SIDC Weekly Bulletin
Review of past solar and geomagnetic activity.| Source | SIDC (RWC-Belgium) |
| Frequency | Weekly |
| Format | Plain text |
| Mail header | SIDC Weekly Bulletin |
| SIDC code | bul |
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:Issued: 2024 May 15 1745 UTC :Product: documentation at http://www.sidc.be/products/bul #--------------------------------------------------------------------# # SIDC Weekly bulletin on Solar and Geomagnetic activity # #--------------------------------------------------------------------# WEEK 1219 from 2024 May 06 Solar Active Regions (ARs) and flares --------------- The solar flaring activity was at high to very high levels with several M-class flares and X-class flares, over the past week. There were 16 numbered active regions on the visible solar disk throughout the week, which produced 49 C-class flares, 75 M-class flares, and 10 X-class flares. The strongest flare was a GOES X5.8 flare from NOAA Active Regions (AR) 3664 (beta-gamma-delta) which peaked at 01:23 UTC on May 11. NOAA AR 3663 (beta-gamma-delta), AR 3664 (beta-gamma-delta), and AR 3668 (beta-gamma) were the magnetically complex regions which produced almost all flaring activities. Coronal mass ejections --------------------- During the past week, eight notable coronal mass ejections (CMEs) were observed. Among these, two were halo CMEs and six were partial halo CMEs. All these CMEs were associated with X-class/M-class flares from the NOAA active regions (AR) 3664. First halo CME was observed on SOHO/LASCO-C2 images 05:30 UTC on May 08, with a speed of about 530 km/s. This halo CME was associated with an X1.0 flare which peaked at 05:09 UTC, and associated type II and type IV radio emissions were observed starting at 05:01 UTC and 05:08 UTC, respectively. The second halo CME was observed on LASCO-C2 images around 12:48 UTC on May 08, with a speed of about 670 km/s. This halo CME was associated with a M8.7 flare which peaked at 12:04 UTC. The first partial halo CME was observed on LASCO-C2 images around 22:36 UTC on May 08. This CME was associated with a X1.0 flare which peaked at 21:40 UTC. It had a projected width of about 184 deg (as measured by the Cactus tool) and a speed of about 840 km/s. The second partial halo CME was observed on LASCO-C2 images around 09:24 UTC on May 09. This CME was associated with an X2.3 flare which peaked at 09:13 UTC. It had a projected width of about 180 deg and a projected speed of about 1000 km/s. Associated type II and type IV radio emissions were detected at 09:02 UTC and 09:10 UTC, respectively. All the above mentioned halo and partial halo CMEs possibly arrived at Earth on May 10-11. The third partial halo CME was first observed on LASCO-C2 images around 18:58 UTC (with data gap before in LASCO-C2 images) on May 09, with a speed of about 800 km/s. This CME was associated with an X1.1 flare which peaked at 17:44 UTC, and associated type II and type IV radio emissions were detected at 17:32 UTC and 17:45 UTC, respectively. The fourth partial halo CME was observed on LASCO-C2 images around 07:12 UTC on May 10, with a speed of about 950 km/s. This CME was associated with a X4.0 flare which peaked at 06:54 UTC. Associated type II and type IV radio emissions were detected at 06:46 UTC and 06:51 UTC, respectively. The third and fourth partial halo CMEs possibly arrived at Earth on May 11-12. The fifth bright partial halo CME was observed on LASCO-C2 images around 01:36 UTC on May 11. This CME was associated with an X5.8 flare which peaked at 01:23 UTC. Associated type II and type