Dynamics Around an Asteroid Modeled as a Mass Tripole

Santos, L. B. T.; Marchi, L. O.; Sousa-Silva, P. A.; Sanchez, Diogo M.; Aljbaae, S.; Prado, A. F. B. A.

doi:10.22201/ia.01851101p.2020.56.02.09

Cited by 3 publications

(1 citation statement)

References 34 publications

(62 reference statements)

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“…Lan et al (2017) showed that, from five parameters (which are determined with the help of the polyhedral model), it is possible to define the geometric shape and to obtain the physical characteristics of a real asteroid and to obtain its gravitational field. In order to generalize the work of Lan et al (2017), Barbosa Torres dos Santos et al (2020 investigate the qualitative dynamics in the vicinity of an asteroid with an convex shape using a rotating tripole model from a semi-analytical study.…”

Section: Introductionmentioning

confidence: 99%

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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Section: Introductionmentioning

confidence: 99%

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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Dynamical Evaluation of Gravity Spherical Harmonic Coefficients due to Generally Shaped Polyhedra

Gavriilidou,

Tsoulis

2024

International Association of Geodesy Symposia

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The gravitational potential uncertainty process arising from the stochastic consideration of generally shaped polyhedra is outlined and tested on the real shape model of asteroid Psyche. The examined method is based on the computation of partial derivatives of spherical harmonic coefficients as implied by corresponding coordinate changes of the polyhedron’s vertices, while the derived results are compared with gravity signal differences induced by the shape’s variations using the line integral analytical approach. For the numerical tests, 3 regular grids of points with dimensions 600 km2 were considered. The differences of the obtained results between the two approaches range from 85 m2/s2 to 300 m2/s2 for the gravitational potential uncertainties and from 2% to 2.4% for the normalized gravitational potential uncertainties. Additional tests were carried out on different points with increasing distance from the asteroid’s surface to correlate the computed uncertainties with the spherical harmonic coefficients’ maximum degree of expansion. As seen, inside the uncertainty region defined by the boundary of Brillouin sphere, the computed normalized gravitational potential uncertainties differ at the level of 0.04% for solutions of maximum degree of expansion {5, 10, 15, 20} while outside they gradually become identical. Therefore, the position of the computation points as well as the morphology of the examined mass distribution that defines the Brillouin sphere seem to strongly affect the derived results.

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Dynamics around small irregularly shaped objects modeled as a mass dipole

Abozaid,

Radwan,

Ibrahim

et al. 2024

Sci Rep

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In this work, we investigate the dynamics of a spacecraft near two primary bodies. The massive body is considered to have a spherical shape, while the less massive one is elongated and modeled as a dipole. The dipole consists of two connected masses, one is spherical and the other is an oblate spheroid. The gravitational potential of the elongated body is determined by four independent parameters. To study the dynamics, we construct the equations of motion of a spacecraft with negligible mass under the effect of the current force model. The existence and locations of the equilibrium points are analyzed for various values of the system parameters. We found that the existence and locations of the points are affected by the system parameters. Also, we studied the linear stability of the equilibrium points. We found some stable collinear points when the oblateness parameter is negative, otherwise the points are not stable. We used the curves of zero velocity to identify the regions of allowed motion. Furthermore, we discussed the 2001 SN263 asteroid system and found some stable collinear points when the oblateness parameter is negative. In addition, the triangular points of the system are stable in a linear sense.

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Dynamics Around an Asteroid Modeled as a Mass Tripole

Cited by 3 publications

References 34 publications

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

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

Dynamical Evaluation of Gravity Spherical Harmonic Coefficients due to Generally Shaped Polyhedra

Dynamics around small irregularly shaped objects modeled as a mass dipole

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