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The common envelope binary interaction occurs when a star transfers mass ontoa companion that cannot fully accrete it. The interaction can lead to a mergerof the two objects or to a close binary. The common envelope interaction is thegateway of all evolved compact binaries, all stellar mergers and likely many ofthe stellar transients witnessed to date. Common envelope simulations areneeded to understand this interaction and to interpret stars and binariesthought to be the byproduct of this stage. At this time, simulations are unableto reproduce the few observational data available and several ideas have beenput forward to address their shortcomings. The need for more definitivesimulation validation is pressing, and is already being fulfilled byobservations from time-domain surveys. In this article, we present an initialmethod and its implementation for post-processing grid-based common envelopesimulations to produce the light-curve so as to compare simulations withupcoming observations. Here we implemented a zeroth order method to calculatethe light emitted from common envelope hydrodynamic simulations carried outwith the 3D hydrodynamic code Enzo used in uni-grid mode. The code implementsan approach for the computation of luminosity in both optically thick andoptically thin regimes and is tested using the first 135 days of the commonenvelope simulation of Passy et al. (2012), where a 0.8 solar masses red giantbranch star interacts with a 0.6 solar masses companion. This code is used tohighlight two large obstacles that need to be overcome before realistic lightcurves can be calculated. We explain the nature of these problems and theattempted solutions and approximations in full detail to enable the next stepto be identified and implemented. We also discuss our simulation in relation torecent data of transients identified as common envelope interactions.

Common envelope light-curves - I. grid-code module calibration