Correlations in the chaotic spectrum of pressure modes in rapidly rotating stars. (arXiv:1811.04673v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Evano_B/0/1/0/all/0/1">Benjamin Evano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Georgeot_B/0/1/0/all/0/1">Bertrand Georgeot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lignieres_F/0/1/0/all/0/1">François Lignières</a>
The oscillation spectrum of pressure waves in stars can be determined by
monitoring their luminosity. For rapidly rotating stars, the corresponding ray
dynamics is mixed, with chaotic and regular zones in phase space. Our numerical
simulations show that the chaotic spectra of these systems exhibit strong peaks
in the autocorrelation which are at odd with Random Matrix Theory predictions.
We explain these peaks through a semiclassical theory based on the peculiar
distribution of the actions of classical periodic orbits. Indeed this
distribution is strongly bunched around the average action between two
consecutive rebounds and its multiples. In stars this phenomenon is a direct
consequence of the strong decrease of the sound speed towards the star surface,
but it would arise in any other physical system with a similar bunching of
orbit actions. The peaks discussed could be observed by space missions and give
insight on the star interiors.
The oscillation spectrum of pressure waves in stars can be determined by
monitoring their luminosity. For rapidly rotating stars, the corresponding ray
dynamics is mixed, with chaotic and regular zones in phase space. Our numerical
simulations show that the chaotic spectra of these systems exhibit strong peaks
in the autocorrelation which are at odd with Random Matrix Theory predictions.
We explain these peaks through a semiclassical theory based on the peculiar
distribution of the actions of classical periodic orbits. Indeed this
distribution is strongly bunched around the average action between two
consecutive rebounds and its multiples. In stars this phenomenon is a direct
consequence of the strong decrease of the sound speed towards the star surface,
but it would arise in any other physical system with a similar bunching of
orbit actions. The peaks discussed could be observed by space missions and give
insight on the star interiors.
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