- Conference date: 8–10 October 2008
- Location: Seoul (South Korea)
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. Even though low‐mass stars are the most numerous to come out of the star formation processes, there are only a few examples of dynamically measured masses for young objects. We present the light curve modeling of two eclipsing binary systems found in the Orion nebular cluster and therefore expected to have an age of a few million years. For the first system, J05352184‐20130546085, we measured substellar masses for both components, making them the first dynamic masses of pre‐main sequence brown dwarfs to be determined. The components of the second system presented, Parenago 1802, have very similar masses below half a solar mass, which allows us to test the basic hypothesis that two stars of the same mass and age will evolve identically in every way.
- Early stellar evolution
- Eclipsing binaries
- Star formation
- Stellar evolution
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