Last major update issued on January 25, 2005 at 05:00 UTC.
geomagnetic data - last month (updated daily)]
[Solar wind and electron fluence charts (updated daily)]
[Solar cycles 21-23 (last update January 2, 2005)]
[Solar cycles 1-20]
[Graphical comparison of cycles 21, 22 and 23 (last update January 2, 2005)]
[Graphical comparison of cycles 2, 10, 13, 17, 20 and 23 (last update January 2, 2005)]
[Historical solar and geomagnetic data charts 1954-2004 (last update November 8, 2004)]
[Archived reports (last update January 19, 2005)]
The geomagnetic field was quiet on January 24. Solar wind speed ranged between 547 and 650 km/sec under the weakening influence of a high speed stream from coronal hole CH140.
Solar flux measured at 20h UTC on 2.8 GHz was 94.6. The planetary
index was 6 (STAR Ap - based on the mean of three hour interval ap
Three hour interval K indices: 21122221 (planetary), 21222221 (Boulder).
The background x-ray flux is at the class A8 level.
At midnight there were 4 spotted regions on the visible solar disk. The solar flare activity level was very low. No C class events were recorded during the day.Region 10723 was quiet and stable.
Spotted regions not numbered by SEC/NOAA:
[S504] This region emerged in the southeast quadrant on January 24. Location at midnight: S12E03.
January 22-24: No obvious fully or partly Earth directed CMEs were observed.
history (since late October 2002)
Compare today's report with the situation one solar rotation ago: 28 days ago 27 days ago 26 days ago
A coronal hole (CH141) in the southern hemisphere could rotate to a geoeffective position on January 25-26. A recurrent trans equatorial coronal hole (CH142) will likely rotate to a geoeffective position on January 27-29.
Processed SOHO/EIT 284 image at 01:06 UTC on January 25. The darkest areas on the solar disk are likely coronal holes.
The geomagnetic field is expected to be mostly quiet on January 25-27. On January 28-29 a high speed stream from coronal hole CH141 is likely to cause unsettled to active conditions while effects from coronal hole CH142 could extend these conditions until February 1.
|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) Material from a CME is likely to impact Earth within 96 hours.
3) There is a possibility of either M or X class flares within the next 48 hours.
Green: 0-20% probability, Yellow: 20-60% probability, Red: 60-100% probability.
Long distance low and medium frequency (below 2 MHz) propagation along east-west paths over high and upper middle latitudes is poor. Propagation along long distance north-south paths is very poor. Trans Atlantic propagation conditions are normally monitored every night on 1470 kHz. Dominant station tonight: Radio Vibración (Venezuela) with a very weak signal. A few stations from North America were heard with mostly weak signals, CJYQ on 930 kHz had the best signal.
Compare to the previous day's image.
Data for all numbered solar regions according to the Solar Region Summary provided by NOAA/SEC. 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 SEC or where SEC has observed no spots. SEC active region numbers in the table below and in the active region map above are the historic SEC/USAF numbers.
|Active region||Date numbered||SEC
|Location at midnight||Area||Classification||Comment|
classification was HSX at midnight, area 0070
classification was DAO at midnight, area 0080
|Total spot count:||12||10|
flux at Earth
|International sunspot number||Smoothed sunspot number|
cycle 23 sunspot max.
|2004.07||119.1||51.0||(39.6 predicted, -1.9)|
|2004.08||109.6||40.9||(38.0 predicted, -1.6)|
|2004.09||103.1||27.7||(36.1 predicted, -1.9)|
|2004.10||105.9||48.4||(33.9 predicted, -2.2)|
|2004.11||113.2||43.7||(32.0 predicted, -1.9)|
|2004.12||94.5||17.9||(29.7 predicted, -2.3)|
|2005.01||106.5 (1)||42.2 (2)||(27.0 predicted, -2.7)|
1) Running average based on the daily 20:00 UTC observed solar flux
value at 2800 MHz.
2) Unofficial, accumulated value based on the Boulder (NOAA/SEC) sunspot number. The official international sunspot number is typically 30-50% less.
This report has been prepared by Jan Alvestad. It is based partly on my own observations and analysis, and partly on data from some of these solar data sources. All time references are to the UTC day. Comments and suggestions are always welcome.