  Observation of blue-shifted X-ray absorption lines indicates the presence of
wind from the accretion disk in X-ray binaries. Magnetohydrodynamic (MHD)
driving is one of the possible wind launching mechanisms. Recent theoretical
development makes magnetic accretion-ejection self-similar solutions much more
generalized, and wind can be launched even at much lower magnetization compared
to equipartition value, which was the only possibility beforehand. Here, we
model the transmitted spectra through MHD driven photoionized wind - models
which have different values of magnetizations. We investigate the possibility
of detecting absorption lines by the upcoming instruments XRISM and Athena.
Attempts are made to find the robustness of the method of fitting asymmetric
line profiles by multiple Gaussians. We use photoionization code XSTAR to
simulate the transmitted model spectra. Fake observed spectra are finally
produced by convolving model spectra with instruments' responses. Since the
line asymmetries are apparent in the convolved spectra as well, this can be
used as an observable diagnostic to fit for, in future XRISM and Athena
spectra. We demonstrate some amount of rigor in assessing the equivalent widths
of the major absorption lines, including the Fe XXVI Ly$\alpha$ doublets which
can be clearly distinguished in the superior quality, future high resolution
spectra. Disk magnetization becomes another crucial MHD variable that can
significantly alter the absorption line profiles. Low magnetization pure MHD
outflow models are dense enough to be observed by the existing or upcoming
instruments. Thus these models become simpler alternatives to MHD-thermal
models. Fitting with multiple Gaussians is a promising method to handle
asymmetric line profiles, as well as the Fe XXVI Ly$\alpha$ doublets.
