Variable Star Light Curves in Koopman Space
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arXiv
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| Hauptverfasser: | , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866914884777672704 |
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| author | Mekhaël, Nicolas Pasquato, Mario Carenini, Gaia Braga, Vittorio F. Trevisan, Piero Bono, Giuseppe Hezaveh, Yashar |
| author_facet | Mekhaël, Nicolas Pasquato, Mario Carenini, Gaia Braga, Vittorio F. Trevisan, Piero Bono, Giuseppe Hezaveh, Yashar |
| contents | We present the first application of data-driven techniques for dynamical system analysis based on Koopman theory to variable stars. We focus on light curves of RRLyrae type variables, in the Galactic globular cluster $ω$ Centauri. Light curves are thus summarized by a handful of complex eigenvalues, corresponding to oscillatory or fading dynamical modes. We find that variable stars of the RRc subclass can be summarized in terms of fewer ($\approx 8$) eigenvalues, while RRab need comparatively more ($\approx 12$). This result can be leveraged for classification and reflects the simpler structure of RRc light curves. We then consider variable stars displaying secular variations due to the Tseraskaya-Blazhko effect and find a change in relevant eigenvalues with time, with possible implications for the physical interpretation of the effect. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_16868 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Variable Star Light Curves in Koopman Space Mekhaël, Nicolas Pasquato, Mario Carenini, Gaia Braga, Vittorio F. Trevisan, Piero Bono, Giuseppe Hezaveh, Yashar Solar and Stellar Astrophysics Astrophysics of Galaxies Instrumentation and Methods for Astrophysics We present the first application of data-driven techniques for dynamical system analysis based on Koopman theory to variable stars. We focus on light curves of RRLyrae type variables, in the Galactic globular cluster $ω$ Centauri. Light curves are thus summarized by a handful of complex eigenvalues, corresponding to oscillatory or fading dynamical modes. We find that variable stars of the RRc subclass can be summarized in terms of fewer ($\approx 8$) eigenvalues, while RRab need comparatively more ($\approx 12$). This result can be leveraged for classification and reflects the simpler structure of RRc light curves. We then consider variable stars displaying secular variations due to the Tseraskaya-Blazhko effect and find a change in relevant eigenvalues with time, with possible implications for the physical interpretation of the effect. |
| title | Variable Star Light Curves in Koopman Space |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2407.16868 |