Low-dimensional chaos in stellar pulsations

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Low-dimensional chaos in stellar pulsations is the current interpretation of an established phenomenon. The light curves of intrinsic variable stars with large amplitudes have been known for centuries to exhibit behavior that goes from extreme regularity, as for the classical Cepheids and the RR Lyrae stars, to extreme irregularity, as for the so called Irregular variables. In the Population II stars this irregularity gradually increases from the low period W Virginis variables through the RV Tauri variables into the regime of the semiregular variables.

Regular behavior of the Cepheids[edit]

The regular behavior of the Cepheids has been successfully modeled with numerical hydrodynamics since the 1960s[1] ,[2] and from a theoretical point of view it is easily understood as due to the presence of center manifold which arises because of the weakly dissipative nature of the dynamical system.[3] This, and the fact that the pulsations are weakly nonlinear, allows a description of the system in terms of amplitude equations[4] [5] and a construction of the bifurcation diagram (see also bifurcation theory) of the possible types of pulsation (or limit cycles), such fundamental mode pulsation, first or second overtone pulsation, or more complicated, double-mode pulsations in which several modes are excited with constant amplitudes. The boundaries of the instability strip where pulsation sets in during the star's evolution correspond to a Hopf bifurcation.

Irregularity of Population II stars[edit]

In contrast, the irregularity of the large amplitude Population II stars is more challenging to explain. The variation of the pulsation amplitude over one period implies large dissipation, and therefore there exists no center manifold. Various mechanisms have been proposed, but are found lacking. One, suggests the presence of several closely spaced pulsation frequencies that would beat against each other, but no such frequencies exist in the appropriate stellar models. Another, more interesting suggestion is that the variations are of a stochastic nature,[6] but no mechanism has been proposed or exists that could provide the energy for such large observed amplitude variations). It is now established that the mechanism behind the irregular light curves is an underlying low dimensional chaotic dynamics (see also Chaos theory). This conclusion is based on two types of studies:

Numerical hydrodynamics simulations[edit]

The numerical computations of the pulsations of sequences of W Virginis stellar models exhibit two approaches to irregular behavior that are a clear signature of low dimensional chaos. The first indication comes from first return maps in which one plots one maximum radius, or any other suitable variable, versus the next one. The sequence of models shows a period doubling bifurcation, or cascade, leading to chaos. The near quadratic shape of the map is indicative of chaos and implies an underlying horseshoe map [7] [8] .[9] Other sequences of models follow a somewhat different route, but also to chaos, namely the Pommeau-Manneville or tangent bifurcation route. [10] .[11]

The following shows a similar visualization of the period doubling cascade to chaos for a sequence of stellar models that differ by their average surface temperature T. The graph shows triplets of values of the stellar radius (Ri, Ri+1, Ri+2) where the indices i, i+1, i+2 indicate successive time intervals.

PeriodiDoubling1.jpg PeriodDoubling2.jpg Period Doubling3.jpg PeriodDoubling4.jpg PeriodDoubling5.jpg PeriodDoubling6.jpg
P0 P2 P4 P8 Banded Chaos FullChaos

The presence of low dimensional chaos is also confirmed by another, more sophisticated, analysis of the model pulsations which extracts the lowest unstable periodic orbits and examines their topological organization (twisting). The underlying attractor is found to be banded like the Roessler attractor, with however an additional twist in the band. .[12]

Global flow reconstruction from observed light curves[edit]

The method of global flow reconstruction [13] uses a single observed signal {si} to infer properties of the dynamical system that generated it. First N-dimensional 'vectors' Si=(si,si-1,si-2,...,si-N+1) are constructed. The next step consists in finding an expression for the nonlinear evolution operator M that takes the system from time i to time i+1, i.e. Si+1= M (Si). Takens' theorem guarantees that under very general circumstances the topological properties of this reconstructed evolution operator are the same as that of the physical system, provided the embedding dimension N is large enough. Thus from the knowledge of a single observed variable one can infer properties about the real physical system which is governed by a number of independent variables.

This approach has been applied to the AAVSO data for the star R Scuti [14] .[15] It could be inferred that the irregular pulsations of this star arise from an underlying 4-dimensional dynamics. Phrased differently this says that from any 4 neighboring observations one can predict the next one. From a physical point of view it says that there are 4 independent variables that describe the dynamic of the system. The method of false nearest neighbors corroborates an embedding dimension of 4. The fractal dimension of the dynamics of R Scuti as inferred from the computed Lyapunov exponents lies between 3.1 and 3.2.

