Solar Terrestrial Activity Report

Last major update issued on January 12, 2025 at 06:55 UT. Revised on March 16, 2025 based on archived SDO/HMI images

Recent activity

The geomagnetic field was at quiet to unsettled levels on January 11. Solar wind speed at SOHO ranged between 389 and 490 km/sec, averaging 418 km/sec (-10 km/sec compared to the previous day). The high latitude magnetometer at Andenes recorded quiet to active 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 156.0 - decreasing 16.0 over the previous solar rotation. (Centered 1 year average SF at 1 AU - 183 days ago: 191.14. In comparison SC24 peaked on June 28, 2014 at 145.50 while SC23 peaked on February 23, 2002 at 198.15. Current SC25 peak: 191.44 on July 8, 2024 (given a base solar flux level of 65, this is +57.07% compared to the SC24 peak and -5.04% compared to the SC23 peak). The Potsdam WDC planetary A index was 6 (STAR Ap - based on the mean of three hour interval ap indices: 6.5). Three hour interval K indices: 21111321 (planetary), 21122321 (Boulder), 41310323 (Andenes).

The background x-ray flux is at the class C1 level (GOES 18).

At the time of counting spots, spots were observed in 17 active regions using 2K resolution (SN: 269) and in 13 active regions using 1K resolution (SN: 179) images.

AR 13947 [N10W52] decayed slowly and was mostly quiet despite having a magnetic delta configuration in a trailing penumbra. C1 flares: C1.7 @ 14:37 UT
AR 13950 [S19W31] decayed slowly and quietly.
AR 13951 [S14W66] decayed slowly and quietly.
AR 13953 [N20W59] decayed slowly and quietly.
AR 13955 [S32W67] decayed slowly and quietly.
AR 13956 [N06E11] matured and was mostly quiet.

Spotted regions not observed (or interpreted differently) by SWPC/USAF:
S10539 [N13W80] decayed slowly and quietly.
S10549 [N13W60] reemerged with small spots.
S10558 [N06W09] reemerged with a tiny spot.
S10559 [S18E00] was quiet and stable.
S10563 [N15E57] was quiet and stable.
S10564 [N20W25] developed slowly and quietly.
New region S10571 [N17E85] rotated partly into view with a large spot.
New region S10572 [S06E63] emerged with a few spots.
New region S10573 [S11W53] emerged with tiny spots.
New region S10574 [N12E62] emerged with a tiny spot.
New region S10575 [S45W34] emerged with a tiny spot.

C2+ flares

C1 flares: C1.3 @ 03:13, C1.1 @ 06:56, C1.4 @ 10:55, C1.1 @ 14:54, C1.1 @ 19:53, C1.8 @ 20:48, C1.2 @ 22:40, C1.4 @ 22:14 UT

Coronal mass ejections (CMEs)

January 9-11: No obviously Earth directed CMEs.

Coronal holes

[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 small negative polarity northern hemisphere coronal hole (CH1266) rotated across the central meridian on January 10-11.

Propagation

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 to fair.

Forecast

The geomagnetic field is expected to be quiet on January 12-13. Quiet to unsettled levels are expected on January 14-15 due to effects from CH1266.

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.

Active solar regions

(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.

Monthly solar cycle data

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: WDC-SILSO, Royal Observatory Of Belgium, Brussels

Solar cycles 24-25

Update on the progress of solar cycle 25 as of December 30, 2024

Sunspot activity increased again during the second half of December 2024, and this will be the eighth consecutive month with average solar flux above 180. The average solar flux at 1 AU since May 1, 2024 is 205. There is an increasing chance solar cycle 25 could have a higher 1 year solar flux average than solar cycle 23. The above plot displays a projected peak for the ISN 365d smoothed sunspot number on October 12, 2024. All the other smoothed sunspot numbers as well as the smoothed 365d solar flux have projected peaks October 12-15. A sudden decrease in activity during the first months of 2025 could move the SC25 max to sometime between July and October 2024.

--------------------------------------------------------------------------------------

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.