Hovering in Space: Those Mysterious Lagrangian Points

AbstractWe continue to investigate the binary system Kepler-16, consisting of a K-type main-sequence star, a red dwarf and a circumbinary Saturnian planet. As part of our study, we describe the system's habitable zone based on different climate models. We also report on stability investigations for possible Earth-mass Trojans while expanding a previous study by B. L. Quarles and collaborators given in 2012. For the climate models, we carefully consider the relevance of the system's parameters. Furthermore, we pursue new stability simulations for the Earth-mass objects starting along the orbit of Kepler-16b. The eccentricity distribution as obtained prefers values close to circular, whereas the inclination distribution remains flat. The stable solutions are distributed near the co-orbital Lagrangian points, thus enhancing the plausibility that Earth-mass Trojans might be able to exist in the Kepler-16(AB) system.

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Lagrangian Points

10.1007/springerreference_223126 ◽

2012 ◽

Keyword(s):

Lagrangian Points

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Asymptotic solutions of the restricted problem near the equilateral Lagrangian points

Celestial Mechanics ◽

10.1007/bf01227668 ◽

1985 ◽

Vol 35 (2) ◽

pp. 189-200 ◽

Cited By ~ 3

Author(s):

R. Cid ◽

S. Ferrer ◽

J. A. Caballero

Keyword(s):

Restricted Problem ◽

Asymptotic Solutions ◽

Lagrangian Points

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Location and stability of the triangular Lagrange points in photo-gravitational elliptic restricted three body problem with the more massive primary as an oblate spheroid

International Journal of Advanced Astronomy ◽

10.14419/ijaa.v7i2.29814 ◽

2019 ◽

Vol 7 (2) ◽

pp. 57

Author(s):

A. Arantza Jency ◽

Ram Krishan Sharma

Keyword(s):

Body Problem ◽

Critical Mass ◽

Oblate Spheroid ◽

Motion Equation ◽

Restricted Three Body Problem ◽

Three Body Problem ◽

Lagrangian Points ◽

Mean Motion ◽

The Mean ◽

Three Body

The triangular Lagrangian points of the elliptic restricted three-body problem (ERTBP) with oblate and radiating more massive primary are studied. The mean motion equation used here is different from the ones employed in many studies on the perturbed ERTBP. The effect of oblateness on the mean motion equation varies. This change influences the location and stability of the triangular Lagrangian points. The points tend to shift in the y-direction. The influence of the oblateness on the critical mass ratio is also altered. But the eccentricity limit for stability remains the same.

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