Computation of halo orbits in the photogravitational Sun-Earth system with oblateness

Tiwary, Rishikesh Dutta; Kushvah, Badam Singh

doi:10.1007/s10509-015-2243-5

Cited by 28 publications

(22 citation statements)

References 31 publications

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“…Analytical approximation need to be combined with numerical techniques to generate a halo orbit accurate enough for mission design. In the present study, we use as the first guess for the differential correction process for obtaining halo orbits, the modified third-order approximation of Thurman and Worfolk [27] extended by Tiwary and Kushvah [23] for PRTBP using Lindstedt-Poincaré method, where more massive primary is the source of radiation and smaller primary is an oblate spheroid with its equatorial plane coincident with the plane of motion.…”

Section: Liberation Points and Halo Orbitsmentioning

confidence: 99%

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Halo Orbits at Sun-Mars L1, L2 in the Photogravitational Restricted Three-Body Problem with Oblateness

Pushparaj¹,

Sharma²

2017

AdAp

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Abstract. Photogravitational Restricted Three-Body Problem (PRTBP) with smaller primary being an oblate spheroid with its equatorial plane coincident with the plane of motion of the primaries is considered and halo orbits in the vicinity of Sun-Mars Lagrangian points L1 and L2 are computed numerically. The effects of perturbations on size, shape, location and time period of the halo orbits are studied. It is found that the increase in solar radiation pressure at constant oblateness elongates the halo orbits at L1 and the orbits move towards the radiating body. At L2, the halo orbits shrink and move towards the smaller primary with increase in solar radiation pressure at constant oblateness. For constant radiation pressure, increase in oblateness causes the location of L1 and L2 halo orbits to move away from the smaller primary. The time period of L1 halo orbits increases with increase in radiation pressure for constant oblateness and decreases with increase in oblateness for constant radiation pressure. However, the effect of solar radiation pressure and oblateness for L2 halo orbits is reversed.

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Section: Liberation Points and Halo Orbitsmentioning

confidence: 99%

“…The PRTBP with oblateness effect arises from the classical problem if at least one of the primaries is an intense emitter of radiation and the other primary is an oblate spheroid as in Sharma [16] and Tiwary and Kushvah [23]. Radzievskii [13] formulated the PRTBP and studied it for three specific bodies: Sun, a planet and a dust particle.…”

Section: Introductionmentioning

confidence: 99%

Halo Orbits at Sun-Mars L1, L2 in the Photogravitational Restricted Three-Body Problem with Oblateness

Pushparaj¹,

Sharma²

2017

AdAp

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“…The distance between these Lagrangian points and the smaller primary is considered to be the normalized unit as in Koon et al [14] and Tiwary and Kushvah [12].…”

Section: Computation Of Halo Orbitsmentioning

confidence: 99%

“…Figure 8 shows the comparison between them. The analytical solution which includes the radiation pressure of more massive primary and oblateness of the smaller primary can improve the accuracy over the existing solution as given by Tiwary and Kushvah [12].…”

Section: Numerically Generated Halo Orbitsmentioning

confidence: 99%

“…Sharma [11] studied the periodic orbits around the Lagrangian points in the planar RTBP by considering Sun as source of radiation and smaller primary as an oblate spheroid with its equatorial plane coincident with the plane of motion. Tiwary and Kushvah [12] followed the model of Sharma [11] to study the halo orbits around the Lagrangian points L 1 and L 2 analytically. However, they did not consider the z term in oblateness in their study.…”

Section: Introductionmentioning

confidence: 99%

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Halo Orbits around Sun-Earth L1 in Photogravitational Restricted Three-Body Problem with Oblateness of Smaller Primary

Chidambararaj¹,

Sharma²

2016

IJAA

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This paper deals with generation of halo orbits in the three-dimensional photogravitational restricted three-body problem, where the more massive primary is considered as the source of radiation and the smaller primary is an oblate spheroid with its equatorial plane coincident with the plane of motion. Both the terms due to oblateness of the smaller primary are considered. Numerical as well as analytical solutions are obtained around the Lagrangian point L1, which lies between the primaries, of the Sun-Earth system. A comparison with the real time flight data of SOHO mission is made. Inclusion of oblateness of the smaller primary can improve the accuracy. Due to the effect of radiation pressure and oblateness, the size and the orbital period of the halo orbit around L1 are found to increase.

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Analysis of nominal halo orbits in the Sun–Earth system

2021

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Computation of halo orbits in the photogravitational Sun-Earth system with oblateness

Cited by 28 publications

References 31 publications

Halo Orbits at Sun-Mars L1, L2 in the Photogravitational Restricted Three-Body Problem with Oblateness

Halo Orbits at Sun-Mars L1, L2 in the Photogravitational Restricted Three-Body Problem with Oblateness

Halo Orbits around Sun-Earth L1 in Photogravitational Restricted Three-Body Problem with Oblateness of Smaller Primary

Analysis of nominal halo orbits in the Sun–Earth system

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