Branes in Supernova Shells

This paper is firstly intended to review shortly the most recent developments and ideas resulting from the necessity of having a scale at which gravitation to unify the other fundamental forces. With the declared intention of predicting an in situ distinct possibility for Kaluza-Klein gravitons formation in the supernova shell we are using state of the art simulations (Langer et al. 1999; ud-Doula & Owocki 2002; ud-Doula & Owocki 2003; ud-Doula 2004) for massive stellar winds to infer that the supernova shock which will hit such winds will meet a non-isotropic and non-homogeneous matter distribution with a very distinct geometry. By linking this to the mechanism of particle shock acceleration at cosmic ray energies (Fermi acceleration) and the related spallation in the wind shell, the result is the creation of proper conditions for Kaluza-Klein gravitons formation in the supernova shell from neutrino secondary particles (cosmic ray spallation products) interacting with ∼ 1018 eV