Solar prominence activity
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Following a series of small flares and subsequent magnetic field destabilization, cool plasma is heated and transferred to a solar prominence, following magnetic field lines in the solar corona. Prominences are clouds of cool (few tens of thousands of Kelvin) material suspended in the hot (millions of Kelvin) corona by the magnetic field structure; this magnetic field also hampers thermal conduction from the corona to the prominence. Such prominence magnetic field structure can be further destabilized, producing a solar eruption, with possible consequences on “space weather” at Earth and elsewhere in the heliosphere.
To produce this movie, SDO/AIA observation data have been transformed to polar coordinates, so that gravity points towards the bottom of images. Five extreme-UV images (with wavelengths given in Ångström: 304, 171, 193, 211, 131) have been combined to give each image of the movie, with colors chosen according to the temperature of maximum UV emission of the coronal plasma in each band (from 50,000K to 10 million K). The image width could fit 150 times our planet’s diameter (1.8 million kilometers) at the solar limb.
Data courtesy of NASA/SDO and the AIA science team, processed at MEDOC (CNES/CNRS-INSU/Univ. Paris-Sud)
This event has been featured as “Sun dance“ by NASA Astronomy Picture Of the Day.
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