Searching for Less-Disturbed Orbital Regions Around the Near-Earth Asteroid 2001 SN263

Sanchez, Diogo M.; Prado, A. F. B. A.

doi:10.2514/1.a34402

Cited by 10 publications

(6 citation statements)

References 33 publications

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“…However, the SRP destabilized about 50% of them, changing their distribution in the (dy 0 , h) plane. Such a drastic effect of the SRP was already seen in Chanut et al (2017) studying the dynamics around the asteroid Bennu, and also in Sanchez and Prado (2019) studying the Less-Disturbed Orbital Regions Around the Near-Earth Asteroid 2001 SN 263 .…”

Section: Close Approach With Earthmentioning

confidence: 68%

First approximation for spacecraft motion relative to (99942) Apophis

Aljbaae,

Sanchez,

Prado

et al. 2020

Preprint

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We aim at providing a preliminary approach on the dynamics of a spacecraft in orbit about the asteroid (99942) Apophis during its Earth close approach. The physical properties from the polyhedral shape of the target are derived assigning each tetrahedron to a point mass in its center. That considerably reduces the computation processing time compared to previous methods to evaluate the gravitational potential. The surfaces of section close to Apophis are build considering or not the gravitational perturbations of the Sun, the planets, and the SRP. The Earth is the one that most affects the invisticated region making the vast majority of the orbits to collide or escape from the system. Moreover, from numerical analysis of orbits started on March 1, 2029, the less perturbed region is characterized by the variation of the semimajor axis of 40-days orbits, which do not exceed 2 km very close to the central body (a < 4 km, e < 0.4). However, no regions investigated could be a possible option for inserting a spacecraft into natural orbits around Apophis during the close approach with our planet. Finally, to solve the stabilization problem in the system, we apply a robust path following control law to control the orbital geometry of a spacecraft. At last, we present an example of successful operation of our orbit control with a total v of 0.495 m/s for 60 days. All our results are gathered in the CPM-ASTEROID database, which will be regularly updated by considering other asteroids.

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Section: Close Approach With Earthmentioning

confidence: 68%

First approximation for spacecraft motion relative to (99942) Apophis

Aljbaae,

Sanchez,

Prado

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…On the other hand, orbits with low or almost zero values of PI iv could be stable. Additionally, as seen in Sanchez & Prado (2019), periodic orbits would appear with near zero values in both PMaps of type II and IV. However, there is an exception to these rules: resonances.…”

Section: Pmap Of Type IVmentioning

confidence: 78%

“…In this context, this paper aims to investigate the dynamics of particles around Haumea, in the region where the ring of Haumea was found, i.e., particles with semimajor axis from 2000 km to 2500 km. To investigate the behaviour of these particles, we use Perturbation Maps (Sanchez & Prado 2019). These maps are grids of initial conditions that show how much the perturbations, coming from several sources in the system, such as those from the moons of Haumea, affect the orbital motion of these particles.…”

Section: Introductionmentioning

confidence: 99%

Perturbation Maps and the ring of Haumea

Sanchez

Deienno

Prado

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT The dwarf planet Haumea is a trans-Neptunian object that is orbited by two moons and has a recently discovered ring. The particles of this ring are near the 3:1 resonance between the spin of Haumea and the orbital motion of the particles. In this work, the ring of Haumea is investigated using Perturbation Maps. These maps show the behaviour and impact of perturbations acting over particles around Haumea. The information coming from the maps depends on the integral type for the disturbing acceleration used to build the maps. The types II and IV are used. The numerical simulations are focused in the region between 2000 and 2500 km from the centre of Haumea, which is the region where the ring was observed, considering two initial values for the 3:1 resonant angle: θres = 0° and θres = 270°. The possible stable region for the initial angle θres = 0° is larger than the stable region for the initial angle θres = 270°. Furthermore, we found that these stable regions are not continuous, indicating that there are possible gaps in the ring. Therefore, our results suggest that Haumea may not have only one single ring, but a system of rings instead. Possible transit of the particles between the ring and the region close to the orbit of Namaka is also shown.

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“…On the other hand, there is a large region with solutions that remain bounded around 243 Ida when we consider retrograde orbits and 𝑎 0 < 200 km, as shown in Fig. 12b (Sanchez & Prado 2019). Note that this region exist even when the eccentricity is high.…”

Section: Numerical Simulations Methodologymentioning

confidence: 88%

A particle-linkage model for elongated asteroids with three-dimensional mass distribution

Santos

Marchi

Aljbaae

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The goal of the present paper is to develop a simplified model to describe the gravitational fields of elongated asteroids. The proposed model consists of representing an elongated asteroid using a triple-particle-linkage system distributed in the three-dimensional space and it is an extension of previous planar models. A non-linear optimisation method is used to determine the parameters of our model, minimising the errors of all the external equilibrium points with respect to the solutions calculated with a more realistic approach, the Mascon model, which are assumed to give the real values of the system. The model considered in this article is then applied to three real irregular asteroids: 1620 Geographos, 433 Eros, and 243 Ida. The results show that the current triple-particle-linkage three-dimensional model gives better accuracy when compared to the axisymmetric triple-particle-linkage model available in the literature, and provides an advantage in terms of accuracy over the mass point model, while keeping computational time low. This model is also used to carry out simulations to characterise regions with solutions that remain bounded or that escape from around each asteroid under analysis. We investigated initial inclinations of 0○ (direct orbits) and 180○ (retrograde orbits). We considered the gravitational field of the asteroid, the gravitational attraction of the Sun, and the SRP. Our results are then compared to the results obtained using the Mascon gravitational model, based on the polyhedral shape source. We found good agreement between the two models.

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Searching for Less-Disturbed Orbital Regions Around the Near-Earth Asteroid 2001 SN263

Cited by 10 publications

References 33 publications

First approximation for spacecraft motion relative to (99942) Apophis

First approximation for spacecraft motion relative to (99942) Apophis

Perturbation Maps and the ring of Haumea

A particle-linkage model for elongated asteroids with three-dimensional mass distribution

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