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On the ground of the large number of gamma-ray bursts (GRBs) detected withcosmological redshift, we classified GRBs in seven subclasses, all with binaryprogenitors originating gravitational waves (GWs). Each binary is composed bycombinations of carbon-oxygen cores (CO$_{\rm core}$), neutron stars (NSs),black holes (BHs) and white dwarfs (WDs). The long bursts, traditionallyassumed to originate from a BH with an ultra-relativistic jetted emission, notemitting GWs, have been subclassified as (I) X-ray flashes (XRFs), (II)binary-driven hypernovae (BdHNe), and (III) BH-supernovae (BH-SNe). They areframed within the induced gravitational collapse (IGC) paradigm with progenitora CO$_{\rm core}$-NS/BH binary. The supernova (SN) explosion of the CO$_{\rmcore}$ triggers an accretion process onto the NS/BH. If the accretion does notlead the NS to its critical mass, an XRF occurs, while when the BH is presentor formed by accretion, a BdHN occurs. When the binaries are not disrupted,XRFs lead to NS-NS and BdHNe lead to NS-BH. The short bursts, originating inNS-NS, are subclassified as (IV) short gamma-ray flashes (S-GRFs) and (V) shortGRBs (S-GRBs), the latter when a BH is formed. There are (VI) ultra-short GRBs(U-GRBs) and (VII) gamma-ray flashes (GRFs), respectively formed in NS-BH andNS-WD. We use the occurrence rate and GW emission of these subclasses to assesstheir detectability by Advanced LIGO-Virgo, eLISA, and resonant bars. Wediscuss the consequences of our results in view of the announcement of theLIGO-Virgo Collaboration of the source GW 170817 as being originated by aNS-NS.

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