Using smoothed particle hydrodynamics , we numerically simulate steady state accretion discs for Cataclysmic Variable Dwarf Novae systems that have a secondary-to-primary mass ratio 0.35 \leq q \leq 0.55 .
After these accretion discs have come to quasi-equilibrium , we rotate each disc out of the orbital plane by \delta = ( 1 , 2 , 3 , 4 , 5 , or 20 ) ^ { o } to induce negative superhumps .
For accretion discs tilted 5 ^ { o } , we generate light curves and associated Fourier transforms for an atlas on negative superhumps and retrograde precession .
Our simulation results suggest that accretion discs need to be tilted more than three degrees for negative superhumps to be statistically significant .
We also show that if the disc is tilted enough such that the gas stream strikes a disc face , then a dense cooling ring is generated near the radius of impact .

In addition to the atlas , we study these artificially tilted accretion discs to find the source to negative superhumps .
Our results suggest that the source is additional light from innermost disc annuli , and this additional light waxes and wanes with the amount of gas stream overflow received as the secondary orbits .
The nodes , where the gas stream transitions from flowing over to under the disc rim ( and vice versa ) , precess in the retrograde direction .