supergranular

Supergranulation is a phenomenon observed in the photosphere of the Sun, the outermost layer of the Sun's atmosphere. It is characterized by the presence of large, convective cells that are significantly larger than the smaller granulation cells typically observed on the Sun's surface. These supergranules are approximately 30,000 kilometers in diameter and have lifespans of about 24 hours. They are formed by the upward movement of hot plasma from the Sun's interior, which then cools and sinks back down, creating a cycle of convection.

Supergranulation plays a crucial role in the dynamics of the Sun's magnetic field. The boundaries of supergranules are associated with strong magnetic fields, which can lead to the formation of active regions and sunspots. These magnetic fields are thought to be generated by the interaction of the convective flows within the supergranules and the Sun's differential rotation.

The study of supergranulation is important for understanding the Sun's magnetic activity and its impact on space weather. By observing and modeling supergranulation, scientists can gain insights into the processes that drive the Sun's magnetic field and the mechanisms behind solar flares and coronal mass ejections.