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Cepheids with giant companions

arxiv.org · 16,986 words · saved by 1 readers

Context. Binary double (BIND) Cepheids are systems comprising two Cepheid components. This feature provides important constraints that allow us to reveal the origin of Cepheids, trace their evolution, and test pulsation theory. Ten BIND Cepheids are now known, with only one having its parameters determined. In five systems, the difference between the pulsational periods of Cepheid components is unusually high. Aims. We aim to estimate the physical parameters of the components of nine BIND Cepheids newly identified in the Magellanic Clouds and the Milky Way, investigate their evolutionary configurations, and formation scenarios. We also expand the parameter space of characterized individual Cepheids in mass, radius, period, and metallicity. Methods. To achieve these goals, we extended the recently introduced 𝑞 -PED method to BIND Cepheids, combining observational constraints with theoretical pulsation and evolutionary models. With the pending determination of the spectroscopic mass ra

1 1 institutetext: 1 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland 2 Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 3 Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101-1292, USA 4 Universidad de Concepción, Departamento Astronomía, Casilla 160-C, Concepción, Chile 1 1 email: fespinoza@camk.edu.pl Cepheids with giant companions III. Evolutionary modeling of nine binary double Cepheids from the Milky Way and Magellanic Clouds F. Espinoza-Aranc

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