Аннотация
The common envelope binary interaction occurs when a star transfers mass onto
a companion that cannot fully accrete it. The interaction can lead to a merger
of the two objects or to a close binary. The common envelope interaction is the
gateway of all evolved compact binaries, all stellar mergers and likely many of
the stellar transients witnessed to date. Common envelope simulations are
needed to understand this interaction and to interpret stars and binaries
thought to be the byproduct of this stage. At this time, simulations are unable
to reproduce the few observational data available and several ideas have been
put forward to address their shortcomings. The need for more definitive
simulation validation is pressing, and is already being fulfilled by
observations from time-domain surveys. In this article, we present an initial
method and its implementation for post-processing grid-based common envelope
simulations to produce the light-curve so as to compare simulations with
upcoming observations. Here we implemented a zeroth order method to calculate
the light emitted from common envelope hydrodynamic simulations carried out
with the 3D hydrodynamic code Enzo used in uni-grid mode. The code implements
an approach for the computation of luminosity in both optically thick and
optically thin regimes and is tested using the first 135 days of the common
envelope simulation of Passy et al. (2012), where a 0.8 solar masses red giant
branch star interacts with a 0.6 solar masses companion. This code is used to
highlight two large obstacles that need to be overcome before realistic light
curves can be calculated. We explain the nature of these problems and the
attempted solutions and approximations in full detail to enable the next step
to be identified and implemented. We also discuss our simulation in relation to
recent data of transients identified as common envelope interactions.
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