EDP Sciences
Free Access
Volume 409, Number 2, October II 2003
Page(s) 611 - 618
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20031114
Published online 17 November 2003

A&A 409, 611-618 (2003)
DOI: 10.1051/0004-6361:20031114

Disentangling discrepancies between stellar evolution theory and sub-solar mass stars

The influence of the mixing length parameter for the UV Psc binary
E. Lastennet1, J. Fernandes1, D. Valls-Gabaud2 and E. Oblak3

1  Observatório Astronómico da Universidade de Coimbra, Santa Clara, 3040 Coimbra, Portugal
2  UMR CNRS 5572, Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées, 14 avenue Édouard Belin, 31400 Toulouse, France
3  UMR CNRS 6091, Laboratoire d'Astrophysique, Observatoire de Besançon, 41bis avenue de l'Observatoire, BP 1615, 25010 Besançon, France

(Received 23 July 2002 / Accepted 16 July 2003 )

Serious discrepancies have recently been observed between predictions of stellar evolution models in the 0.7-1.1  $M_{\odot}$ mass range and accurately measured properties of binary stars with components in this mass range. We study one of these objects, the eclipsing binary UV Piscium, which is particularly interesting because Popper (1997) derived age estimates for each component that differed by more than a factor of two. In an attempt to solve this significant discrepancy (a difference in age of 11 Gyr), we compute a large grid of stellar evolution models with the CESAM code for each component. By fixing the masses to their accurately determined values (relative error smaller than 1% for both stars), we consider a wide range of possible metallicities Z (0.01 to 0.05), and helium content Y (0.25 to 0.34) uncorrelated to Z. In addition, the mixing length parameter $\alpha_{\rm MLT}$ is left as another free parameter. We obtain a best fit in the $T_{\rm eff}$-radius diagram for a common chemical composition ( Z, Y)  = (0.012, 0.31), but a different MLT parameter $\alpha_{\rm MLT, A}$  = 0.95  $\pm$ 0.12(statistical)+0.30(systematic) and $\alpha_{\rm MLT, B}$  = 0.65  $\pm$ 0.07(stat)+0.10(syst). The apparent age discrepancy found by Popper (1997) disappears with this solution, the components being coeval to within 1%. This suggests that fixing $\alpha_{\rm MLT}$ to its solar value (~1.6), a common hypothesis assumed in most stellar evolutionary models, may not be correct. Secondly, since $\alpha_{\rm MLT}$ is smaller for the less massive component, this suggests that the $\alpha_{\rm MLT}$ parameter may decrease with stellar mass, showing yet another shortcoming of the mixing length theory to explain stellar convection. This trend needs further confirmation with other binary stars with accurate data.

Key words: stars: individual: UV Psc -- stars: fundamental parameters -- stars: binaries: eclipsing -- stars: abundances -- stars: Hertzsprung-Russell (HR) and C-M diagrams

Offprint request: J. Fernandes, jmfernan@mat.uc.pt

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© ESO 2003

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