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Very massive primordial stars ($140 M_{\odot} < M < 260 M_{\odot}$) aresupposed to end their lives as pair-instability supernovae. Such an event canbe traced by a typical chemical signature in low metallicity stars, but at thepresent time, this signature is lacking in the extremely metal-poor stars weare able to observe. Does it mean that those very massive objects did not form,contrarily to the primordial star formation scenarios? Could they avoid thistragical fate?  We explore the effects of rotation, anisotropic mass loss and magnetic fieldson the core size of a very massive Population III model, in order to check ifits mass is sufficiently modified to prevent the pair instability.  We obtain that a Population III model of $150 M_{\odot}$ with$\upsilon/\upsilon_{\rm crit}=0.56$ computed with the inclusion of windanisotropy and Tayler-Spruit dynamo avoids the pair instability explosion.

Can very massive stars avoid Pair-instability Supernovae?