  Stellar-mass black holes (BHs) surrounded by neutrino-dominated accretion
flows (NDAFs) are the plausible candidates to power gamma-ray bursts (GRBs) via
neutrinos emission and their annihilation. The progenitors of short-duration
GRBs (SGRBs) are generally considered to be compact binaries mergers. According
to the simulation results, the disk mass of the NDAF has been limited after
merger events. We can estimate such disk mass by using the current SGRB
observational data and fireball model. The results show that the disk mass of a
certain SGRB mainly depends on its output energy, jet opening angle, and
central BH characteristics. Even for the extreme BH parameters, some SGRBs
require massive disks, which approach or exceed the limits in simulations. We
suggest that there may exist alternative magnetohydrodynamic processes or some
mechanisms increasing the neutrino emission to produce SGRBs with the
reasonable BH parameters and disk mass.
