02). The Potsdam WDC planetary A index was 7 (STAR Ap - based on the mean of three hour interval ap indices: 7.4). Three hour interval K indices: 33122111 (planetary), 33332321 (Boulder), 44133332 (Andenes).
The background x-ray flux is at the class B4 level (GOES 16).
At the time of counting spots (see image time), spots were observed in 7 active regions using 2K resolution (SN: 136) and in 4 active regions using 1K resolution (SN: 65) SDO/HMI images.
Region 12974 [S18E27] displayed no significant change,
yet managed to produce an M1.4 flare.
Region 12975 [N12E31] decayed slowly and quietly. The easternmost
spots are now quite close to the leading spots of AR 12976 and some
interaction is possible.
Region 12976 [N15E47] was mostly quiet and could produce M class flares.
Spotted regions not observed (or interpreted
differently) by SWPC:
S7438 [N14E02] was quiet and stable.
New region S7448 [N17E19] emerged with tiny spots.
New region S7449 [S15E52] was observed with tiny spots in an
old plage area.
New region S7450 [S18W23] emerged near CH1070 with tiny spots.
C2+ flares:
| Magnitude | Peak time (UT) | Location | Source | Recorded by | Comment |
| C2.6 | 02:45 | 12976 | GOES16 | ||
| M1.4/1F | 05:26 | S21E36 | 12974 | GOES16 | LDE, CME, weak type II and IV radio sweeps |
March 23-24: No obviously Earth directed CMEs
were observed in available LASCO imagery.
March 25: A CME was observed after the M1.4 event in AR 12974. The
CME could reach Earth sometime between noon on March 27 and the early hours
of March 28.
[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 trans equatorial coronal hole (CH1070) was in an Earth facing position on March 23-25.
Long distance low and medium frequency (below 2 MHz) propagation along paths north of due west over upper middle and high latitudes is poor to fair. Propagation on long distance northeast-southwest paths is poor.
Quiet to minor storm conditions are likely on March 26-28 as a high speed stream from CH1070 becomes the dominant solar wind source. The March 25 CME could further increase the disturbance level on March 27 and 28, maybe reaching major storm levels.
| Coronal holes (1) | Coronal mass ejection (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 |
Magnetic (SDO) |
SWPC | STAR | Current | Previous | ||||||
| 2K | 1K | ||||||||||
| 12971 | 2022.03.15 2022.03.17 |
N16W67 | location: N18W60 | ||||||||
| 12972 | 2022.03.19 2022.03.19 |
S29W60 |
 |
location: S27W58 | |||||||
| 12973 | 2022.03.19 2022.03.20 |
N19W20 | |||||||||
| S7438 | 2022.03.19 | 4 | N14E02 | 0004 | AXX |
 |
 |
||||
| 12974 | 2022.03.21 2022.03.22 |
2 | 13 | 6 | S19E25 | 0030 | CRO | CRO |
 |
 |
area: 0050 |
| S7442 | 2022.03.21 | N19W25 | |||||||||
| S7443 | 2022.03.21 | S24E19 | |||||||||
| S7444 | 2022.03.21 | S29W54 | |||||||||
| 12975 | 2022.03.22 2022.03.23 |
5 | 13 | 5 | N12E39 | 0160 | ESO | EAO |
 |
 |
location: N12E31 area: 0080 SWPC location is way off |
| 12976 | 2022.03.22 2022.03.24 |
13 | 27 | 11 | N16E47 | 0450 | EHO | EHO |
 |
 |
location: N15E47 |
| S7448 | 2022.03.25 | 5 | 3 | N17E19 | 0015 | BXO |
 |
||||
| S7449 | 2022.03.25 | 2 | S15E52 | 0002 | AXX |
 |
|||||
| S7450 | 2022.03.25 | 2 | S18W23 | 0002 | BXO |
 |
|||||
| Total spot count: | 20 | 66 | 25 | ||||||||
| Sunspot number: | 50 | 136 | 65 | (total spot count + 10 * number of spotted regions) | |||||||
| Weighted SN: | 38 | 84 | 43 | (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): | 55 | 75 | 52 | ||||||||
| 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 (solar max) | 7.88 |
| 2017.09 | 91.3 | 92.3 | 43.6 | 18.2 (-1.3) | 18.22 (cycle 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 |
| 2020.08 | 71.6 | 73.4 | 7.5 | 9.5 (+0.5) | 5.68 |
| 2020.09 | 70.7 | 71.4 | 0.7 | 10.5 (+1.0) | 8.59 |
| 2020.10 | 74.6 | 74.2 | 14.6 | 11.9 (+1.4) | 6.13 |
| 2020.11 | 89.9 | 88.0 | 34.5 | 13.6 (+1.7) | 4.77 |
| 2020.12 | 86.9 | 84.2 | 23.1 | 15.3 (+1.7) | 4.72 |
| 2021.01 | 76.0 | 73.6 | 10.4 | 17.3 (+2.0) | 4.39 |
| 2021.02 | 74.3 | 72.4 | 8.2 | 19.0 (+1.7) | 9.50 |
| 2021.03 | 76.0 | 75.2 | 17.2 | 21.7 (+2.7) | 10.17 |
| 2021.04 | 75.9 | 76.4 | 24.5 | 24.8 (+3.1) | 8.40 |
| 2021.05 | 75.3 | 77.1 | 21.2 | 25.8 (+1.0) | 6.50 |
| 2021.06 | 79.4 | 81.8 | 25.0 | 27.7 (+1.9) | 5.52 |
| 2021.07 | 81.0 | 83.6 | 34.3 | 31.4 (+3.7) | 5.51 |
| 2021.08 | 77.7 | 79.7 | 22.0 | 35.3 (+3.9) | 6.19 |
| 2021.09 | 87.0 | 88.2 | 51.3 | (39.9 projected, +4.6) | 6.33 |
| 2021.10 | 88.9 | 88.3 | 38.1 | (43.6 projected, +3.7) | 7.38 |
| 2021.11 | 86.2 | 84.4 | 35.0 | (48.2 projected, +4.6) | 9.83 |
| 2021.12 | 103.0 | 99.8 | 67.6 | (54.0 projected, +5.8) | 6.40 |
| 2022.01 | 103.8 | 100.5 | 54.0 | (57.7 projected, +3.7) | 8.92 |
| 2022.02 | 109.1 | 106.5 | 59.7 | (62.4 projected, +4.7) | 10.46 |
| 2022.03 | 110.9 (1) | 51.3 (2A) / 63.6 (2B) / 77.5 (2C) | (67.9 projected, +5.5) | (9.9) | |
| 2022.04 | (73.0 projected, +5.1) | ||||
| 2022.05 | (79.4 projected, +6.4) | ||||
| 2022.06 | (85.3 projected, +5.9) | ||||
| 2022.07 | (92.6 projected, +7.3) | ||||
| 2022.08 | (99.2 projected, +6.6) | ||||
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 30 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: SIDC-SILSO.
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.
