  Recently, two gravitational wave (GW) signals, named as GW150914 and
GW151226, have been detected by the two LIGO detectors. Although both signals
were identified as originating from merging black hole (BH) binaries, GWs from
systems containing neutron stars (NSs) are also expected to be detected in the
near future by the Advanced detector network. In this work, we assess the
accuracy in measuring the NS mass ($M_{ns}$) for the GWs from BH-NS binaries
adopting the Advanced LIGO sensitivity with a signal-to-noise ratio of 10. By
using the Fisher matrix method, we calculate the measurement errors ($\sigma$)
in $M_{ns}$ assuming the NS mass of $1 \leq M_{ns}/M_{\odot} \leq 2$ and low
mass BHs with the range of $4 \leq M_{bh}/M_{\odot} \leq 10$. We used the
TaylorF2 waveform model where the spins are aligned with the orbital angular
momentum, but here we only consider the BH spins. We find that the fractional
errors ($\sigma/M_{ns} \times 100$) are in the range of $10\% - 50\%$ in our
mass region for a given dimensionless BH spin as $\chi_{bh} = 0$. The errors
tend to increase as the BH spin increases, and this tendency is stronger for
higher NS masses (or higher total masses). In particular, for the highest mass
NSs ($M_{ns}=2~M_{\odot}$), the errors $\sigma$ can be larger than the true
value of $M_{ns}$ if the dimensionless BH spin exceeds $\sim 0.6$.
