Young neutron stars ( NSs ) born in core-collapse explosions are promising candidates for the central engines of fast radio bursts ( FRBs ) , since the first localized repeating burst FRB 121102 happens in a star forming dwarf galaxy , which is similar to the host galaxies of superluminous supernovae ( SLSNe ) and long gamma-ray bursts ( LGRBs ) .
However , FRB 180924 and FRB 190523 are localized to massive galaxies with low rates of star formation , compared with the host of FRB 121102 .
Meanwhile , the offsets between the bursts and host centers are about 4 kpc and 29 kpc for FRB 180924 and FRB 190523 , respectively .
These properties of hosts are similar to short gamma-ray bursts ( SGRBs ) , which are produced by mergers of binary neutron star ( BNS ) or neutron star-black hole ( NS-BH ) .
Therefore , the NSs powering FRBs may be formed in BNS mergers .
In this paper , we study the BNS merger rates , merger times , and predict their most likely merger locations for different types of host galaxies using population synthesis method .
We find that the BNS merger channel is consistent with the recently reported offsets of FRB 180924 and FRB 190523 .
The offset distribution of short GRBs is well reproduced by population synthesis using galaxy model which is similar to GRB hosts .
The event rate of FRBs ( including non-repeating and repeating ) , is larger than those of BNS merger and short GRBs , which requires a large fraction of observed FRBs emitting several bursts .
Using curvature radiation by bunches in NS magnetospheres , we also predict the observational properties of FRBs from BNS mergers , including the dispersion measure , and rotation measure .
At late times ( t \geq 1 yr ) , the contribution to dispersion measure and rotation measure from BNS merger ejecta could be neglected .