Top: R Scuti observed AAVSO light curve (smoothed); Bottom: Synthetic light curve, obtained with the help of the reconstructed evolution operator. Note the similarity with the observed light curve.

From an analysis of the fixed points of the evolution operator a nice physical picture can be inferred, namely that the pulsations arise from the excitation of an unstable pulsation mode that couples nonlinearly to a second, stable pulsation mode which is in a 2:1 resonance with the first one, a scenario described by the Shilnikov theorem "[14]".

This resonance mechanism is not limited to R Scuti, but has been found to hold for several other stars for which the observational data are sufficiently good [16]

References[edit]

  1. ^ Christy, R. F., 1964, The Calculation of Stellar Pulsation, Reviews of Modern Physics 36, 555 "[1]"
  2. ^ Cox, A. N., Brownlee, R. R., Eilers, D. D., 1966 Time-Dependent Method for Computation of Radiation Diffusion and Hydro-Dynamics, Astrophysical Journal, 144, 1024 "[2]"
  3. ^ Buchler, J.R. 1993, A Dynamical Systems Approach to Nonlinear Stellar Pulsations, in Nonlinear Phenomena in Stellar Variability, Eds. M. Takeuti & J.R. Buchler, Dordrecht: Kluwer Publishers, reprinted from 1993, Astrophysics and Space Science, 210, 1–31. "[3]"</a>
  4. ^ Spiegel, E. A., Cosmic Arrhythmias in Chaos in Astrophysics, NATO ASI Ser. C, Vol. 161, eds. J. R. Buchler J. M. Perdang \& E. A. Spiegel, (Dordrecht : Reidel)
  5. ^ Buchler, J.R. & Goupil, M.J. 1984, Amplitude Equations for Nonadiabatic, Nonlinear Stellar Pulsators, I. The Formalism, Astrophysical Journal 279, 394–400, "[4]"
  6. ^ Koenig, M., Paunzen, E., Timmer, J., 1999, On the irregular temporal behaviour of the variable star R Scuti, Monthly Notices of the Royal APeriodiDoubling1.jpg stronomical Society, 303, 297, "[5]"
  7. ^ Buchler, J.R. & Kovacs, G. 1987, Period-Doubling Bifurcations and Chaos in W Virginis Models, Astrophysical Journal Letters 320, L57-L62, "[6]".
  8. ^ Kovacs G., Buchler J.R. 1988, Regular and Irregular Pulsations in Population II Cepheids, Astrophysical Journal 334, 971–994 "[7]".
  9. ^ Aikawa, T. 1990, Intermittent chaos in a subharmonic bifurcation sequence of stellar pulsation models, Astrophysics and Space Science, 164, 295 "[8]"
  10. ^ Buchler, J.R., Goupil M.J. & Kovacs G. 1987, Tangent Bifurcations and Intermittency in the Pulsations of Population II Cepheid Models, Physics Letters A 126, 177–180.
  11. ^ Aikawa, T. 1987, The Pomeau-Manneville intermittent transition to chaos in hydrodynamic pulsation models, Astrophysics and Space Science, 139, 281
  12. ^ Letellier, C., Gouesbet, G., Soufi, F., Buchler, J.R. & Kollath, Z., 1996, Chaos in variable stars: Topological analysis of W Vir model pulsations, Chaos, 6, 466—476, "[9]".
  13. ^ Packard, N., Crutchfield, J., Farmer, J. D. and Shaw, R., 1980, Geometry from a time series, Physical Review Letters 45, 712, "[10]"
  14. ^ Buchler, J. R., Serre, T., Kollath, Z. & Mattei, J. 1995, A Chaotic Pulsating Star – The Case of R Scuti, Physical Review Letters, 74, 842–845 "[11]"
  15. ^ Buchler, J. R.; Kollath, Z.; Serre, T.; Mattei, J., 1996, A Nonlinear Analysis of the Variable Star R Scuti, Astrophysical Journal 462, 489, "[12]"
  16. ^ Buchler, J. R., Kollath, Zoltan and Cadmus, R., 2004, Evidence for Low-Dimensional Chaos in Semiregular Variable Stars, Astrophysical Journal, Vol. 613, pp. 532 – 547 "[13]"