Now we can use GONG to peer into the solar interior from Earth.

Associated with sunspots are coronal loops, loops of magnetic flux, upwelling from the solar interior.

The differential profile of the surface was thought to extend into the solar interior as rotating cylinders of constant angular momentum.

Flares occur in active regions around sunspots, where intense magnetic fields penetrate the photosphere to link the corona to the solar interior.

The solar interior is not directly observable, and the Sun itself is opaque to electromagnetic radiation.

Another example of convective overshoot is at the base of the convection zone in the solar interior.

This affects the heat transfer rate and the temperature of the solar interior which can be indirectly measured by helioseismology.

Local helioseismology provides a three-dimensional view of the solar interior, which is important to understand large-scale flows, magnetic structures, and their interactions in the solar interior.

An inverse problem must then be solved to infer the local structure and dynamics of the solar interior.

Sunspots, on the other hand, are produced from a strong toroidal (longitudinally directed) magnetic field within the solar interior.