päikeselaikude

Päikeselaigud are temporary phenomena on the Sun's photosphere that appear as darker spots compared to surrounding areas. They are caused by intense magnetic activity which inhibits convection, a process that transports heat from the Sun's interior to its surface. This reduction in heat transfer results in cooler surface temperatures within the sunspot, making them appear darker. Sunspots are not stationary and can move across the solar surface due to the Sun's rotation. They also vary in size and can persist for days or even weeks.

The number and distribution of sunspots follow a cycle known as the solar cycle, which typically lasts about 11 years. During the peak of the solar cycle, known as solar maximum, the number of sunspots is highest. Conversely, during solar minimum, sunspots are rare. This cycle is closely linked to the Sun's magnetic field reversals. Sunspots are often observed in groups, and these groups can be associated with other solar phenomena such as solar flares and coronal mass ejections, which are energetic releases of radiation and plasma from the Sun. Historically, the observation of sunspots has played a significant role in our understanding of solar physics and the Sun's dynamic nature.