Nonlinear convective pulsation models of RR Lyrae stars are used to obtain a theoretical fit of the observed light curves for a number of pulsators in the Galactic globular cluster M3, with the purpose of constraining their intrinsic stellar parameters and the cluster distance modulus. The dependence of the fit quality on the input stellar properties is investigated and the self consistency of the adopted theoretical scenario is discussed.

Modeling M3 RR Lyrae light curves

DEGL'INNOCENTI, SCILLA
2008

Abstract

Nonlinear convective pulsation models of RR Lyrae stars are used to obtain a theoretical fit of the observed light curves for a number of pulsators in the Galactic globular cluster M3, with the purpose of constraining their intrinsic stellar parameters and the cluster distance modulus. The dependence of the fit quality on the input stellar properties is investigated and the self consistency of the adopted theoretical scenario is discussed.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11568/119837
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