The correlation between Lyalpha absorption in the spectra of quasar pairs can be used to measure the transverse distance scale at zsimilar to2, which is sensitive to the cosmological constant (Omega(Lambda)) or other forms of vacuum energy. Using hydro-PM simulations, I compute the three-dimensional power spectrum of the Lyalpha forest flux, P-F(k), from which the redshift-space anisotropy of the correlation can be obtained. I compute directly the linear theory bias parameters of the Lyalpha forest, potentially allowing simulation results to be extended to arbitrarily large scales. I investigate the dependence of P-F(k) on the primordial power spectrum, the temperature-density relation of the gas, and the mean flux decrement, finding that the redshift-space anisotropy is relatively insensitive to these parameters. A table of results is provided for different parameter variations. I investigate the constraint that can be obtained on Omega(Lambda) using quasars from a large survey. Assuming 13(theta/1')(2) pairs at a separation of less than theta and including separations less than 10', a measurement to less than or similar to5% can be made if simulations can predict the redshift-space anisotropy with less than or similar to5% accuracy or to less than or similar to10% if the anisotropy must be measured from the data. The Sloan Digital Sky Survey (SDSS) will obtain spectra for a factor of similar to5 fewer pairs than this, so follow-up observations of fainter pair candidates will be necessary. I discuss the requirements on the spectral resolution and signal-to-noise ratio (SDSS quality spectra are sufficient). I find that a box size of similar to40 h(-1) Mpc and a resolution of similar to40 h(-1) kpc are necessary for convergence of the calculations to less than or similar to5% on all relevant scales, although somewhat poorer resolution can be used for large scales.