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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 2024-03-28

An X1.1 flare, with peak time 20:56 UTC on March 28, was produced by NOAA AR 3615. No dimming is observed with this event and the coronagraph imagery is not yet available to determine if there is an Earth-directed CME. Due to the location of the flaring region an increase in proton flux is possible in the next hours, and there is an overall heightened risk for proton events in the next days from any further strong X- or M-class flares from this region as it rotates towards the limb.

Flaremail 2024-03-28

A class X1.1 solar X-ray flare occurred on 2024/03/28 with peak time 20:56UT

CACTus Halo 2024-03-27

A halo or partial-halo CME was detected with the following characteristics: t0 | dt0| pa | da | v | dv | minv| maxv| 2024-03-27T03:12:11.858 | 3.0 | 84 | 258 | 1201 | 505 | 151 | 1953 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: Quiet
    (A<20 and K<4)
  • All quiet: False
  • Provisional SSN:

Solar Activity

URSIgram 2024-03-29

The solar flaring activity was at high levels. The largest flare of the period was an X1.1 flare with peak time 20:56 UTC March 28. This flare originated from Catania region 22 (NOAA AR 3615), which is the largest and most complex region on disk (magnetic configuration Beta-Gamma-Delta). This region produced the majority of the flaring activity including four further M-class flares. Catania region 31 (NOAA AR 3620) decayed into a plage region. The remaining few active regions on disk are all simple and were either stable or in decay. The solar flaring activity is expected to be at moderate to high levels over the next 24 hours with C-class flares expected, M-class flares likely and a low probability for an X-class flare. No Earth directed Coronal Mass Ejections (CMEs) have been detected in the available coronagraph imagery. A positive polarity coronal hole in the southern hemisphere continues to traverse the central meridian since March 27. Over the past 24 hours the greater than 10 MeV GOES proton flux was below the 10pfu threshold. There is a slight chance that the proton flux may increase in response to any strong flares from NOAA AR 3615 The greater than 2 MeV electron flux increased slightly but remained below the 1000 pfu threshold as measured by GOES 16. It is expected to exceed this threshold over the next days. The 24-hour electron fluence was at nominal levels. The electron fluence is expected to increase to normal to moderate levels over the next day.

Solar Wind

URSIgram 2024-03-29

Geomagnetic conditions were at quiet to unsettled levels (NOAA Kp 3 and Local K Bel 3). Geomagnetic conditions are expected to be at quiet to unsettled levels on March 29 to March 30. The solar wind conditions reflected a slow solar wind regime. The solar wind speed gradually decreased from values around 430 km/s to around 350 km/s. The interplanetary magnetic field ranged between 0 and 5 nT. The Bz component reached a minimum value of -2 nT. The interplanetary magnetic field phi angle switched between the positive and negative sectors. The solar wind speed is expected to reflect slow solar wind conditions on March 29 and March 30. Possible enhancements in the solar wind speed, due to a weak high-speed stream associated with the positive polarity coronal holes, may be expected from March 31.

Research

News

NOAA 3615 finally did it!

NOAA 3615 produced its first X-class flare late on 28 March.

Teamwork

A long-duration X1 flare was associated with the strongest proton event so far this solar cycle, as well as with an earth-directed full halo CME. ***UPDATED***

NOAA 3599's spectacular eruption

Active region NOAA 3599 had already rotated over the Sun's west limb when it produced a spectacular long duration C-class flare.
 

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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