of this paper is to look for correspondences between acoustic and magnetic wave losses on the one hand, and ‘travel time’ shifts on the other, and thereby to verify that the seismology of the wounded Sun depends on propagation, transmission, and conversion in overlying active region atmospheres. [We introduce a directionally filtered time-distance approach[^3] to simulation data that is directly extensible to real helioseismic data, and thereby envisage a Directional-Time-Distance (DTD) seismology sensitive to magnetic field orientation. In Section \[sec:BVP\], the DTD results are verified using the Boundary Value approach of @Cal09ab.]{}

[ The purpose of this paper is to demonstrate that the above mode conversion scenarios actually operate in the solar context; to survey how they depend on field inclination $\theta$ and wave orientation $\phi$; and to assess the utility of DTD in discerning directional magnetic effects. To this end, we explore only vertical atmospheric stratification, characterized by density scale heights of order 0.15 Mm, and ignore magnetic field inhomogeneity, which in sunspots has scale length of order many Mm. A subsequent paper will address wave simulations in realistic sunspot models using DTD. This is not to say though that flux tubes are not important to wave propagation, though 