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Finding our place in the universe : how we discovered Laniakea-- the Milky Way's home
\"The book tells the story of how Courtois and her cosmography colleagues discovered and mapped the Laniakea galactic supercluster, the first and most accurate description to date of our home galaxy's location in the universe. Courtois reveals the joys and challenges of international astronomy research and collaborations, humanizing the scientists along the way and making the science accessible. She also makes an effort to shed light on the life and work of herself and other women astronomers. It's a story that would appeal to a wide audience.\"-- Provided by publisher.
Book
Perihelia Reduction and Global Kolmogorov Tori in the Planetary Problem
We prove the existence of an almost full measure set of
The
proof exploits nice parity properties of a new set of coordinates for the planetary problem, which reduces completely the number of
degrees of freedom for the system (in particular, its degeneracy due to rotations) and, moreover, is well fitted to its reflection
invariance. It allows the explicit construction of an associated close to be integrable system, replacing Birkhoff normal form, common
tool of previous literature.
eBook
Machine learning applied to asteroid dynamics
Machine learning (ML) is the branch of computer science that studies computer algorithms that can learn from data. It is mainly divided into supervised learning, where the computer is presented with examples of entries, and the goal is to learn a general rule that maps inputs to outputs, and unsupervised learning, where no label is provided to the learning algorithm, leaving it alone to find structures. Deep learning is a branch of machine learning based on numerous layers of artificial neural networks, which are computing systems inspired by the biological neural networks that constitute animal brains. In asteroid dynamics, machine learning methods have been recently used to identify members of asteroid families, small bodies images in astronomical fields, and to identify resonant arguments images of asteroids in three-body resonances, among other applications. Here, we will conduct a full review of available literature in the field and classify it in terms of metrics recently used by other authors to assess the state of the art of applications of machine learning in other astronomical subfields. For comparison, applications of machine learning to Solar System bodies, a larger area that includes imaging and spectrophotometry of small bodies, have already reached a state classified as progressing. Research communities and methodologies are more established, and the use of ML led to the discovery of new celestial objects or features, or new insights in the area. ML applied to asteroid dynamics, however, is still in the emerging phase, with smaller groups, methodologies still not well-established, and fewer papers producing discoveries or insights. Large observational surveys, like those conducted at the Zwicky Transient Facility or at the Vera C. Rubin Observatory, will produce in the next years very substantial datasets of orbital and physical properties for asteroids. Applications of ML for clustering, image identification, and anomaly detection, among others, are currently being developed and are expected of being of great help in the next few years.
Journal Article
Retrograde resonances at high mass ratio in the circular restricted 3-body problem
Studies involving retrograde orbits have been an emerging field in recent years, particularly in the case where there are resonances between objects orbiting in opposite directions. The high amount of data from space exploration missions increases the possibility of observing binary stellar systems which may have additional bodies with retrograde orbits. Furthermore, such orbits are relevant to understanding the dynamics of spacecrafts around binary asteroids, being essential to planning exploratory missions. In this work, we survey retrograde orbits around binary systems with mass ratio between 0.01 (hierarchical) and 0.5 (equal masses) in the framework of the planar circular restricted three-body problem (PCR3BP). We build surfaces of section and identify retrograde resonances up to fifth order, namely the 2/−1, 3/−2, 1/−1, 2/−3, 1/−2, 1/−3 and 1/−4 resonances. We conclude that retrograde resonances occur in binary systems at high mass ratio, including the co-orbital (1/−1) resonance. Period doubling bifurcations occur for the 1/−1 resonance, and period doubling and period tripling bifurcations are observed for the 1/−2 resonance. Asymmetric retrograde resonances of the type 1/−n occur for almost equal masses of the binary system. This study may be used for identifying retrograde planets in extrasolar systems and may possibly have applications to astrodynamics mission planning.
Journal Article
The p : q resonance for dissipative spin–orbit problem in celestial mechanics
In this paper, we investigate the existence of p : q resonant orbit for the dissipative spin–orbit problem of the celestial mechanics. Our result is the generalization of the work (Biasco and Chierchia in J Differ Equ 246(11):4345–4370, 2009) from C∞ topology to analytic and finitely differentiable topology. Moreover, our result gives the existence condition of p : q resonance solutions for concrete dissipative spin–orbit model under arbitrary potential frequency μ, which can reduce to result in work (Biasco and Chierchia in J Differ Equ 246(11):4345–4370, 2009) when μ=2. It is also a generalization from low-order resonance to arbitrary-order resonance. Our proof is based on Lyapunov–Schmidt decomposition, the contraction mapping principle on Sobolev space Hs and Hρ,s and perturbation theory.
Journal Article
An attempt to build a dynamical catalog of present-day solar system co-orbitals
The main objective of this paper is to fully study 1:1 mean-motion resonance in the Solar System. We calculated stability points applying a resonant semi-analytic theory valid for any value of eccentricity or inclination. The location of each equilibrium point changes as the orbital elements of an object change, which led us to map the location of them. For the case of low inclination and low eccentricity we recovered the known L4 and L5 points. The three global types of orbits for this resonance; Tadpoles, Quasi-satellites and Horseshoes, vary as a function of the orbital elements, even disappearing for some cases. In order to build a catalog of real co-orbital objects, we filtered the NASA Horizons minor-body catalog inside the maximum resonant width and analyzed which objects are indeed in resonance. In total, we found 173 objects to be in co-orbital resonant motion with Solar System planets excluding Jupiter. We were able to recover all the already known objects and to confirm the resonant state of some new ones. Mercury remains to be the only planet with zero known co-orbitals and no L5 Earth Trojan has been discovered so far. Among the interesting identified orbits we highlight the one of 2021 FV1, a new Mars Quasi-satellite. Despite having circulating critical angles, we found some objects to be dynamically driven by the resonance such as 2021 GN1.
Journal Article
Investigation of optimal transfers to retrograde co-orbital orbits in the Earth-Moon system
Recent findings on retrograde co-orbital mean-motion resonances in the Earth-Moon system, highlight the potential use of spacecraft in retrograde resonances. Based on these discoveries, this study investigates retrograde co-orbital resonances within the Earth-Moon system, focusing on both optimal and sub-optimal orbital transfers to such configurations. The paper provides a comprehensive analysis of retrograde co-orbital resonances, optimization techniques to evaluate and enhance the performance of bi-impulsive transfers to these configurations. The results reveal the feasibility of low-cost transfers, which could support a range of future missions, including space exploration and satellite deployment. Combining advanced optimization processes, we obtained solutions for orbital transfers for different arrival points in retrograde co-orbitals improving mission efficiency and offering a cost-effective approach to interplanetary exploration.
Journal Article
Use of Transit Timing to Detect Terrestrial-Mass Extrasolar Planets
Future surveys for transiting extrasolar planets are expected to detect hundreds of jovian-mass planets and tens of terrestrial-mass planets. For many of these newly discovered planets, the intervals between successive transits will be measured with an accuracy of 0.1 to 100 minutes. We show that these timing measurements will allow for the detection of additional planets in the system (not necessarily transiting) by their gravitational interaction with the transiting planet. The transit-time variations depend on the mass of the additional planet, and in some cases terrestrial-mass planets will produce a measurable effect. In systems where two planets are seen to transit, the density of both planets can be determined without radial-velocity observations.
Journal Article