  On the ground of the large number of gamma-ray bursts (GRBs) detected with
cosmological redshift, we classified GRBs in seven subclasses, all with binary
progenitors originating gravitational waves (GWs). Each binary is composed by
combinations of carbon-oxygen cores (CO$_{\rm core}$), neutron stars (NSs),
black holes (BHs) and white dwarfs (WDs). The long bursts, traditionally
assumed to originate from a BH with an ultra-relativistic jetted emission, not
emitting GWs, have been subclassified as (I) X-ray flashes (XRFs), (II)
binary-driven hypernovae (BdHNe), and (III) BH-supernovae (BH-SNe). They are
framed within the induced gravitational collapse (IGC) paradigm with progenitor
a CO$_{\rm core}$-NS/BH binary. The supernova (SN) explosion of the CO$_{\rm
core}$ triggers an accretion process onto the NS/BH. If the accretion does not
lead the NS to its critical mass, an XRF occurs, while when the BH is present
or 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 in
NS-NS, are subclassified as (IV) short gamma-ray flashes (S-GRFs) and (V) short
GRBs (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 and
NS-WD. We use the occurrence 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 a
NS-NS.
