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The event occurred in 2012, near the local maximum of sunspots that can be seen in this graph.. At 02:08 UT on 23 July 2012, a large coronal mass ejection (CME) was launched from the Sun. [3] The eruption emanated from solar active region 11520 and coincided with what was at most an X2.5-class solar flare. [4]
On August 31, 2012, a long prominence/filament of solar material that had been hovering in the Sun's atmosphere, the corona, erupted out into space at 4:36 p.m. EDT. Diagram of the magnetic-field structure of a solar flare and its origin, inferred to result from the deformation of such a magnetic structure linking the solar interior with the ...
Solar flare, a large explosion in the Sun's atmosphere caused by tangling, crossing or reorganizing of magnetic field lines; Coronal mass ejection (CME), a massive burst of plasma from the Sun, sometimes associated with solar flares; Geomagnetic storm, the interaction of the Sun's outburst with Earth's magnetic field
Full coverage: Total solar eclipse photos, videos and reactions from the path of totality. Solar Eclipse 2024: 33 photos that show the rare astronomical event in all of its glory. Photos: Past ...
CMEs typically reach Earth one to five days after leaving the Sun. The strongest deceleration or acceleration occurs close to the Sun, but it can continue even beyond Earth orbit (1 AU), which was observed using measurements at Mars [21] and by the Ulysses spacecraft. [22] ICMEs faster than about 500 km/s (310 mi/s) eventually drive a shock ...
The moon will appear to move in front of the sun beginning at 2:07 p.m. on April 8 in Rochester, New York. The window of totality is just 3 minutes and 38 seconds, with variance for location, and ...
This article is part of Our Top 5 Energy Stocks for 2012 series. As we look forward to 2012 in the energy sector, I feel like a kid in a candy store. There are so many exciting developments, from ...
A common measure of flare duration is the full width at half maximum (FWHM) time of flux in the soft X-ray bands 0.05 to 0.4 and 0.1 to 0.8 nm measured by GOES. The FWHM time spans from when a flare's flux first reaches halfway between its maximum flux and the background flux and when it again reaches this value as the flare decays.