Last major update issued on August 31, 2012 at 06:10 UTC.
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The geomagnetic field was very quiet on August 30. Solar wind speed at SOHO ranged between 350 and 457 km/s.
Solar flux measured at 20h UTC on 2.8 GHz was 127.8 (decreasing 11.9 over the last solar rotation). The Potsdam WDC planetary A index was 4 (STAR Ap - based on the mean of three hour interval ap indices: 3.5). Three hour interval K indices: 11111011 (planetary), 11122211 (Boulder).
The background x-ray flux is at the class B9 level.
At midnight UTC the visible solar disk had 13 spotted active regions (in 2K resolution SDO images).
Region 11553 [S21W30] developed further with the major spots in a
compact configuration. A minor M class flare is possible.
Region 11554 [N16W66] was quite active during the first half of the day, however, as the magnetic layout simplified activity ceased and the region is decaying. Flare: C7.6 at 09:12 UTC
Region 11555 [N07E03] decayed slowly and quietly.
Region 11558 [N17E36] decayed and could soon become spotless. This is AR 11559 in SWPC data but was originally AR 11558.
Region 11560 [N03E24] developed further and is quickly becoming the most interesting region on the visible disk. A magnetic delta structure has formed in a trailing penumbra. M flares are possible.
New region 11561 [S12E16] emerged on August 29 and was numbered the next day by SWPC.
New region 11562 [S17E52] emerged on August 29 and got its NOAA number the next day.
New region 11563 [S26E70] rotated into view. The region produced an M1.3 flare at 12:11 UTC.
Spotted regions not numbered by NOAA/SWPC:
S1884 [N13E18] was quiet and stable.
S1885 [N24W15] reemerged with a tiny spot.
S1890 [S23E36] decayed and could soon become spotless.
New region S1891 [S15E83] rotated partly into view.
New region S1892 [N13W29] emerged with a few spots.
August 28-30: No obviously Earth directed CMEs were observed in LASCO and STEREO imagery.
Coronal hole history (since October
Compare today's report to the situation one solar rotation ago: 28 days ago 27 days ago 26 days ago
A small trans equatorial coronal hole (CH531) was in an Earth facing position on August 27.
The above coronal hole map is based on a method where coronal holes are detected automatically. While the method may need some fine tuning, it has significant advantages over detecting coronal holes manually. The main improvement is the ability to detect coronal holes at and just beyond the solar limbs. Early results using this method for SDO images over a span of several weeks indicate a good match between coronal holes observed over the visible disk and their extent and position at the east and west limbs. Note that the polar coronal holes are easily detected using this method, the extent and intensity of both CHs are consistent with other data sources.
Long distance low and medium frequency (below 2 MHz) propagation along paths north of due west over high and upper middle latitudes is fair to good. Propagation on long distance northeast-southwest paths is poor.
The geomagnetic field is expected to be quiet to unsettled on August 31 due to weak effects from CH531 and quiet on September 1-2.
|Coronal holes (1)||Coronal mass ejection (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
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.
Click on image for higher resolution image) Compare to the previous day's image. 0.5k image
When available the active region map has a coronal hole polarity overlay where red (pink) is negative and blue (blue-green) is positive.
Data for all numbered solar regions according to the Solar Region Summary provided by NOAA/SWPC. 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 SWPC or where SWPC has observed no spots. SWPC active region numbers in the table below and in the active region map above are the historic SWPC/USAF numbers.
|Active region||Date numbered
|Spot count||Location at midnight||Area||Classification||SDO / HMI 4K continuum
image with magnetic polarity overlay
count includes 1 tiny leader spot not in image
|2||N17E37||0010||AXX||originally AR 11558|
|Total spot count:||38||101||50|
|Sunspot number:||118||231||140||(total spot count + 10 * number of spotted regions)|
|Weighted SN:||63||136||85||(Sum of total spot count + classification weighting for each AR. Classification weighting: X=0, R=3, A/S=5, H/K=10)|
|Relative sunspot number (Wolf number):||71||81||77||k * (sunspot number). k = 0.6 for SWPC, k = 0.35 for STAR SDO 2K, k = 0.55 for STAR SDO 1K|
|Month||Average measured solar flux||International sunspot number (SIDC)||Smoothed sunspot number||Average ap
|2012.02||106.5||32.9||(67.4 projected, +1.9)||8.81|
|2012.03||114.7||64.3||(68.1 projected, +0.7)||16.08|
|2012.04||113.0||55.2||(67.5 projected, -0.6)||10.10|
|2012.05||121.5||69.0||(65.8 projected, -1.7)||7.06|
|2012.06||119.6||64.5||(65.0 projected, -0.8)||10.08|
|2012.07||133.9||66.5||(66.0 projected, +1.0)||13.90|
|2012.08||114.9 (1)||81.3 (2A) / 84.0 (2B)||(68.6 projected, +2.6)||(7.70)|
1) Running average based on the daily 20:00 UTC observed solar flux value at
2A) Current impact on the monthly sunspot number based on the Boulder (NOAA/SWPC) sunspot number (accumulated daily sunspots / month days). The official SIDC international sunspot number is typically 30-50% lower. 2B) Month average to date.
3) Running average based on the quicklook and definitive Potsdam WDC ap indices. Values in red are based on the definitive international Potsdam WDC ap indices.
This report has been prepared by Jan Alvestad. It is based on analysis of data from whatever sources are available at the time the report is prepared. All time references are to the UTC day. Comments and suggestions are always welcome.
SDO images are courtesy of NASA/SDO and the AIA, EVE, and HMI science teams.