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Submitted on 2005-12-20
Maybe you noticed: the daily ursigrams and geoalert have changed a little! From today onwards, we provide an estimation of the International Sunspot Number, in short: the Estimated ISN.
Submitted on 2005-12-06
Ten years ago, SOHO, the Solar and Heliospheric Observatory, was launched. The satellite is able to watch the Sun continuously. It was meant to stay operational for 2 years, but now, 10 years later, it still is! The SIDC is closely involved in the EIT and LASCO instruments, which prove to be very valuable to do the space weather forecast.
Submitted on 2005-11-08
As active as was the Sun in September, as quiet is it now. Both the 10.7 cm solar radio flux and the International Sunspot Number are pointing to solar minimum.
Submitted on 2005-10-28
Since October 21, the x-ray radiation dropped below the A-level. After the turbulent presence of the big sunspot 37/0808 during September, the Sun is taking a break. The 'All-quiet-alert' that was broadcast since Wednesday is still valid.
Submitted on 2005-10-03
The solar telescope of the SIDC caught the moon in front of the Sun. The result in visible light and in the H-alpha wavelength is shown below.
Submitted on 2005-09-08
Yesterday, September 7, the GOES satellite detected a strongly enhanced x-ray flux. The curve went up to X17, the saturation level of the satellite! In the ranks, this is the fourth biggest flare since 1976 according to IPS.
Submitted on 2005-06-02
Every first day of the month, the provisional International Sunspot Number is calculated based on observations of sunspots sent to us by observers all over the world.
Submitted on 2005-05-12
We signed up for a period with more activity after a long time of flaring silence. The long duration C8.0 flare in the night between May 2 and 3 was the starting shot of a new series of M-flares.
Submitted on 2005-04-29
In the time period around solar minimum, we have less sunspots, less flares, less coronal mass ejections (CMEs). If there are CMEs, they predominantly originate from erupting filaments.
SOHO/EIT 304 can capture nicely filaments and possible eruptions. Filaments are pictured as dark lines on the solar disk. When they erupt, they appear as orange loops in the black area around the Sun.
Submitted on 2005-04-14
The 'mega-cool' filament is still visible in recent H-alpha pictures. It lasted for 3 solar rotations.
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