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 .