Yes
They are solar prominences.
prominences
It has to be solar flares, supra-sunspots, solar wind, or prominences.
These loops are called penumbral fibrils. They are structures of hot gas in the sun's photosphere that connect different parts of sunspots, contributing to the magnetic activity and energy transfer within those regions.
The reddish loops of gas observed in sunspot regions are known as solar prominences. These prominences are large, bright features that extend outward from the Sun's surface, often associated with sunspots and magnetic field lines. They consist of hot plasma and can appear as arcs or loops, showcasing the Sun's magnetic activity. Their dynamic nature can lead to eruptions, contributing to solar flares and coronal mass ejections.
The reddish loops of gas that link parts of sunspot regions are known as solar prominences. These structures are made of plasma and can extend thousands of kilometers into the solar atmosphere, known as the corona. Prominences are often associated with the magnetic fields around sunspots and can be seen during solar eclipses or using specialized telescopes. Their dynamic nature can lead to eruptions, which are called solar flares.
Prominences are arcs of glowing gas that are anchored to the Sun's surface by magnetic fields. They are caused by the interaction between the Sun's magnetic field and its plasma atmosphere. Plasma flows along the magnetic field lines, giving rise to the appearance of solar prominences.
prominence
Solar prominences, they are loops of plasma captured by magnetic flux lines linking individual sunspots.
Solar prominences, they are loops of plasma captured by magnetic flux lines linking individual sunspots.
Magnetic field lines.
The reddish loops of gas that link parts of sunspot regions are known as solar prominences. These large, bright features extend outward from the Sun's surface and are composed of plasma, a hot ionized gas. Prominences are often associated with the Sun's magnetic field and can be seen during solar eclipses as they rise above the solar limb. They can vary in size and shape and may last from days to weeks before dissipating.