By J. R. Buchler, J. M. Perdang, E. A. Spiegel (auth.), J. R. Buchler, J. M. Perdang, E. A. Spiegel (eds.)
The according to iod of an oscillator tells us a lot approximately its constitution. J. J. Thomson's deduction particle with the e/rn of an electron was once within the atom could be the main beautiful example. For us, the deduction of the suggest density of a celebrity from its oscillation interval is one other very important instance. What then will we deduce approximately an oscillator that's not periodic? If there are a number of frequencies or if the habit is chaotic, may well we now not desire to benefit much more smooth important facts approximately its workings? the hot development within the idea of dynamical structures, rather within the elucidat ion of the character of chaos, makes it look moderate to invite this now. this is often an account of a few of the happenings of a workshop at which this query was once raised and mentioned. ~iTe have been inc0rested in seeing ways that the current knowing of chaos may perhaps advisor astrophysical modelling and the translation of observations. yet we didn't try and disguise that we have been additionally attracted to chaos itself, and that made for a delightful rapport among the chaoticists and astrophysicists on the assembly. we've numerous introductory papers on chaos in those lawsuits, really at the research of information from platforms that could be suspected of chaotic habit. The papers of Geisel, Grassberger and Guckenheimer introduce the methods of characterizing chaos and Perdang illustrates how a few of these principles will be positioned into perform in particular cases.
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These authors, investigating the stars of the solar neighborhood, found no statistically significant peak at the 3a level in the power spectra of their velocity measurements; nevertheless, at the 2a level, the star a C Mi (procyon), of spectral type F5 IV-V, exhibits a peak at a period of 57 ± 1 s, with velocity amplitude of 15 m/s. , star of a structure similar to the sun's, studied by Traub et al. Observational work in this direction is now being continued by Fossat and coworkers (cf. Gelly et al.
From a collection of 16 a Cepheids investigated by at least one of these methods, 9 stars are found to be non-radially oscillating; for two stars, a CMa and 12 Lac, non-radiality has been assessed on the basis of several methods; for four stars, a CMa, a Cep, 12 Lac and BW Vul quadrupole modes have been identified. Shobbrook (1979) reports that the frequency spectra of a number of a Cephei stars are changing over periods of decades and sometimes of years, indicating a secularly varying shape function of their light or velocity curves (cf.
1 II li r, /1 r. J ~ "', • .. 1"\,\1,1 ,_ \" \J ~ U \"~ l i ~ ~ ~ ~ ~~ Fig. 6. PERDANG light curves of several group 1 pulsators. RU Camelopardalis, usually classified as a W Vir variable (cf. 0 mag. Carrying out a total of 24 observations, Sandford (1927) reported that the velocity curve, with a range of 30 km/s, was not the mirror image of the light curve, as it should be for bona fide RR Lyrae stars. From searches of the older literature, he also concluded that this object was exceptionally faint in 1888, 1894, and 1896; this was the first evidence for disordered variability in RU Cam.