GRB 090510: A GENUINE SHORT GRB FROM A BINARY NEUTRON STAR COALESCING INTO A KERR–NEWMAN BLACK HOLE

In a new classification of merging binary neutron stars (NSs) we separate short gamma-ray bursts (GRBs) into two subclasses. The ones with Eiso  10 52 erg coalesce to form a massive NS and are indicated as short gamma-ray flashes (S-GRFs). The hardest, with Eiso  10 52 erg, coalesce to form a black hole (BH) and are indicated as genuine short GRBs (S-GRBs). Within the fireshell model, S-GRBs exhibit three different components: the proper GRB (P-GRB) emission, observed at the transparency of a self-accelerating baryon-e+e- plasma; the prompt emission, originating from the interaction of the accelerated baryons with the circumburst medium; and the highenergy (GeV) emission, observed after the P-GRB and indicating the formation of a BH. GRB 090510 gives the first evidence for the formation of a Kerr BH or, possibly, a Kerr–Newman BH. Its P-GRB spectrum can be fitted by a convolution of thermal spectra whose origin can be traced back to an axially symmetric dyadotorus. A large value of the angular momentum of the newborn BH is consistent with the large energetics of this S-GRB, which reach in the 1–10,000keV range Eiso = 3.95  0.21 ´ 10 ( ) 52 erg and in the 0.1–100GeV range ELAT = 5.78  0.60 ´ 10 ( ) 52 erg, the most energetic GeV emission ever observed in S-GRBs. The theoretical redshift zth = 0.75  0.17 that we derive from the fireshell theory is consistent with the spectroscopic measurement z = 0.903  0.003, showing the self-consistency of the theoretical approach. All S-GRBs exhibit GeV emission, when inside the Fermi-LAT field of view, unlike S-GRFs, which never evidence it. The GeV emission appears to be the discriminant for the formation of a BH in GRBs, confirmed by their observed overall energetics.