IV radio emissions were detected at 01:13 UTC and 01:24 UTC, respectively. This CME had a speed of about 1050 km/s which possibly arrived at Earth on May 12. Another possibly partial halo CME was observed in LASCO-C2 images around 02:00 UTC on May 12 with a speed of about 600 km/s, which was possibly associated with a filament eruption on the SE quadrant of the Sun. Coronal Holes --------------------- Two coronal holes (CH) have crossed the central meridian during the past week. The first one was a positive polarity, equatorial, north CH. The second one was a negative polarity, mid-latitude, south CH. Both CHs crossed the central meridian on May 10, and the associated high speed stream possibly started to enhance the solar wind environment near Earth on May 11. Proton flux levels --------------------- The greater than 10 MeV GOES proton flux was below the 10 pfu threshold level at the beginning of the week. It started to increase around 11:00 UTC on May 09, associated with coronal mass ejections and flaring activities from NOAA AR 3664, and crossed the 10 pfu threshold level around 13:30 UTC on May 10. It briefly dropped below the 10 pfu threshold level from 01:10 UTC to 02:10 UTC on May 11 before increasing again from 02:10 UTC on May 11 and dropping below the threshold level at 12:45 UTC on May 12. The greater than 50 MeV GOES proton flux began to increase from 01:40 UTC on May 11, crossed the 10 pfu threshold level at 05:50 UTC on May 11, and dropped below the threshold level around 17:00 UTC on May 11. The greater than 100 MeV GOES proton flux also started to enhance from 01:40 UTC on May 11 but it remained below the 10 pfu threshold throughout the week. By the end of the week, all three proton fluxes (greater than 10 MeV, greater than 50 MeV, and greater than 100 MeV) were below the 10 pfu threshold level and decreasing. Electron fluxes at GEO --------------------- The greater than 2 MeV electron flux, as measured by the GOES-16 satellite, was below the threshold level over the past week. The 24h electron fluence was at normal level during the past week. Solar wind --------------------- At the beginning of the past week, the solar wind parameters were disturbed due to the influence of interplanetary coronal mass ejections (ICME) associated with CMEs observed on May 01-03, as well as high speed streams (HSS) originating from three positive coronal holes (CH) that crossed central meridian during May 02-04. The solar wind speed increased to as high as 560 km/s, interplanetary magnetic field reached 16 nT, and North-South component (Bz) decreased to as low as -12 nT following the arrival of ICME and HSS. The solar wind speed decreased to 400 km/s on May 10 noon just before the arrival of strongest ICME. Earth came under the influence of strongest ICMEs in 20 years on the evening of May 10. The first shock was detected in the solar wind data around 16:42 UTC on May 10. The interplanetary magnetic field jumped from 4 nT to 44 nT, the solar wind speed jumped from 460 km/s to 700 km/s and the solar wind density at the shock increased from 5/cm3 to 30/cm3. The second shock was observed on around 21:39 UT on May 10. The solar wind speed increased as high as 800 km/s, the interplanetary magnetic field increased as high as 74 nT, and Bz component decreased as low as -50 nT. These two shocks were related to the CMEs observed during May 08-09, and possibly two to four associated ICMEs arrived at Earth during May 10-11. The third shock-like structure was detected in the solar wind data around 17:55 UTC on May 11. The interplanetary magnetic