  The binary star Par 1802 in the Orion Nebula presents an interesting puzzle
in the field of stellar dynamics and evolution. Binary systems such as Par 1802
are thought to form from the same natal material and thus the stellar members
are expected to have very similar physical attributes. However, Par 1802's
stars have significantly different temperatures despite their identical (within
$3\%$) masses of about $0.39$ solar mass. The leading proof-of-concept idea is
that a third companion gravitationally induced the two stars to orbit closer
than their Roche-limit, which facilitated heating through tidal effects. Here
we expand on this idea and study the three-body dynamical evolution of such a
system, including tidal and pre-main-sequence evolution. We also include tidal
heating and mass transfer at the onset of Roche-limit Crossing. We show, as a
proof-of-concept, that mass transfer combined with tidal heating can naturally
explain the observed temperature discrepancy. We also predict the orbital
configuration of the possible tertiary companion. Finally we suggest that the
dynamical evolution of such a system has pervasive consequences. We expect an
abundance of systems to undergo mass transfer during their pre-main-sequence
time, which can cause temperature differences.
