Protuberanssit

Protuberanssit are large, bright features extending outward from the Sun's surface, often in a loop shape. They are composed of plasma, which is ionized gas, and are anchored in the Sun's atmosphere. These structures can be many thousands of kilometers long and are one of the most prominent and visually striking phenomena observed on the Sun.

The formation of protuberances is directly linked to the Sun's magnetic field. Intense magnetic field lines originating from sunspots can trap and channel the hot plasma, causing it to rise above the Sun's surface. The plasma is heated to temperatures of tens of thousands of degrees Celsius. Protuberances can persist for days or even weeks, gradually changing shape and size.

When a protuberance becomes unstable, it can erupt, releasing a large amount of energy and plasma into space. These eruptions are known as coronal mass ejections (CMEs). CMEs can have significant impacts on Earth, potentially disrupting satellite communications, power grids, and even posing a hazard to astronauts. Studying protuberances and CMEs helps scientists understand the Sun's behavior and its influence on the space environment around Earth. Observing protuberances typically requires specialized instruments like coronagraphs, which block out the Sun's bright disk to reveal fainter features in its atmosphere.