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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 2024-02-29

A westward partial halo coronal mass ejection (CME) was detected in the LASCO/C2 data at 17:48 UTC on February 28. The CME originated from NOAA AR 3590 in the north-west quadrant of the solar visible disk, and was associated with a long-duration M1.3-class flare peaking at 18:19 UTC. No increase in the greater than 10 MeV proton flux has been detected in association to this eruption. The CME has an estimated speed of around 500 km/s and may result in a flank encounter at Earth on March 3. Unsettled to active geomagnetic conditions are expected due to the arrival of the interplanetary CME.

CACTus Halo 2024-02-29

A halo or partial-halo CME was detected with the following characteristics: t0 | dt0| pa | da | v | dv | minv| maxv| 2024-02-28T17:48:07.840 | 3.0 | 309 | 156 | 548 | 77 | 367 | 694 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: Quiet
  • Geomagnetic: Quiet
    (A<20 and K<4)
  • All quiet: False
  • Provisional SSN: 120

Solar Activity

URSIgram 2024-03-01

Solar flaring activity over the past 24 hours was at low levels. The largest flares was an C4.0 flare with peak time at 01:25 UTC on March 1 from NOAA AR 3590 (beta-gamma-delta). Weaker C-class flares were observed from NOAA ARs 3590, 3594, 3598, and from a yet unnumbered region at the east limb of the visible disk. There are currently 7 numbered active regions on the visible disk. NOAA AR 3590 (beta-gamma-delta) is the largest, most magnetically complex region, and has produced most of the flaring activity in the last 24 hours. A new active region (numbered NOAA AR 3598, alpha) emerged on the south-west quadrant of the visible solar disk (currently around S13W25) and is growing. Meanwhile, NOAA AR 3592 decayed to a plage. One yet unnumbered active region is rotating from the east limb (currently around S13E82) and displayed some flaring activity in the past 24 hours. All other regions were inactive. The solar flaring activity is likely to be at moderate levels over the coming days with C-class flares expected, M-class flares probable, and a small chance for X-class flares. Based on currently available coronagraph images, no Earth directed coronal mass ejections have been observed in the past 24 hours. Over the past 24 hours the greater than 10 MeV GOES proton flux was at nominal levels and is expected to remain so over the next 24 hours. Some enhancements are possible in the case of an eruptive activity from NOAA AR 3590. The greater than 2 MeV GOES 16 electron flux was below the 1000 pfu threshold and is expected to remain so in the next 24 hours. The 24h electron fluence was at nominal level and is expected to remain so in the next 24 hours.

Solar Wind

URSIgram 2024-03-01

Geomagnetic conditions were globally and locally unsettled (Kp 3 and K Bel 3) during the passage of a small magnetic structure in the solar wind. Quiet to unsettled conditions are also expected in the next 24 hours. Slow solar wind conditions were recorded over the past 24 hours. Throughout this period, the solar wind speed decreased from about 405 km/s to about 350 km/s, and the total interplanetary magnetic field ranged between 1 nT and 6 nT. Around 22:40 UTC on February 29, the passage of a small magnetic structure induced small jumps in the magnetic field strength (from 3 nT to 5 nT), and in the solar wind speed (from 375 km/s to 405 km/s). Until 07:10 UTC on March 1, when the magnetic structure ended, the magnetic field was stable with an intensity of 5 nT and a Bz (north-south) component around -4 nT. Following the passage of this magnetic structure, the solar wind speed continued to decline. The phi-angle remained predominantly in the negative sector (directed towards the Sun), with a prolonged period in the positive sector (away from the Sun) during the passage of the magnetic structure. In the next 24 hours, we expect slow solar wind conditions.

Research

News

Wuthering Heights

So far this solar cycle, NOAA 13590 is the largest sunspot group and it has produced the strongest solar flare. Some perspective.

More X-class flares

NOAA 3590 produced 3 X-class flares in 24 hours: an X1.8 flare peaking late on 21 February, an X1.7 flare peaking early on 22 February, and an X6.3 event that peaked on 22 February at 22:34UTC. The latter is the strongest flare so far this solar cycle. ***UPDATED.***

A stunning eruption

A stunning double eruption took place near the northeast solar limb on 12 February.
 

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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