field jumped from 8 nT to 47 nT, the solar wind speed jumped from 800 km/s to 895 km/s. The fourth shock-like structure was detected around 08:59 UTC on May 12. The interplanetary magnetic field jumped from 5 nT to 12 nT, the solar wind speed jumped from 830 km/s to 900 km/s. The fifth shock-like structure was observed on 08:58 UTC on May 12, during which the speed increased from 830 km/s to 850 km/s and the interplanetary magnetic field increased from 5 nT to 12 nT. These three shock-like structures were probably related to the arrival of ICMEs associated with CMEs observed during May 09-11. HSS originating from two CHs, which started to cross the central meridian on May 08, also possibly started to arrive at Earth on May 11. With the arrival of multiple ICMEs and HSS, the solar wind speed increased as high as about 1000 km/s. By the end of the week, the solar wind speed was about 830 km/s and the interplanetary magnetic field returned to stable with a magnitude below 5 nT. Geomagnetism --------------------- At the beginning of the past week, geomagnetic conditions were globally and locally at quiet to minor storm conditions (NOAA Kp and K BEL 2 to 5). It increased from quiet to minor storm conditions between 18:00 UTC on May 05 and 03:00 UTC on May 06. This could be possibly initially due to the arrival of a coronal mass ejections (CME), which was observed during May 01-03, and later due to the arrival of high speed streams (HSS) originating from three positive polarity coronal holes (CHs) which crossed the central meridian during May 02-04. From the evening of May 06 until the evening of May 10, geomagnetic conditions were quiet to unsettled conditions (NOAA Kp and K BEL 2 to 3) both globally and locally. Geomagnetic conditions were globally at severe to extreme storm levels (NOAA Kp 8 to 9) from 15:00 UTC on May 10 to 16:00 UTC on May 11, and then remained at major storm levels until the end of the past week. Locally over Belgium, geomagnetic conditions were at severe storm levels (K BEL=8) from 17:00 UTC on May 10 to 01:00 UTC on May 11 and again from 09:00 UTC to 14:00 UTC on May 12, reaching the extreme storm levels (K BEL=9) from 11:00 UTC to 12:00 UTC on May 12. This was due to the arrival of multiple interplanetary coronal mass ejections (ICMEs), associated to CMEs observed during May May 08-11, as well as due to the arrival of high speed streams originating from coronal holes that started to cross the central meridian on May 08. At the end of the past week, geomagnetic conditions was at active conditions (K BEL=4) locally over the Belgium. --------------------------------------------------------------------------- DAILY INDICES DATE RC EISN 10CM Ak BKG M X 2024 May 06 199 187 171 022 C2.4 5 1 2024 May 07 /// 180 204 009 C3.8 11 0 2024 May 08 /// 154 227 008 C6.1 13 3 2024 May 09 /// 170 233 009 C5.1 13 2 2024 May 10 131 166 223 124 C5.2 11 1 2024 May 11 /// 160 214 315 C5.7 5 2 2024 May 12 /// 186 222 046 C4.9 9 1 --------------------------------------------------------------------------- # RC : Sunspot index (Wolf Number) from Catania Observatory (Italy) # EISN : Estimated International Sunspot Number # 10cm : 10.7 cm radioflux (DRAO, Canada) # Ak : Ak Index Wingst (Germany) # BKG : Background GOES X-ray level (NOAA, USA) # M,X : Number of X-ray flares in M and X class, see below (NOAA, USA) --------------------------------------------------------------------------- NOTICEABLE EVENTS SUMMARY DAY BEGIN MAX END LOC XRAY OP 10CM Catania/NOAA RADIO_BURST_TYPES 06 0047 0106 0114 N24W32 M1.6 2F 84/3663 06 0509 0528 0538 ////// M1.3 