Magnetic braking is a theory that explains the loss of stellar angular momentum due to material captured by the stellar magnetic field and released at great distance from the surface of the star. It plays an important role in the evolution of binary star systems.
The currently accepted theory of the evolution of the solar system indicates that the solar system originates from a contracting gas cloud. As the cloud contracts, the angular momentum {\ displaystyle L} L must be preserved. Any small net rotation of the cloud will cause the rotation to increase as the cloud collapses, forcing the material into a rotating disk. In the dense center of this disk a protostar forms, that obtains heat of the gravitational energy of the collapse. As the collapse continues, the rotational speed can increase to the point where the prototype of accumulation can break due to the centrifugal force at the equator.
Therefore, the rotation rate should be slowed during the first 100,000 years of star life to avoid this scenario. One possible explanation for braking is the interaction of the magnetic field of the protostar with the stellar wind. In the case of our own Sun, when the angular moments of the planets are compared with those of the Sun, the Sun has less than 1% of its supposed angular momentum. In other words, the Sun has slowed its spin while the planets have not.