Untitled

Demirçan, Osman; Özdemir, Sacit; Tanriver, Mehmet

doi:10.1023/a:1000535803241

Cited by 2 publications

(1 citation statement)

References 2 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our photometry provides three epochs of minima: a primary eclipse at HJD=2451587.30641 (±0.00017) and secondary eclipses at HJD=2451779.40820 (±0.00016) and 2451910.29094 (±0.00017). We have combined them with the orbital ephemeris in Table 2 and the epochs of minima published by Kaiser et al (1990), M97 andDemircan et al (1997). The earliest of such minima dates back to 1903.…”

Section: Orbital Period Stabilitymentioning

confidence: 99%

Asiago eclipsing binaries program

Tomasella¹,

Munari²,

Siviero³

et al. 2008

A&A

View full text Add to dashboard Cite

The orbit and fundamental physical parameters of the double-lined eclipsing binary V505 Per are derived by means of Echelle highresolution and high S /N spectroscopy, and B, V photometry. In addition, effective temperatures, gravities, rotational velocities, and metallicities of both components are also obtained from atmospheric χ 2 analysis, showing an excellent match with the results of the orbital solution. An E B−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 (M 1 = 1.2693 ± 0.0011 and M 2 = 1.2514 ± 0.0012 M ) 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 (T 1 = 6512 ± 21 K, T 2 = 6462 ± 12 K, R 1 = 1.287 ± 0.014, R 2 = 1.266 ± 0.013 R ). 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 λ OV = 0.093 and 0.087 for the 1.27 and 1.25 M components, respectively. According to the computed BaSTI models, the age of the system is ∼0.9 Gyr, and the element diffusion

show abstract

Section: Orbital Period Stabilitymentioning

confidence: 99%