only originated from mode transmission/conversion. The 2.5D simulations of @KhoCal11aa [@KhoCal12aa] similarly impose a deep fast wave driver (at $-5$ Mm). In the current SPARC simulations though, a shallow more realistic solar driver is placed at $z=-0.156$ Mm, and this excites both acoustic and magnetic oscillations directly (see Figure \[fig:FzVz\]). Consequently, some portion of the magnetic wave energy fluxes at the top may have travelled directly along the fast and Alfvén dispersion relation loci rather than tunnelling from the fast branch. Nevertheless, the correspondence between the flux maps presented here and in @CalGoo08aa is striking.

![Pure field-aligned acoustic and Alfvén fluxes $F_{\parallel\rm ac}$ (left column) and $F_{\rm Alf}$ (right column) for the case $B_0=1$ kG, $\nu=5$ mHz, $k_h=1$ 0.75, and 0.5 $\rm Mm^{-1}$ (top to bottom).[]{data-label="fig:Fpar"}](\figdir/Fparalf_5mHz_1kG){width="\hsize"}

![image](\figdir/tau_PSC_5mHz){width=".4\hsize"} ![image](\figdir/tau_PSC_5mHz_1kG){width=".4\hsize"}\
![image](\figdir/tau_PSC_3mHz){width=".4\hsize"} ![image](\figdir/tau_PSC_3mHz_1kG){width=".4\hsize"}

As the magnetic field inclination $\theta$ increases toward $90^\circ$, the vertical acoustic and magnetic fluxes obviously diminish since asymptotically, as $z_f\to\infty$, both are identically field-aligned. They therefore give a biased view of energy loss rates; even for purely horizontal magnetic field, the parallel acoustic and Alfvén waves take energy away (horizontally) from the sites of mode conversion. Using vector identities, it is easily shown that ${{{\bmath{F}}}}_{\rm mag} = p_{\rm mag}{{\bmath{v}}}+{{{\bmath{b}}}}{{\bmath{\cdot}}}{{\bmath{v}}}\,{{\bmath{B}}}_0/\mu_0$, 