Near-solar metallicity ( and low-redshift ) Pair-Instability Supernova ( PISN ) candidates challenge stellar evolution models .
Indeed , at such a metallicity , even an initially very massive star generally loses so much mass by stellar winds that it will avoid the electron-positron pair-creation instability .
We use recent results showing that a magnetic field at the surface of a massive star can significantly reduce its effective mass-loss rate to compute magnetic models of very massive stars ( VMSs ) at solar metallicity and explore the possibility that such stars end as PISNe .
We implement the quenching of the mass loss produced by a surface dipolar magnetic field into the Geneva stellar evolution code and compute new stellar models with an initial mass of 200 M _ { \sun } at solar metallicity , with and without rotation .
It considerably reduces the total amount of mass lost by the star during its life .
For the non-rotating model , the total ( CO-core ) mass of the models is 72.8 M _ { \sun } ( 70.1 M _ { \sun } ) at the onset of the electron-positron pair-creation instability .
For the rotating model , we obtain 65.6 M _ { \sun } ( 62.4 M _ { \sun } ) .
In both cases , a significant fraction of the internal mass lies in the region where pair instability occurs in the \log ( T ) - \log ( \rho ) plane .
The interaction of the reduced mass loss with the magnetic field efficiently brakes the surface of the rotating model , producing a strong shear and hence a very efficient mixing that makes the star evolve nearly homogeneously .
The core characteristics of our models indicate that solar metallicity models of magnetic VMSs may evolve to PISNe ( and pulsation PISNe ) .