ON THE EVOLUTIONARY AND PULSATION MASS OF CLASSICAL CEPHEIDS. III. THE CASE OF THE ECLIPSING BINARY CEPHEID CEP0227 IN THE LARGE MAGELLANIC CLOUD

• Published in: The Astrophysical journal Vol. 749; no. 2; pp. 1 - 15
• Main Authors: PRADA MORONI, P. G, GENNARO, M, BONO, G, PIETRZYNSKI, G, GIEREN, W, PILECKI, B, GRACZYK, D, THOMPSON, I. B
• Format: Journal Article
• Language: English
• Published: Bristol IOP 20.04.2012
• Subjects: APPROXIMATIONS; Astronomical models; Astronomy; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; Bayesian analysis; Cepheid variables; CEPHEIDS; CHEMICAL COMPOSITION; Construction; Earth, ocean, space; Eclipsing binary stars; Evolutionary; Exact sciences and technology; GRAVITATION; HYDROGEN BURNING; LUMINOSITY; MAGELLANIC CLOUDS; MASS; Mathematical models; Planes; PULSATIONS; STAR EVOLUTION; Stellar mass; Eclipsing binary stars; Luminosity; Loss rate; Convective overshooting; stars: distances; Magellanic Clouds; Chemical composition; Age; Hydrogen burning; Gravity; binaries: eclipsing; Isochrone; stars: evolution; Cepheids; Mass distribution; Mass loss; Stellar evolution; Distance modulus; stars: variables: Cepheids; stars: oscillations; Stellar mass; Normal distribution; Physical parameter; Models; Large Magellanic Cloud
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637x/749/2/108

We present a new Bayesian approach to constrain the intrinsic parameters (stellar mass and age) of the eclipsing binary system-CEP0227-in the Large Magellanic Cloud (LMC). We computed several sets of evolutionary models covering a broad range in chemical compositions and in stellar mass. Independent sets of models were also constructed either by neglecting or by including a moderate convective core overshooting ( beta sub(ov) = 0.2) during central hydrogen-burning phases. Sets of models were also constructed either by neglecting or by assuming a canonical ([eta] = 0.4, 0.8) or an enhanced ([eta] = 4) mass-loss rate. The most probable solutions were computed in three different planes: luminosity-temperature, mass-radius, and gravity-temperature. By using the Bayes factor, we found that the most probable solutions were obtained in the gravity-temperature plane with a Gaussian mass prior distribution. The evolutionary models constructed by assuming a moderate convective core overshooting ( beta sub(ov) = 0.2) and a canonical mass-loss rate ([eta] = 0.4) give stellar masses for the primary (Cepheid)-M = 4.14 super(+0.04) sub(- 0.05) M sub([middot in circle])-and for the secondary-M = 4.15 super(+0.04) sub(-0.05) M sub([middot in circle])-that agree at the 1% level with dynamical measurements. Moreover, we found ages for the two components and for the combined system-t = 151 super(+4) sub(-3) Myr-that agree at the 5% level. The solutions based on evolutionary models that neglect the mass loss attain similar parameters, while those ones based on models that either account for an enhanced mass loss or neglect convective core overshooting have lower Bayes factors and larger confidence intervals. The dependence on the mass-loss rate might be the consequence of the crude approximation we use to mimic this phenomenon. By using the isochrone of the most probable solution and a Gaussian prior on the LMC distance, we found a true distance modulus-18.53 super(+0.02) sub(-0.0 2) mag-and a reddening value-E(B - V) = 0.142 super(+0.005) sub(-0.010) mag-that agree quite well with similar estimates in the literature.