  The post-merger gravitational wave (GW) radiation of the remnant formed in
the binary neutron star (BNS) coalescence has not been directly measured, yet.
We show in this work that the properties of the BNS involved in GW170817,
additionally constrained by PSR J0030+0451, the lower limit on the maximum
gravitational mass of non-rotating neutron star (NS) and some nuclear data, are
in favor of strong post-merger GW radiation. This conclusion applies to the
mergers of Galactic BNS systems as well. Significant post-merger GW radiation
is also preferred to improve the consistency between the maximum gravitational
mass of the non-rotating NS inferred from GW170817/GRB170817A/AT2017gfo and the
latest mass measurements of pulsars. The prominent post-merger gravitational
radiation of GW170817-like events are expected to be detectable by advanced
LIGO/Virgo detectors in the next decade and then shed valuable lights on the
properties of the matter in the extremely high density.
