Granulation
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Evolution of granulation in active region plage
Swedish 1-m Solar Telescope
The solar surface is characterized by the presence of an ever-lasting granulation pattern which is due to convective motions of the gas in the photosphere. Convection is a very efficient way to transport heat from the hot subsurface layers to the cooler surface above. Bright granules are convective cells in which hot gas rises into the solar photosphere and releases its heat before sinking back to the surface through the dark lanes surrounding them (the so-called intergranular lanes).
Granules on the solar surface occur in a variety of sizes and shapes. Their average diameter is on the order of 1500-2000 km. They are very dynamic, with lifetimes ranging from 5 to 10 minutes.
In the presence of strong magnetic fields, the properties of the granulation change. Granules are smaller and slightly larger. This is clearly seen in the movie, which shows granulation in an active region consisting of pores and many tiny magnetic elements located within the intergranular lanes, together with quiet Sun granulation in the upper part of the field of view.
The observations were taken with the Swedish 1m Solar Telescope in continuum intensity at 436.4 nm. The movie covers almost one hour of evolution of the granulation on the solar surface.
To download the movie, click HERE
Movie credit: Michiel van Noort and Luc Rouppe van der Voort (ITA, University of Oslo)
Text credit: Luis Bellot Rubio (IAA-CSIC)
Source: SST Galleries