Solar Terrestrial Activity Report

Activity chart

Last major update issued on July 28, 2012 at 06:00 UTC.

[Solar and geomagnetic data - last month (updated daily)]
[Solar wind and electron fluence charts (updated daily)]
[Solar cycles 21-24 (last update June 2, 2012)] [Cycle 24 progress NEW]
[Solar cycles 1-20]
[Graphical comparison of cycles 21, 22, 23 and 24 (last update June 2, 2012)]
[Graphical comparison of cycles 10, 12, 13, 14, 16 and 24 (last update June 2, 2012)]
[Historical solar and geomagnetic data charts 1954-2006 (last update April 5, 2007)]
[Archived reports since January 2003 (last update July 1, 2012)]

[POES auroral activity level since October 2009 - updated July 17, 2012]
[Solar polar fields vs solar cycles - updated June 27, 2011]

Recent activity

The geomagnetic field was quiet on July 27. Solar wind speed at SOHO ranged between 283 and 398 km/s.

Solar flux measured at 20h UTC on 2.8 GHz was 123.3 (decreasing 0.7 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: 3.6). Three hour interval K indices: 01110102 (planetary), 11111202 (Boulder).

The background x-ray flux is at the class B5 level.

At midnight UTC the visible solar disk had 11 spotted active regions (in 2K resolution SDO images).

Region 11526 [S15W25] decayed quickly and quietly.
Region 11527 [N25E15] was quiet and stable.
Region 11528 [N17E12] was quiet and stable. The region has polarity intermixing. Flare: C5.0 at 04:02 UTC
Region 11529 [S11E17] was quiet and stable.
Region 11530 [S19E27] added small spots and has polarity intermixing.
Region 11531 [N15W71] decayed slowly. A few minor C flares were produced early in the day.
Region 11532 [S22E61] is a large and complex region with a magnetic delta structure in the largest leading penumbra. Further M class flaring is possible. Flare: M2.7 at 17:26 UTC. A small and slow CME was observed after this event.
New region 11533 [S28E18] emerged on July 26 and was numbered by SWPC the next day.

Spotted active regions not numbered or interpreted differently by NOAA/SWPC:
S1820
[N17W18] reemerged with a tiny spot.
New region S1825 [N17E67] rotated into view with a small spot.
New region S1826 [S25W14] emerged with a tiny spot.

Coronal mass ejections (CMEs)

July 25-27: No obviously Earth directed CMEs were observed in LASCO and STEREO imagery.

Coronal holes

Coronal hole history (since 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 (CH525) was in an Earth facing position on July 25-27.

Coronal hole map

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.

Propagation

Long distance low and medium frequency (below 2 MHz) propagation along paths north of due west over high and upper middle latitudes is poor to fair. Propagation on long distance northeast-southwest paths is poor.

Forecast

The geomagnetic field is expected to be quiet initially on July 28, a high speed stream from CH525 will likely arrive later in the day causing unsettled to minor storm conditions until July 30.

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 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.

Active solar regions

Click on image for higher resolution image) Compare to the previous day's 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
detected
Spot count Location at midnight Area Classification SDO / HMI 4K continuum
image with magnetic polarity overlay
Comment
SWPC STAR SDO SWPC STAR Current Previous
2K 1K
11525 2012.07.16
2012.07.17
      S21W86        

plage

11526 2012.07.19
2012.07.20
3 7 1 S17W28 0020 CRO BXO location: S15W25
11531 2012.07.19
2012.07.26
3 9 4 N15W73 0010 BXO DRI location: N15W71

area: 0020

S1811 2012.07.21       S11W56           plage
11528 2012.07.22
2012.07.23
2 11 5 N17E11 0030 HSX CAO beta-gamma

area: 0080

11527 2012.07.22
2012.07.23
  3   N27E11 0000   AXX location: N25E15
11529 2012.07.22
2012.07.23
2 4 1 S11E16 0080 HSX CSO area: 0120
11530 2012.07.23
2012.07.24
3 14 4 S19E28 0130 CSO CSO beta-gamma

area: 0250

S1817 2012.07.23       S34W45           plage
S1819 2012.07.24       N21W07         plage
S1820 2012.07.24   1   N17W18          
11532 2012.07.25
2012.07.26
3 31 16 S20E53 0060 CSO FKI beta-gamma-delta

area: 0500

location: S22E61

what is SWPC observing?

S1822 2012.07.25       N20W22           plage
11533 2012.07.26
2012.07.27
5 13 5 S28E18 0040 CAO DRI  
S1825 2012.07.27   1 1 N17E67 0000   AXX    
S1826 2012.07.27   1   S25W14 0000   AXX    
Total spot count: 21 95 37  
Sunspot number: 91 205 117  (total spot count + 10 * number of spotted regions)
Weighted penumbral SN: 49 126 68  (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): 55 72 64 k * (sunspot number). k = 0.6 for SWPC, k = 0.35 (changed from 0.45 on March 1, 2011) for STAR SDO 2K, k = 0.55 for STAR SDO 1K

Monthly solar cycle data

Month Average measured solar flux International sunspot number (SIDC) Smoothed sunspot number Average ap
(3)
2008.07 65.7 (SF minimum) 0.5 2.8 (-0.4)  
2008.12 69.2 0.8 1.7 (-)
sunspot minimum
 
2011.04 112.6 54.4 41.8 (+4.9) 8.83
2011.05 95.8 41.6 47.6 (+5.8) 8.94
2011.06 95.8 37.0 53.2 (+5.6) 8.06
2011.07 94.2 43.9 57.2 (+4.0) 8.16
2011.08 101.7 50.6 59.0 (+1.8) 7.26
2011.09 133.8 78.0 59.5 (+0.5) 12.27
2011.10 137.3 88.0 59.9 (+0.4) 8.28
2011.11 153.5 96.7 61.1 (+1.2) 5.55
2011.12 141.3 73.0 63.4 (+2.3) 3.78
2012.01 132.5 58.3 (65.0 projected, +1.6) 7.15
2012.02 106.5 33.1 (66.5 projected, +1.5) 8.81
2012.03 114.7 64.2 (67.2 projected, +0.7) 16.08
2012.04 113.0 55.2 (66.5 projected, -0.7) 10.10
2012.05 121.5 69.0 (64.8 projected, -1.7) 7.06
2012.06 119.6 64.5 (64.0 projected, -0.8) 10.08
2012.07 133.9 (1) 86.4 (2A) / 99.2 (2B) (65.0 projected, +1.0) (15.13)

1) Running average based on the daily 20:00 UTC observed solar flux value at 2800 MHz.
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.