Empirical Tests of Pre-Main-Sequence Stellar Evolution Models with Eclipsing Binaries

摘要: Abstract We examine the performance of standard pre-main-sequence (PMS) stellar evolution models against accurately measured properties a benchmark sample 26 PMS stars in 13 eclipsing binary (EB) systems having masses 0.04–4.0 M ⊙ and nominal ages ≈1–20 Myr. provide definitive compilation all fundamental for EBs, with careful consistent reassessment observational uncertainties. also various model sets, including physical ingredients limits applicability. No set isochrones is able to successfully reproduce EBs. In H–R diagram, inferred individual by are accurate better than 10% at ≳1 M , but below 1 M they discrepant 50–100%. Adjusting observed radii temperatures using empirical relations effects magnetic activity helps resolve discrepancies few cases, fails as general solution. find evidence that failure match data linked triples EB sample; least half EBs possess tertiary companions. Excluding triples, ∼10% down 0.5 M which current fully contaminated tertiaries. consider several mechanisms might cause changes thus corrupt agreement predictions. show energies orbits comparable needed potentially explain scatter through injection heat, perhaps involving tidal interaction. It seems from hand this mechanism, however it operates detail, has more influence on surface their internal structure, lithium abundances broadly good The members young clusters appear individually coeval within 20%, collectively an apparent age spread ∼50%, suggesting true spreads clusters. However, may be result induced