Eruptive prominence in different spectral lines

Lomnicky Peak Observatory, CoMP-S

Solar prominences are seen as bright translucent clouds at the solar limb because they mainly scatter light from the underlying disc. These clouds form in regions of complex magnetic topology, which can evolve abruptly, disintegrating the prominence and ejecting magnetised material into the heliosphere. Interestingly for space weather predictions, 50% of solar tornadoes — a particular kind of prominence associated with apparently rotating, vertical, funnel-shaped dark structures — are eruptive and can have strong implications for the coronal magnetic field and the heliosphere.

Example of an eruptive prominence on AR 11991, observed on March 10, 2014 above the southeast limb of the Sun in 4 spectral lines: from left to right, Na I 587 nm (08:25:17 UT), H I 656 nm (08:21:53 UT), Ca II 854 nm (08:19:35 UT), and He I 1083 nm (08:15:59 UT).

Image credit: Jan Rybak (AISAS)