Abstract
Pre-main sequence stellar evolutionary models allow the understanding of star formation processes and early stellar evolution. A comparison of these evolutionary models and fundamental stellar parameters, directly determined through observations, provides useful data for testing the predictions of existing models and, what's more, provides them with an empirical mass calibration.
A thorough spectroscopic and photometric analysis of eclipsing binary systems yields highly accurate properties of the system and of its stellar components, in such a manner that they are determined independently of their distance and other theoretical assumptions.
The newly discovered system is an example of very young, low-mass eclipsing binary member of the Orion Nebula Cluster. Therefore, it has a likely age of only a few million years. The components of the newly discovered system are both brown dwarfs, with masses of 0.054 and 0.034 solar masses, respectively, making this system the first example of an eclipsing brown dwarf pair.
