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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742389.0, MPI für Astronomie / Publikationen_mpia
Spectroscopic properties of a two-dimensional time-dependent Cepheid model. I. Description and validation of the model
Authors:Vasilyev, V.; Ludwig, H. -. G.; Freytag, B.; Lemasle, B.; Marconi, M.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:Astronomy and Astrophysics
Volume:606
Start Page:id. A140 (13 pp)
Audience:Not Specified
Abstract / Description:Context. Standard spectroscopic analyses of Cepheid variables are based on hydrostatic one-dimensional model atmospheres, with convection treated using various formulations of mixing-length theory. <BR /> Aims: This paper aims to carry out an investigation of the validity of the quasi-static approximation in the context of pulsating stars. We check the adequacy of a two-dimensional time-dependent model of a Cepheid-like variable with focus on its spectroscopic properties. <BR /> Methods: With the radiation-hydrodynamics code CO5BOLD, we construct a two-dimensional time-dependent envelope model of a Cepheid with Teff = 5600 K, log g = 2.0, solar metallicity, and a 2.8-day pulsation period. Subsequently, we perform extensive spectral syntheses of a set of artificial iron lines in local thermodynamic equilibrium. The set of lines allows us to systematically study effects of line strength, ionization stage, and excitation potential. <BR /> Results: We evaluate the microturbulent velocity, line asymmetry, projection factor, and Doppler shifts. The microturbulent velocity, averaged over all lines, depends on the pulsational phase and varies between 1.5 and 2.7 km s-1. The derived projection factor lies between 1.23 and 1.27, which agrees with observational results. The mean Doppler shift is non-zero and negative, -1 km s-1, after averaging over several full periods and lines. This residual line-of-sight velocity (related to the "K-term") is primarily caused by horizontal inhomogeneities, and consequently we interpret it as the familiar convective blueshift ubiquitously present in non-pulsating late-type stars. Limited statistics prevent firm conclusions on the line asymmetries. <BR /> Conclusions: Our two-dimensional model provides a reasonably accurate representation of the spectroscopic properties of a short-period Cepheid-like variable star. Some properties are primarily controlled by convective inhomogeneities rather than by the Cepheid-defining pulsations. Extended multi-dimensional modelling offers new insight into the nature of pulsating stars.
Free Keywords:radiative transfer; stars: variables: Cepheids; methods: numerical; stars: atmospheres; convection; stars: oscillations
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-6361
URL:http://adsabs.harvard.edu/abs/2017A%26A...606A.140...
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