Identification of Asteroids in Two-Body Resonances

Smirnov, E. A.; Dovgalev, I. S.

doi:10.1134/s0038094618040056

Cited by 7 publications

(3 citation statements)

References 21 publications

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“…2.37755 AU according to Fig.2. The result is slightly differ from our integration with only Earth perturbations (2.377825 AU), and from paperSmirnov, Dovgalev, (2018) (2.377829 AU).…”

contrasting

confidence: 99%

Resonance perturbation of (5026) Martes and 20052 WW113 asteroid pair

Rosaev

2023

Preprint

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The orbital dynamics of a very young asteroid pair (5026) Martes and 2005 WW113 is studied. We detect strong resonant perturbations of the larger member of the pair (5026) Martes by the 3:11 mean motion resonance with the Earth. The unbounded secondary (2005 WW113) has orbited far from the resonance and is not perturbed. We provide a new estimation of the resonance structure and found that, under the planetary perturbations, a single resonance splits into a multiplet. The nominal position of the resonance is 2.37783 AU. However, the center of the corresponding chaotic zone is detected at 2.37754 AU. As a result, we noted a small but not negligible difference between the calculated and observed position of resonance. The multiplet structure of the 3:11 Earth resonance cannot explain this offset (the position of the main term of the multiplet is 2.377698 AU).

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“…2.37755 AU according to Fig.2. The result is slightly differ from our integration with only Earth perturbations (2.377825 AU), and from paperSmirnov, Dovgalev, (2018) (2.377829 AU).…”

contrasting

confidence: 99%

Resonance perturbation of (5026) Martes and 20052 WW113 asteroid pair

Rosaev

2023

Preprint

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“…The most common patterns of resonant angles are pure librations with a small amplitude for two-body MMRs (Figure 1(c)) and a larger amplitude for three-body MMRs (Figures 1(d)-(f)), pure circulation (Figures 1(a)-(b)), and the mixed cases when the periods of librations are replaced by the periods of circulation (Figures 1(g)-(h)). For the librations, the usual value of the amplitude is less than π, even for three-body MMRs (Figure 1(f); Smirnov & Shevchenko 2013;Smirnov & Markov 2017;Smirnov & Dovgalev 2018). In these cases, the LLM achieves high accuracy and differentiates different behaviors.…”

Section: Discussionmentioning

confidence: 97%

“…More complicated analysis can be done by using Lomb-Scargle periodograms (Lomb 1976;Scargle 1982;Zechmeister & Kürster 2009). However, this method is not perfect too and achieves only 90% accuracy (Smirnov & Dovgalev 2018). Moreover, it requires special knowledge and the implementation of complex algorithms, which is a timeconsuming task.…”

Section: Introductionmentioning

confidence: 99%

Fast, Simple, and Accurate Time Series Analysis with Large Language Models: An Example of Mean-motion Resonances Identification

Smirnov

2024

ApJ

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Classical machine learning has been actively utilized in astronomy to address various challenges, including predicting orbital stability, classifying asteroids, galaxies, and other objects, and analyzing images. However, the emerging trend in artificial intelligence involves the use of large language models such as GPT-4 and ChatGPT. These models are trained on a large corpus of text and can perform a wide range of natural language processing tasks, including text generation, translation, summarization, and classification. Surprisingly, these capabilities present significant potential for application in astronomy. This paper demonstrates how the new model gpt-4-vision-preview can analyze visual patterns and accurately classify asteroids as resonant or nonresonant with high accuracy. This process requires no training, fine-tuning, or coding beyond writing the appropriate prompt in natural language. Moreover, this approach can be extended to other common problems within astronomy.

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Resonance perturbation of (5026) Martes and 2005 WW113 asteroid pair

Rosaev

2024

Celest Mech Dyn Astron

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Identification of Asteroids in Two-Body Resonances

Cited by 7 publications

References 21 publications

Resonance perturbation of (5026) Martes and 20052 WW113 asteroid pair

Resonance perturbation of (5026) Martes and 20052 WW113 asteroid pair

Fast, Simple, and Accurate Time Series Analysis with Large Language Models: An Example of Mean-motion Resonances Identification

Resonance perturbation of (5026) Martes and 2005 WW113 asteroid pair

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