The Sun’s ultra-hot upper atmosphere, called the corona, is a dynamic
environment where transient events occur on various scales. These events are
related to changes in the magnetic field structures. One spectacular evidence
of these magnetic structures are prominences.
Solar prominences – also known as filaments when viewed against the solar disk, are relatively cold and dense plasma clouds suspended in equilibrium by magnetic fields in the hot corona. Prominences can remain relatively quiet and stable for hours, days or even a month (quiescent), but as the magnetic fields that support them change, the instability triggers either a slow decay of emission (disparitions brusques) or a more active phenomenon, a prominence eruption.
Reference:
http://helioviewer.org/
Solar prominences – also known as filaments when viewed against the solar disk, are relatively cold and dense plasma clouds suspended in equilibrium by magnetic fields in the hot corona. Prominences can remain relatively quiet and stable for hours, days or even a month (quiescent), but as the magnetic fields that support them change, the instability triggers either a slow decay of emission (disparitions brusques) or a more active phenomenon, a prominence eruption.
Reference:
http://helioviewer.org/
No comments:
Post a Comment