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Observations

Space Based Imaging

More data: SWAP, EUI

Ground Based Imaging

More: H-α, WL, Ca-IIK, Drawings

Ground Based Radio

More: ARCAS+HSRS, CALLISTO

Space Based Timelines

More data: LYRA, TSI

WDC Sunspot Index

More data: SILSO

Space Weather Services

Detections

Solar Map

Latest Alerts

Presto 2024-10-31

An X2.0-flare with start time 21:12 UTC, end time 21:27 UTC and peak time 21:20 UTC on Oct 31st was produced by SIDC Sunspot Group 217 (NOAA Active Region 3878). This region has a complex magnetic field configuration, classified as type beta-gamma-delta, and has produced multiple M-class flaring over the past days. The greater than 10 MeV proton flux levels are expected to increase over the next hours. Coronagraph imagery are further awaited to check for any possible Earth-directed coronal mass ejection related to this event.

CACTus Halo 2024-10-31

A halo or partial-halo CME was detected with the following characteristics: t0 | dt0| pa | da | v | dv | minv| maxv| 2024-10-28T11:24:11.308 | 6.0 | 234 | 246 | 686 | 369 | 95 | 1202 t0: onset time, earliest indication of liftoff dt0: duration of liftoff (hours) pa: principal angle, counterclockwise from North (degrees) da: angular width of the CME (degrees), v: median velocity (km/s) dv: variation (1 sigma) of velocity over the width of the CME mindv: lowest velocity detected within the CME maxdv: highest velocity detected within the CME

Forecasts

  • Flare: M-class flares
    (≥50%)
  • Protons: Warning condition
    (increased activity)
  • Geomagnetic: Active conditions
    (A>=20 or K=4)
  • All quiet: False
  • Provisional SSN: 211

Solar Activity

URSIgram 2024-11-01

Solar flaring activity over the past 24 hours was at very high levels with multiple M-class flares and an X2.0-flare with start time 21:12 UTC, end time 21:27 UTC, peak time 21:20 UTC on Oct 31st, associated with SIDC Sunspot Group 217 (NOAA Active Region 3878). There are eleven numbered active regions on the visible solar disc with SIDC Sunspot Group 217 (NOAA Active Region 3878) and SIDC Sunspot Group 273 (NOAA Active Region 3869) being the largest and most complex ones, classified as magnetic type beta-gamma-delta. SIDC Sunspot Group 217 (NOAA Active Region 3878) was responsible for most of the of flaring activity together with SIDC Sunspot Group 298 (NOAA Active Region 3876, magnetic type beta-gamma) and an isolated low M-class flaring contribution from SIDC Sunspot Group 297 (NOAA Active Region 3875, magnetic type beta), which exhibited further growth. The solar flaring activity is likely to be at moderate to high levels over the coming days with likely M-class flaring and 35% chances for X-flares. No Earth-directed coronal mass ejections (CMEs) have been detected in the available coronagraph imagery over the past 24 hours. Over the past 24 hours the greater than 10 MeV GOES proton flux has gradually decreased bellow the 10 pfu minor radiation storm threshold with an intermediate enhancement possibly related to the observed X-class flaring. The greater than 10 MeV GOES proton flux is expected to decrease towards nominal levels over the 24 hours with chances for new enhancements related to anticipated high levels of solar eruptive activity. The greater than 2 MeV electron flux as measured by GOES 16 and GOES 18 was below the 1000 pfu threshold and could reach the 1000 pfu threshold over the next 24 hours. The 24h electron fluence was at nominal levels and is expected to remain so in the next 24 hours.

Solar Wind

URSIgram 2024-11-01

The geomagnetic conditions over the past 24 hours were globally quite to active and locally over Belgium quiet to unsettled. Mostly quiet to unsettled geomagnetic conditions are expected for the next 24 hours with remaining chances of isolated active conditions. Quiet to active conditions are expected for Nov 3rd with chances of reaching minor storm levels on Nov 3rd and Nov 4th. Over the past 24 hours the solar wind parameters (ACE and DSCOVR) have been indicative of the continuous influence of a high speed stream from a negative polarity coronal hole. The interplanetary magnetic field was slightly elevated reaching a maximum value of 10.4 nT with a minimum Bz of -8.1 nT. The solar wind velocity was varying between 377 km/s and 620 km/s. The B field phi angle remained predominantly in the negative sector (directed towards the Sun). The solar wind conditions are expected to remain at slightly elevated conditions over the next 24 hours and return to background slow solar wind regime until probable high speed stream arrivals from two negative polarity coronal holes and a possible minor glancing blow arrival on Nov 3rd and Nov 4th.

Research

News

SUVIX2

X2.0 flare in NOAA 3878

Another X-class flare, and once again from a different region. NOAA 3878 was the source of an X2.0 flare on 31 October.
HalphaX3

Comparing 2 solar storms

The solar storms of 24 and 26 October are compared from the initial X-class flare to the geomagnetic disturbance that resulted from the associated coronal mass ejection.
AIA094_X1

X1.8 flare in NOAA 3873

Another X-class flare, but from a different region. The associated coronal mass ejection may deliver a glancing blow on 28 October.
 

Activities

Ground Observations

The SIDC monitors the level of solar activity from the photosphere to the corona with ground based instruments located in Uccle and Humain.

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Space Instruments

To avoid the disturbing or blocking effect of the Earth atmosphere, EUV observations of the solar corona need to be made from space...

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Space Weather & Climate

We monitor and forecast solar variability to provide information services  to society and industry about the influence of space weather and climate.

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Data Processing & Distribution

Data processing is necessary to extract relevant information for research studies, whereas data distribution and visualization are part of ROB open data policy.

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Modeling

Modelling of Solar phenomena allows scientists to test theories and to predict Space Weather phenomena and their impact on Earth.

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Supporting Research

The SIDC shares and expands its expertise through interaction with both upcoming and experienced researchers.

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