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Theoretical and observational evidences have been recently gained for atwo-fold classification of short bursts: 1) short gamma-ray flashes (S-GRFs),with isotropic energy $E_{iso}<10^{52}$~erg and no BH formation, and 2) theauthentic short gamma-ray bursts (S-GRBs), with isotropic energy$E_{iso}>10^{52}$~erg evidencing a BH formation in the binary neutron starmerging process. The signature for the BH formation consists in the on-set ofthe high energy ($0.1$--$100$~GeV) emission, coeval to the prompt emission, inall S-GRBs. No GeV emission is expected nor observed in the S-GRFs. In thispaper we present two additional S-GRBs, GRB 081024B and GRB 140402A, followingthe already identified S-GRBs, i.e., GRB 090227B, GRB 090510 and GRB 140619B.We also return on the absence of the GeV emission of the S-GRB 090227B, at anangle of $71^{\rm{o}}$ from the \textit{Fermi}-LAT boresight. All the correctlyidentified S-GRBs correlate to the high energy emission, implying nosignificant presence of beaming in the GeV emission. The existence of a commonpower-law behavior in the GeV luminosities, following the BH formation, whenmeasured in the source rest-frame, points to a commonality in the mass and spinof the newly-formed BH in all S-GRBs.

GRB 081024B and GRB 140402A: two additional short GRBs from binary neutron star mergers