päikeselaigud

Päikeselaigud, known in English as sunspots, are temporary phenomena on the Sun's photosphere that appear as darker spots than the surrounding areas. They are regions of reduced surface temperature caused by concentrations of magnetic field flux that inhibit convection. These magnetic fields are significantly stronger than in the surrounding photosphere. While still incredibly hot, sunspots are cooler than the surrounding plasma, which is why they appear dark by comparison.

The number of sunspots visible on the Sun fluctuates in an approximately 11-year cycle, known as the solar cycle. This cycle is characterized by periods of high solar activity, where sunspots are abundant, and periods of low activity, where few or no sunspots are visible. Sunspots can vary in size, from small pores just a few hundred kilometers across to large regions spanning tens of thousands of kilometers.

Sunspots are often found in pairs or groups with opposite magnetic polarities. The formation of sunspots is closely linked to solar flares and coronal mass ejections, which are explosive releases of energy and plasma from the Sun's atmosphere. These events can have significant impacts on Earth, affecting satellite operations, radio communications, and power grids. Studying sunspots helps scientists understand the Sun's magnetic activity and its influence on space weather.