Last major update issued on May 17, 2006 at 04:00 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)]
[Historical solar and geomagnetic data charts 1954-2005 (last update March 3, 2006)]
[Archived reports (last update May 3, 2006)]
The geomagnetic field was inactive to very quiet on May 16. Solar wind speed ranged between 309 and 368 (all day average 335) km/sec. Early on May 17 the interplanetary magnetic field has become stronger and swung southwards.
Solar flux measured at 20h UTC on 2.8 GHz was 71.5. The planetary A index
was 2 (STAR Ap - based on the mean of three hour interval ap
Three hour interval K indices: 10001011 (planetary), 11001101 (Boulder).
The background x-ray flux is at the class A2 level.
At midnight the visible solar disk was spotless. The solar flare activity level was very low. No C class events were recorded during the day.
May 14-16: 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 trans equatorial coronal hole (CH224) was in an Earth facing position on May 13-15. A coronal hole (CH225) in the southern hemisphere will be in an Earth facing position on May 16-17.
Processed SOHO/EIT 284 image at 01:06 UTC on May 17. The darkest areas on the solar disk are likely coronal holes.
The geomagnetic field is expected to be quiet to active on May 17-20 due to high speed streams from CH224 and CH225. Isolated minor storm intervals are possible.
|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. Propagation on long distance northeast-southwest paths is fair. Trans Atlantic propagation conditions are normally monitored every night on 1470 kHz. Near LSR both Radio Cristal del Uruguay and Rafaela Argentina were audible. On other frequencies most of the stations audible were from Argentina (710, 870 kHz a.o.) and Uruguay (1130 and 1410 kHz). From North America stations from Newfoundland had fair signal levels while both 1510 WWZN and 1660 WWRU had poor to fair signals.
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|
|Total spot count:||0||0|
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||81.9 (1)||20.9 (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.