  The proposed space gravitational wave (GW) detector LISA has potential to
detect stellar-mass black hole binaries (BBHs). The majority of the detected
BBHs are expected to emit nearly monochromatic GWs, whose frequency evolution
will be efficiently described by Taylor expansions. We study the measurability
of the associated time derivative coefficients of the frequencies, by extending
a recent work based on a simplified Fisher matrix analysis. Additionally, we
provide qualitative discussions on how to extract astrophysical information,
such as orbital eccentricity and tertiary perturbation, from the observed
derivative coefficients.