84/3663 III/1 06 0538 0635 0647 N24W32 X4.5 3B 84/3663 VI/1III/1 06 0949 0959 1004 ////// M1.5 84/3663 06 2137 2148 2158 N25W42 M1.2 2N 84/3663 06 2158 2227 2307 ////// M4.3 84/3663 07 0041 0058 0123 N27W40 M2.6 SF 84/3663 VI/1 07 0558 0616 0627 ////// M5.1 84/3663 07 0818 0823 0840 S19E06 M1.3 SN 86/3664 07 1140 1150 1201 S18E03 M2.4 2N 86/3664 07 1243 1254 1259 N27W53 M1.5 SF 84/3663 III/1 07 1316 1325 1332 ////// M1.0 84/3663 /1 07 1332 1335 1339 ////// M1.0 86/3664 36M/1I/1 07 1621 1630 1636 ////// M8.2 84/3663 /2M/1I/136 07 1958 2022 2034 ////// M2.1 86/3664 07 2113 2126 2142 ////// M3.3 84/3663 07 2142 2153 2208 ////// M3.2 84/3663 08 0133 0141 0148 ////// X1.0 B 84/3663 08 0216 0227 0236 ////// M3.4 86/3664 08 0319 0327 0338 ////// M1.8 86/3664 II/1 08 0437 0509 0532 ////// X1.0 B 86/3664 II/2I/2I/3 8V/2 08 0644 0653 0703 ////// M7.1 86/3664 08 0729 0741 0753 ////// M4.5 F 84/3663 08 0931 0937 0942 ////// M1.8 84/3663 V/1 08 0943 0948 0956 ////// M2.1 F 84/3663 08 1109 1122 1126 ////// M4.1 F 84/3663 I/2 08 1126 1204 1217 ////// M8.6 /////// 08 1732 1753 1800 ////// M7.9 N 86/3664 I/3 08 1814 1836 1851 ////// M2.9 F 84/3663 II/3 08 1915 1921 1929 ////// M2.0 86/3664 08 2027 2034 2039 ////// M1.7 86/3664 08 2108 2140 0307 ////// X1.0 86/3664 I/2V/3 08 2205 2227 2312 ////// M9.8 86/3664 I/2V/3 09 0307 0317 0323 ////// M4.0 B 86/3664 09 0323 0332 0345 ////// M4.5 B 86/3664 09 0444 0449 0455 ////// M1.7 F 86/3664 09 0603 0613 0624 ////// M2.3 86/3664 09 0830 0840 0845 ////// M2.1 /////// 09 0845 0913 0936 ////// X2.2 B 86/3664 I/2 1V/3 09 1152 1156 1202 ////// M3.1 86/3664 II/3 09 1205 1212 1220 ////// M2.9 86/3664 09 1316 1323 1329 ////// M3.7 N 86/3664 09 1723 1744 1800 S14W28 X1.1 2B 86/3664 IV/2 09 2115 2121 2125 N28W88 M1.0 SF 84/3663 09 2208 2215 2224 ////// M1.0 /////// 09 2224 2241 2247 ////// M2.6 /////// 09 2304 2308 2313 S17W43 M1.2 SF 86/3664 CTM/1 09 2344 2351 2355 ////// M1.5 86/3664 VI/2 10 0010 0013 0022 ////// M1.3 90/3664 10 0315 0329 0340 ////// M1.4 90/3664 10 0614 0624 0627 ////// M1.3 /////// III/2II/2 10 0627 0654 0706 ////// X3.9 90/3664 III/2II/3IV/2 10 1010 1014 1019 ////// M2.2 90/3664 10 1358 1411 1423 S14W39 M5.9 1N 90/3664 III/2 10 1826 1832 1838 ////// M1.1 90/3664 10 1838 1848 1857 S16W44 M1.7 1F 90/3664 VI/2 10 1857 1905 1910 ////// M2.0 90/3664 10 1935 1953 1956 ////// M1.1 90/3664 10 1956 2003 2018 ////// M1.9 90/3664 11 0110 0123 0139 S15W45 X5.8 2B 86/3664 VI/3IV/2II/3 10 2059 2108 2112 ////// M3.8 90/3664 11 1003 1018 1034 ////// M3.1 86/3664 11 1053 1056 1100 ////// M1.6 86/3664 11 1115 1144 1205 S22W44 X1.5 2B 86/3664 11 1345 1349 1408 S18W52 M1.7 1N 86/3664 11 1446 1525 1552 S15W49 M8.8 2N 86/3664 III/2VI/1 11 2032 2041 2047 ////// M1.2 86/3664 12 0041 0045 0052 S20W68 M3.2 SF 86/3664 IV/1 12 0537 0552 0606 S20W65 M2.4 SF 86/3664 12 1227 1241 1254 S09E78 M1.6 SF 86/3664 VI/1 12 1340 1347 1349 S09E78 M1.0 SF ///3679 12 1349 1356 1408 S21W70 M1.5 SF 86/3664 12 1611 1626 1638 S18W72 X1.0 1F 86/3664 12 2017 2032 2049 S18W74 M4.8 SN 86/3664 III/2VI/1 12 2201 2206 2212 S16W80 M1.1 SF 86/3664 VI/1 12 2214 2218 2224 S21E11 M1.1 SF ///3676 12 2300 2310 2314 S18W77 M1.0 SF 86/3664 III/1VI/1 #--------------------------------------------------------------------# # Solar Influences Data analysis Center - 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This report is sent once a week, typically on a monday.The weekly bulletin gives an overview of solar and geomagnetic activity of the past week and includes a noticeable solar events list.
Check the ISES code book for information on ISES codes.