Issue |
A&A
Volume 480, Number 2, March III 2008
|
|
---|---|---|
Page(s) | 465 - 473 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20078384 | |
Published online | 25 January 2008 |
Asiago eclipsing binaries program*,**
II. V505 Persei
1
INAF – Osservatorio Astronomico di Padova, Sede di Asiago, 36012 Asiago (VI), Italy e-mail: lina.tomasella@oapd.inaf.it
2
INAF – Osservatorio Astronomico di Collurania, Via M. Maggini, 64100 Teramo, Italy
3
via Filzi 9, 38034 Cembra (TN), Italy
4
University of Ljubljana, Department of Physics, Jadranska 19, 1000 Ljubljana, Slovenia
Received:
31
July
2007
Accepted:
30
November
2007
The orbit and fundamental physical parameters of the double-lined
eclipsing binary V505 Per are derived by means of Echelle high-resolution
and high spectroscopy, and B, V photometry. In addition, effective
temperatures, gravities, rotational velocities, and metallicities of both
components are also obtained from atmospheric
analysis, showing
an excellent match with the results of the orbital solution. An
EB-V ≤ 0.01 mag upper limit to the reddening is derived from
intensity analysis of interstellar NaI (5890.0 & 5895.9 Å) and KI (7699.0 Å) lines. The distance to the system computed from orbital parameters
(60.6 ± 1 pc) is identical to the newly re-reduced Hipparcos parallax
(61.5 ± 1.9 pc). The masses of the two components
(M1 = 1.2693±0.0011 and M2 = 1.2514±0.0012
) place them
in the transition region between convective and radiative stellar cores of
the HR diagram, with the more massive of the two already showing the effect
of evolution within the main sequence band (T1 = 6512±21 K,
T2 = 6462±12 K, R1 = 1.287±0.014, R2 = 1.266±0.013
). This makes this system particularly relevant to theoretical
stellar models as a test of the overshooting. We compare the firm
observational results for V505 Per component stars with the predictions of
various libraries of theoretical stellar models (BaSTI, Padova, Granada,
Yonsei-Yale, Victoria-Regina), as well as with BaSTI models computed
specifically for the masses and chemical abundances of V505 Per. We find
that the overshooting at the masses of V505 Per component stars is already
pretty low, but not nil, and it is described by efficiencies
= 0.093 and 0.087 for the 1.27 and 1.25
components,
respectively. According to the computed BaSTI models, the age of the system
is ~0.9 Gyr, and the element diffusion during this time has reduced the
surface metallicity from the initial [M/H]= -0.03 to the current
[M/H] = -0.13, in excellent agreement with the observed [M/H] = -0.12±0.03.
Key words: stars: fundamental parameters / stars: binaries: spectroscopic / stars: binaries: eclipsing / star: individual: V505 Persei
© ESO, 2008
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