This article has an erratum: [https://doi.org/10.1051/0004-6361/201528031e]
Volume 591, July 2016
|Number of page(s)||28|
|Section||Stellar structure and evolution|
|Published online||02 June 2016|
On the effect of rotation on populations of classical Cepheids
II. Pulsation analysis for metallicities 0.014, 0.006, and 0.002
1 Department of Physics & Astronomy, The Johns Hopkins University, 3400 N Charles St, Baltimore, MD 21218, USA
2 Swiss National Science Foundation Fellow
3 Astronomical Institute, Graduate School of Science, Tohoku University, Sendai, 980-8578 Miyagi, Japan
4 Département d’Astronomie, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
Received: 22 December 2015
Accepted: 18 April 2016
Classical Cepheid variable stars (from hereon: Cepheids) are high-sensitivity probes of stellar evolution and fundamental tracers of cosmic distances. While rotational mixing significantly affects the evolution of Cepheid progenitors (intermediate-mass stars), the impact of the resulting changes in stellar structure and composition on Cepheids and their pulsational properties is hitherto unknown. Here we present the first detailed pulsational instability analysis of stellar evolution models that include the effects of rotation, for both fundamental mode and first overtone pulsation. We employ Geneva evolution models spanning a three-dimensional grid in mass (1.7–15 M⊙), metallicity (Z = 0.014, 0.006, 0.002), and rotation (non-rotating, average & fast rotation). We determine (1) hot and cool instability strip (IS) boundaries taking into account the coupling between convection and pulsation; (2) pulsation periods; and (3) rates of period change. We investigate relations between period and (a) luminosity; (b) age; (c) radius; (d) temperature; (e) rate of period change; (f) mass; (g) the flux-weighted gravity-luminosity relation (FWGLR). We confront all predictions aside from those for age with observations, finding generally excellent agreement. We tabulate period-luminosity relations (PLRs) for several photometric pass-bands and investigate how the finite IS width, different IS crossings, metallicity, and rotation affect PLRs. We show that a Wesenheit index based on H, V, and I photometry is expected to have the smallest intrinsic PLR dispersion. We confirm that rotation resolves the Cepheid mass discrepancy. Period-age relations depend significantly on rotation, with rotation leading to older Cepheids, offering a straightforward explanation for evolved stars in binary systems that cannot be matched by conventional isochrones assuming a single age. We further show that Cepheids obey a tight FWGLR. Rotation is a fundamental property of stars that has important implications for the study of intermediate-mass stars, intermediate-age clusters, and classical Cepheid variable stars.
Key words: stars: variables: Cepheids / supergiants / stars: oscillations / stars: evolution / stars: rotation / distance scale
© ESO, 2016
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