We develop the halo model of large-scale structure to include triaxial dark matter haloes and their intrinsic alignments .
As a direct application we derive general expressions for the two-point correlation function and the power spectrum .
We then focus on the power spectrum and numerically solve the general expressions for two different models of the triaxial profiles .
The first is a toy-model that allows us to isolate the dependence of clustering on halo shape alone and the second is the more realistic profile model of Jing & Suto ( 25 ) .
In both cases , we find that the effect of triaxiality is manifest as a suppression of power at the level of \sim 5 \% on scales k \sim 1 - 10 h { Mpc } ^ { -1 } , which in real space corresponds to the virial radii of clusters .
When considered by mass , we find that for the first model the effects are again apparent as a suppresion of power and that they are more significant for the high mass haloes .
For the Jing & Suto model , we find a suppression of power on large scales followed by a sharp amplification on small scales at the level of \sim 10 - 15 \% .
Interstingly , when averaged over the entire mass function this amplification effect is surpressed .
We also find for the 1-Halo term on scales k < 10 h { Mpc } ^ { -1 } , that the power is dominated by ellipsoidal haloes with semi-minor to semi-major axis ratios a / c < 0.7 .

One of the important features of our formalism is that it allows for the self-consistent inclusion of the intrinsic alignments of haloes .
The alignments are specified through the correlation function of halo seeds .
We develop a useful toy model for this and then make estimates of the alignment contribution to the power spectrum .
Further , through consideration of the ( artificial ) case where all haloes are perfectly aligned , we calculate the maximum possible contribution to the clustering .
We find the hard limit of < 10 \% .
Subject to further scrutiny , the proposed toy-model may serve as a means for linking the actual observed intrinsic alignments of galaxies to physical quantities of interest .