[MOVIE] Chromospheric heating by flux emergence (2/2)
Chromospheric heating by flux emergence (2/2)
Swedish 1-m Solar Telescope
Observations reveal that the solar chromosphere radiates more energy than it absorbs in areas where the magnetic field is strong. The origin of this surplus energy must be in the photosphere or below. Physical processes involved in transporting this energy to the chromosphere, and the dissipation there, are made more efficient by the presence of magnetic fields. However, the precise role of the various processes is not known.
This movie shows the temporal evolution of active region 12593 as seen at different heights in the atmosphere. Vigorous magnetic flux emergence is taking place, leaving clear imprints in all atmospheric layers sampled by the observations. Panel a depicts the deep photosphere. Panel b gives maps of the longitudinal field in the photosphere. White represents fields pointing to the observer, black fields pointing away from the observer. Panel c shows the horizontal component of the magnetic field in the photosphere. Panels d and e show images taken at different wavelengths within the Ca II K line. They sample the lower and the mid chromosphere. Panel f displays images taken at the center of the H-alpha line, to monitor the upper chromosphere. The lower two panels show observations in the Ca II 8542 Å line, which is formed in the chromosphere.