  In our self-similar, analytical, magneto-hydrodynamic (MHD)
accretion-ejection solution, the density at the base of the outflow is
explicitly dependent on the disk accretion rate - a unique property of this
class of solutions. We had earlier found that the ejection index $p >\sim 0.1
(\dot{M}_{acc} \propto r^p ) $ is a key MHD parameter that decides if the flow
can cause absorption lines in the high resolution X-ray spectra of black hole
binaries. Here we choose 3 dense warm solutions with $p = 0.1, 0.3, 0.45$ and
carefully develop a methodology to generate spectra which are convolved with
the Athena and XRISM response functions to predict what they will observe
seeing through such MHD outflows. In this paper two other external parameters
were varied - extent of the disk, $\rm{r_o|_{max}} = 10^5, \, 10^6 \,\,
\rm{r_G}$, and the angle of the line of sight, $i \sim 10 - 25^{\circ}$.
Resultant absorption lines (H and He-like Fe, Ca, Ar) change in strength and
their profiles manifest varying degrees of asymmetry. We checked if a) the
lines and ii) the line asymmetries are detected, in our suit of synthetic
Athena and XRISM spectra. Our analysis shows that Athena should detect the
lines and their asymmetries for a standard 100 ksec observation of a 100 mCrab
source - lines with equivalent width as low as a few eV should be detected if
the 6-8 keV counts are larger than $10^4 - 10^5$ even for the least favourable
simulated cases.
