Stability of exoplanetary systems retrieved from scalar time series. (arXiv:1911.07957v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kovacs_T/0/1/0/all/0/1">Tamas Kovacs</a>
We propose a novel method applied to extrasolar planetary dynamics to
describe the system stability. The observations in this field serve the
measurements mainly of radial velocity, transit time, and/or celestial
position. These scalar time series are used to build up the high-dimensional
phase space trajectory representing the dynamical evolution of planetary
motion. The framework of nonlinear time series analysis and Poincar’e
recurrences allows us to transform the obtained univariate signals into complex
networks whose topology carries the dynamical properties of the underlying
system. The network-based analysis is able to distinguish the regular and
chaotic behaviour not only for synthetic inputs but also for noisy and
irregularly sampled real world observations. The proposed scheme does not
require neither n-body integration nor best fitting planetary model to perform
the stability investigation, therefore, the computation time can be reduced
drastically compared to those of the standard numerical methods.
We propose a novel method applied to extrasolar planetary dynamics to
describe the system stability. The observations in this field serve the
measurements mainly of radial velocity, transit time, and/or celestial
position. These scalar time series are used to build up the high-dimensional
phase space trajectory representing the dynamical evolution of planetary
motion. The framework of nonlinear time series analysis and Poincar’e
recurrences allows us to transform the obtained univariate signals into complex
networks whose topology carries the dynamical properties of the underlying
system. The network-based analysis is able to distinguish the regular and
chaotic behaviour not only for synthetic inputs but also for noisy and
irregularly sampled real world observations. The proposed scheme does not
require neither n-body integration nor best fitting planetary model to perform
the stability investigation, therefore, the computation time can be reduced
drastically compared to those of the standard numerical methods.
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