Last major update issued on October 25, 2006 at 03:35 UTC.
geomagnetic data - last month (updated daily)]
[Solar wind and electron fluence charts (updated daily)]
[Solar cycles 21-23 (last update October 2, 2006)]
[Solar cycles 1-20]
[Graphical comparison of cycles 21, 22 and 23 (last update October 2, 2006)]
[Graphical comparison of cycles 2, 10, 13, 17, 20 and 23 (last update October 2, 2006)]
[Historical solar and geomagnetic data charts 1954-2005 (last update March 3, 2006)]
[Archived reports (last update October 2, 2006)]
The geomagnetic field was quiet on October 24. Solar wind speed ranged between 378 and 519 km/s (all day average 453 km/s - decreasing 46 km/s from the previous day).
Solar flux measured at 20h UTC on 2.8 GHz was 74.8. The planetary A index was 4 (STAR Ap - based on the mean of three hour interval ap indices: 4.0). Three hour interval K indices: 01211111 (planetary), 01322221 (Boulder).
The background x-ray flux is at the class A2 level.
At midnight there was 1 spotted region on the visible solar disk. The solar flare activity level was very low. No C class events were recorded during the day.
Region 10917 decayed slowly and quietly.
October 22-24: No obvious partly or fully Earth directed CMEs were detected in LASCO imagery.
Coronal hole history (since late October 2002)
Compare today's report to the situation one solar rotation ago: 28 days ago 27 days ago 26 days ago
A fragmented trans equatorial coronal hole structure (CH245) will be in an Earth facing position on October 24-26. The extension into the northern hemisphere is poorly defined.
Processed SOHO/EIT 284 image at 19:06 UTC on October 24. The darkest areas on the solar disk are likely coronal holes.
The geomagnetic field is expected to be quiet on October 25-26. On October 27-29 quiet to active conditions are likely due to effects from CH245.
|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: 0-20% 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 to fair. Propagation on long distance northeast-southwest paths is poor.
Monitoring remarks from a location near N58E06: Propagation conditions were unusually variable during the night. At times no North American stations were audible, at other times some stations, like 1130 WBBR, had huge signals. Stations from Venezuela had the most stable signals with 750 RCR excellent.
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|
|10917||2006.10.19||13||11||S05W73||0140||CAO||classification was DSO at midnight, area 0070|
|10918||2006.10.23||2||S04W85||0030||HRX||rotated out of view|
|Total spot count:||15||11|
flux at Earth
|International sunspot number||Smoothed sunspot number|
cycle 23 sunspot max.
|2006.04||89.0||30.2||(17.1 predicted, -0.2)|
|2006.05||80.9||22.2||(16.8 predicted, -0.3)|
|2006.06||76.5||13.9||(15.1 predicted, -1.7)|
|2006.07||75.7||12.2||(13.2 predicted, -1.9)|
|2006.08||79.0||12.9||(12.8 predicted, -0.4)|
|2006.09||77.8||14.5||(12.6 predicted, -0.2)|
|2006.10||74.2 (1)||12.4 (2)||(11.6 predicted, -1.0)|
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% lower.
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.