Period doubling with hysteresis in BL Her-type models

Details Period doubling with hysteresis in BL Her-type models Period doubling with hysteresis in BL Her-type models

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.210..301m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 210, no. 1-2, p. 301-305 (IAU Colloquium 134)

Astronomy and Astrophysics

Astrophysics

1

Hydrodynamics, Hysteresis, Period Doubling, Stellar Models, Stellar Oscillations, Variable Stars, Light Curve, Radial Velocity, Stellar Evolution, Stellar Luminosity

Scientific paper

We have performed recently a survey of the nonlinear hydrodynamical models of the BL Her-type variables (Buchler & Moskalik 1992). Within this project we have studied several sequences of models, i.e., families in which only Teff has been varied from model to model, while all other stellar parameters have been kept constant. The fundamental mode pulsations of each model have been converged to strict periodicity with the relaxation code (Stellingwerf 1974). Such approach speeds up to the calculations and simultaneously yields information about the stability properties of the resulting limit cycles. In all studied sequences except one, we have found a narrow range of Teff (typically 100-150K), in which regular solution becomes unstable towards a priod doubling bifurcation. The instability has its origin in a half-integer resonance, namely the 3:2 coupling between the fundamental mode and the first overtone. This is the same resonance, which also causes period doubling in the models of classical Cepheids. The bifurcation leads to stable period-two oscillations, characterized by an RV Tau-like, albeit strictly periodic behavior of all variables. In other words, the pulsation light curves and velocity curves will exhibit two alternating minima (as well as maxima) of different values. We show the bifurcation for one of our sequences, by plotting minimum pulsational velocities Vmin versus Teff.

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