  HD 176465 is a binary system whose both components are solar-like pulsators
and whose oscillation frequencies were observed by the \kepler\ mission. In
this paper we have modeled the asteroseismic and spectroscopic data of the
stars, and have determined their convection-zone helium abundances using the
signatures left by the He{\sc ii} ionization zone on the mode frequencies. As
expected we find that the components of the binary have the same age within
uncertainties ($3.087 \pm 0.580$ Gyr and $3.569 \pm 0.912$ Gyr); they also have
the same initial helium abundance (Y$_{\mathrm{init}}$=0.253 $\pm$ 0.006 and
0.254 $\pm$ 0.008). Their current metallicity ([Fe/H]=$-0.275 \pm 0.04$ and
$-0.285 \pm 0.04$) is also the same within errors. Fits to the signature of the
He{\sc ii} acoustic glitch yields current helium abundances of $Y_{\rm A} =
0.224 \pm 0.006$ and $Y_{\rm B} = 0.233 \pm 0.008$ for the two components.
Analyzing the complete ensemble of models generated for this investigation we
find that both the amplitude and acoustic depth of the glitch signature arising
from the second helium ionization zone and the base of the convection zone (CZ)
are functions of mass. We show that the acoustic depths of these glitches are
positively correlated with each other. The analysis can help us to detect the
internal structure and constrain the chemical compositions.
