On the rate and on the gravitational wave emission of short and long GRBs

On the ground of the large number of gamma-ray bursts(GRBs)detected with cosmological redshift, we classifiedGRBs in seven subclasses, all with binary progenitors which emit gravitational waves(GWs). Each binary iscomposed of combinations of carbon–oxygen cores(COcore), neutron stars(NSs), black holes(BHs), and whitedwarfs(WDs). The long bursts, traditionally assumed to originate from a BH with an ultrarelativistic jettedemission, not emitting GWs, have been subclassified as(I)X-rayflashes(XRFs),(II)binary-driven hypernovae(BdHNe), and(III)BH–supernovae(BH–SNe). They are framed within the induced gravitational collapseparadigm with a progenitor COcore–NS/BH binary. The SN explosion of the COcoretriggers an accretion processonto the NS/BH. If the accretion does not lead the NS to its critical mass, an XRF occurs, while when the BH ispresent or formed by accretion, a BdHN occurs. When the binaries are not disrupted, XRFs lead to NS–NS andBdHNe lead to NS–BH. The short bursts, originating in NS–NS, are subclassified as(IV)short gamma-rayflashes(S-GRFs)and(V)short GRBs(S-GRBs), the latter when a BH is formed. There are(VI)ultrashort GRBs(U-GRBs)and(VII)gamma-rayflashes(GRFs)formed in NS–BH and NS–WD, respectively. We use theoccurrence rate and GW emission of these subclasses to assess their detectability by Advanced LIGO-Virgo,eLISA, and resonant bars. We discuss the consequences of our results in view of the announcement of the LIGO/Virgo Collaboration of the source GW 170817 as being originated by an NS–NS.