Last major update issued on May 13, 2006 at 02:30 UTC.
geomagnetic data - last month (updated daily)]
[Solar wind and electron fluence charts (updated daily)]
[Solar cycles 21-23 (last update April 1, 2006)]
[Solar cycles 1-20]
[Graphical comparison of cycles 21, 22 and 23 (last update April 1, 2006)]
[Graphical comparison of cycles 2, 10, 13, 17, 20 and 23 (last update April 1, 2006)]
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[Archived reports (last update May 3, 2006)]
The geomagnetic field was quiet to active on May 12. Solar wind speed ranged between 518 and 687 (all day average 590) km/sec under the influence of a high speed stream from CH223.
Solar flux measured at 20h UTC on 2.8 GHz was 75.7. The planetary A index
was 16 (STAR Ap - based on the mean of three hour interval ap
Three hour interval K indices: 44423223 (planetary), 44423222 (Boulder).
The background x-ray flux is at the class A4 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 10880 was quiet and stable.
May 10-12: No partly or fully Earth directed CMEs were observed in LASCO imagery.
Coronal hole 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 recurrent coronal holes (CH223) in the northern hemisphere was in an Earth facing position on May 8-10. A trans equatorial coronal hole (CH224) will likely rotate into an Earth facing position on May 12-15.
Processed SOHO/EIT 284 image at 13:06 UTC on May 12. The darkest areas on the solar disk are likely coronal holes.
The geomagnetic field is expected to be quiet to active on May 13 due to a high speed stream from CH223. Quiet to unsettled conditions are likely on May 14. Another high speeed stream (from CH224) could arrive on May 15 and cause unsettled to minor storm conditions until May 18.
|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 very poor. Propagation on long distance northeast-southwest paths is poor. Trans Atlantic propagation conditions are normally monitored every night on 1470 kHz. Tonight Radio Cristal del Uruguay again had the best signal. was the dominant signal. Only a few TA stations were noted on other frequencies.
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|
|10880||2006.05.04||3||2||S09W42||0020||CSO||classification was HSX at midnight|
|Total spot count:||8||2|
flux at Earth
|International sunspot number||Smoothed sunspot number|
cycle 23 sunspot max.
|2005.11||86.3||18.0||(24.5 predicted, -1.0)|
|2005.12||90.7||41.2||(21.8 predicted, -2.7)|
|2006.01||83.4||15.4||(18.7 predicted, -3.1)|
|2006.02||76.5||4.7||(15.6 predicted, -3.1)|
|2006.03||75.4||10.8||(13.4 predicted, -2.2)|
|2006.04||89.0||30.2||(12.7 predicted, -0.7)|
|2006.05||85.1 (1)||19.8 (2)||(12.2 predicted, -0.5)|
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.