Pulsations of model RR Lyrae stars

Baker, N. H.; Gough, D. O.

doi:10.1086/157492

Cited by 85 publications

(59 citation statements)

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“…2.3). A well known problem that can arise with the Unno's prescriptions, is the occurrence of short-wavelength spatial oscillations of the thermal eigenfunctions (Baker & Gough 1979;Gonczi & Osaki 1980). We discuss this problem in Sect.…”

Section: Introductionmentioning

confidence: 99%

Convection-pulsation coupling

Grigahcène

Dupret

Gabriel

et al. 2005

A&A

188

246

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Abstract. We present in details a time-dependent convection treatment in the frame of the Mixing-Length Theory (MLT). Following the original ideas by Unno (1967, PASJ, 19, 140), this theory has been developed by Gabriel et al. (1974, Bull. Ac. Roy. Belgique, Classe des Sciences, 60, 866) and Gabriel (1996, Bull. Astron. Soc. India, 24, 233). In this paper, we present it in a united form, we detail the basic derivations and approximations and give final improvements. A new perturbation of the energy closure equation is proposed for the first time, making it possible to avoid the occurrence of short wavelength spatial oscillations of the thermal eigenfunctions. This theory accounts for the perturbation of the convective flux, the turbulent Reynolds stress and the turbulent kinetic energy dissipation. It has been numerically implemented in a non-radial non-adiabatic pulsation code and the first results published in a Letter by Dupret et al. (2004a, A&A, 414, L17) indicate that the theory predicts the observed red border of the lower end of the instability strip and the driving mechanism of the recently discovered γ Dor stars.

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Section: Introductionmentioning

confidence: 99%

Convection-pulsation coupling

Grigahcène

Dupret

Gabriel

et al. 2005

A&A

188

246

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“…Finally, current pulsation models are able to reproduce the already quoted correlation between the period and the absolute magnitude in the near-infrared bands and in particular in the K (2.2 µm) band (Bono et al 2001(Bono et al , 2003, providing 1 The red edge is less reliable due to its well known sensitivity to the efficiency of convection and to the uncertianties still affecting the treatment of turbulent convection. useful constraints on the PL(K)-based RR Lyrae distance scale.…”

Section: Calibration Of the Rr Lyrae Distance Scalementioning

confidence: 98%

“…Bono et al 1995 and references therein). A time-dependent generalization of the mixing-length theory was adopted by Baker & Gough (1979) in the construction RR Lyrae nonadiabatic models. These authors studied the effect of including the interaction between pulsation and convection on their stability analysis.…”

Section: Linear Non-adiabatic Modelsmentioning

confidence: 99%

RR Lyrae Pulsation Theory

Marconi¹,

Guzik²,

Bradley³

2009

AIP Conference Proceedings

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Abstract. RR Lyrae stars play an important role as distance indicators and stellar population tracers. In this context the construction of accurate pulsation models is crucial to understand the observed properties and to constrain the intrinsic stellar parameters of these pulsators. The physical mechanism driving pulsation in RR Lyrae stars has been known since the middle of the 20th century and many efforts have been performed during the last few decades in the construction of more and more refined pulsation models. In particular, nonlinear pulsation models including a nonlocal time-dependent treatment of convection, such as the ones originally developed in Los Alamos in the seventies, allow us to reproduce all the relevant observables of stellar radial pulsation and to establish accurate relations and methods to contrain the intrinsic stellar properties and the distances of these variables. The most recent results on RR Lyrae pulsation obtained through these kinds of models will be presented and a few still debated problems will be discussed.

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“…In computations of oscillation frequencies the adiabatic approximation is commonly adopted, and perturbations to the turbulent Reynolds stresses are neglected. When nonadiabatic calculations are carried out the treatment of the perturbation to the convective flux is a major uncertainty in the calculation (e.g., Baker & Gough 1979;Gough 1980;Balmforth 1992a). …”

Section: Superficial Problemsmentioning

confidence: 99%

Prospects for asteroseismology

Christensen‐Dalsgaard¹,

Houdek²

2009

Synergies Between Solar and Stellar Modelling

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The observational basis for asteroseismology is being dramatically strengthened, through more than two years of data from the CoRoT satellite, the flood of data coming from the Kepler mission and, in the slightly longer term, from dedicated ground-based facilities. Our ability to utilize these data depends on further development of techniques for basic data analysis, as well as on an improved understanding of the relation between the observed frequencies and the underlying properties of the stars. Also, stellar modelling must be further developed, to match the increasing diagnostic potential of the data. Here we discuss some aspects of data interpretation and modelling, focussing on the important case of stars with solar-like oscillations.

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Pulsations of model RR Lyrae stars

Cited by 85 publications

References 0 publications

Convection-pulsation coupling

Convection-pulsation coupling

RR Lyrae Pulsation Theory

Prospects for asteroseismology

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