Evolutionary Status of T Tauri Stars
Olga V. Eretnova, Alexander E. Dudorov

TL;DR
This study evaluates various pre-main sequence evolutionary models for T Tauri stars, finding good mass estimates for stars above 0.7 solar masses but significant discrepancies for lower-mass stars, confirming their pre-main sequence status.
Contribution
The paper systematically tests multiple evolutionary models against observational data of binary T Tauri stars, highlighting their accuracy and limitations across different mass ranges.
Findings
Models agree well for stars > 0.7 M_sun with ~10% error.
Significant divergence in isochrones for stars ≤ 0.7 M_sun.
Most T Tauri stars have ages below Kelvin-Helmholtz time.
Abstract
The problem of the determination of T Tauri stars masses and ages using their evolutionary status is discussed. We test of pre-main sequence evolutionary models of D'Antona \& Mazzitelli (1994), Dotter et al. (2008), Bressan et al. (2012) and Chen et al. (2014), Baraffe et al. (2015) using well determined observational parameters of 12 binary T Tauri stars (TTS) and 2 binary red dwarfs. It is shown that the masses derived using the tracks of all models are in good agreement with the masses obtained from the observations of TTS with masses (mean error ). Low-mass stars with have significantly greater mean error: for the tracks of Bressan et al. and Chen et al. and for the other tracks. The isochrones of all tested evolutionary models diverge for the stars with masses $M \le 0.7…
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