Last major update issued on June 27, 2006 at 04:25 UTC.
geomagnetic data - last month (updated daily)]
[Solar wind and electron fluence charts (updated daily)]
[Solar cycles 21-23 (last update June 7, 2006)]
[Solar cycles 1-20]
[Graphical comparison of cycles 21, 22 and 23 (last update June 7, 2006)]
[Graphical comparison of cycles 2, 10, 13, 17, 20 and 23 (last update June 7, 2006)]
[Historical solar and geomagnetic data charts 1954-2005 (last update March 3, 2006)]
[Archived reports (last update June 5, 2006)]
The geomagnetic field was quiet on June 26. Solar wind speed ranged between 270 and 306 km/s (all day average 274 km/s - decreasing 29 km/s from the previous day).
Solar flux measured at 20h UTC on 2.8 GHz was 76.4. The planetary A index
was 3 (STAR Ap - based on the mean of three hour interval ap
Three hour interval K indices: 10001111 (planetary), 00012100 (Boulder).
The background x-ray flux is at the class A5 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 10897 lost penumbra on the leader spot, however, several new spots emerged in the trailing negative polarity area. Polarity separation is poor and C flares are possible.
June 24-26: No 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 recurrent trans equatorial coronal hole (CH229) was in an Earth facing position June 24-26.
Processed SOHO/EIT 284 image at 19:06 UTC on June 26. The darkest areas on the solar disk are likely coronal holes.
The geomagnetic field is expected to be quiet during the first half of June 27, then become quiet to active until June 29 due to effects from CH229.
|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 to good. Trans Atlantic propagation conditions are normally monitored every night on 1470 kHz. Radio Cristal del Uruguay had a strong signal at LSR. Quite a few stations from Argentina and Uruguay were heard on other frequencies with the best signals from 1190 Radio América and 1410 AM Libre.
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|
|10897||2006.06.25||4||10||N06E57||0080||DAO||classification was CAO at midnight, area 0040|
|Total spot count:||4||10|
flux at Earth
|International sunspot number||Smoothed sunspot number|
cycle 23 sunspot max.
|2005.12||90.7||41.2||(22.8 predicted, -2.1)|
|2006.01||83.4||15.4||(20.1 predicted, -2.7)|
|2006.02||76.5||4.7||(17.1 predicted, -3.0)|
|2006.03||75.4||10.8||(15.1 predicted, -2.0)|
|2006.04||89.0||30.2||(14.4 predicted, -0.7)|
|2006.05||80.9||22.2||(13.5 predicted, -0.9)|
|2006.06||75.5 (1)||19.6 (2)||(11.4 predicted, -2.1)|
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.