Analysing the Main Belt asteroid distributions by wavelets
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(2020) 132:34
ORIGINAL ARTICLE
Analysing the Main Belt asteroid distributions by wavelets R. V. Baluev1
· E. I. Rodionov1
Received: 9 January 2020 / Revised: 27 June 2020 / Accepted: 6 July 2020 © Springer Nature B.V. 2020
Abstract We perform statistical wavelet analysis of the Main Belt asteroids, seeking statistically significant asteroid families. The goal is to test the new wavelet analysis algorithm and to compare its results with more traditional methods like the hierarchic clustering. We first consider several 1D distributions for various physical and orbital parameters of asteroids. Then, we consider three bivariate distributions for the three orbital parameters (a, e, i) taken pairwisely. The full 3D analysis of this space is not available here, but based on the 2D results we perform a disentangling of overlapped 2D families and derive a total of 44 3D families with confirmed statistical significance. Keywords Main Belt · Asteroid families · Wavelet analysis · Statistical analysis
1 Introduction First attempts to find asteroid families date back to XIX century, although the discovery of new asteroids was rather slow that time, compared to the contemporary rate. In 1876, based on just about 150 asteroids, D. Kirkwood noticed about 10 asteroid groups, each containing just 2–3 members moving along similar orbits. It was suggested that asteroids in such groups may have a common origin, e.g. fragments of larger disrupted bodies. F. Tisserand continued Kirkwood attempts, composing a list of 417 asteroids (1891) and also introducing a formal orbital classification characteristic now well known as the Tisserand invariant T J (see Hirayama 1922). The number of asteroid families grew as new asteroids were discovered. However, no other factors supported the common origin within a family, except for orbit closeness. Therefore, the physical relationship of such asteroids often remained too disputable. Later on, Hirayama (1918) noticed that it might be not reasonable to compare contemporary orbits of asteroids for that goal. On a long timescale, planetary perturbations may change orbits a lot, even if asteroids indeed were fragments of the same body in some past
Electronic supplementary material The online version of this article (https://doi.org/10.1007/s10569-02009976-2) contains supplementary material, which is available to authorized users.
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R. V. Baluev [email protected] Saint Petersburg State University, Universitetskaya emb. 7–9, St Petersburg, Russia 199034 0123456789().: V,-vol
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R. V. Baluev, E. I. Rodionov
and had close orbits initially. This motivation leaded K. Hirayama to the idea of invariant orbital elements that would remain (nearly) constant regardless of the planetary perturbations. Hirayama constructed such invariant elements based on the Lagrange perturbation theory and introduced them as ‘proper elements’, assuming that asteroids from the same family inherited them from their progenitors, should the latter exist in some past. The proper elements remain very useful
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