Analysis of nominal halo orbits in the Sun–Earth system

Abouelmagd, Elbaz I.; Pal, Ashok; Guirao, Juan Luis García

doi:10.1007/s00419-021-02031-y

Cited by 13 publications

(6 citation statements)

References 41 publications

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“…We should especially remark (see [8]) that for using of the time-dependent eccentricity e(t) in Eqns ( 2)-(3) or equivalently in Eqns. (5) we should first solve Eqn. (1) with aim of expressing time t via true anomaly f (independent variable in (2)-( 3)).…”

Section: The Way Of Taking Into Account the Variable Eccentricity E(f...mentioning

confidence: 99%

“…of ER3BP allows to take into account the effect of tidal phenomena on orbital motions of primaries which are participating in dynamical effects in these equations, during a long-time period. Thus insofar, equations of motion (ER3BP) (5) depend on the aforementioned variable eccentricity.…”

Section: The Way Of Taking Into Account the Variable Eccentricity E(f...mentioning

confidence: 99%

“…Participants of Celestial mechanics community know a lot of modern and old works presenting outstanding results in R3BP (e.g. [1][2][3][4][5][6][7], but not limited to).…”

Section: Introductionmentioning

confidence: 99%

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On the Motion of Small Satellite near the Planet in ER3BP

2021

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In the current study, we explore stability of motion of satellite around the natural moons of planets in Solar system using the novel concept of ER3BP with variable eccentricity. This concept was introduced earlier when novel type of ER3BP (Sunplanet-satellite) was investigated with variable spin state of secondary planet correlated implicitly to the motion of satellite (in the synodic co-rotating Cartesian coordinate system) for its trapped orbit near the secondary planet (which is involved in kepler duet "Sun-planet"). But it is of real interest to explore another kind of aforedescribed problem, ER3BP (planet-moon-satellite) with respect to investigation of motion of satellite m around the natural moon m moon of planet in Solar system with variable eccentricity of the moon in its motion around the planet. So, we consider here two primaries, M planet and m moon, the last is orbiting around their common barycenter on quasi-elliptic orbit with slow-changing, not constant eccentricity (on a large-time scale) due to tidal phenomena. Our aim is to investigate motion of small dot satellite around the natural moon of planet on quasistable elliptic orbit. Both novel theoretical and numerical findings (for various cases of trio "planet-moon-satellite") are presented in the current research.

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Section: The Way Of Taking Into Account the Variable Eccentricity E(f...mentioning

confidence: 99%

Section: The Way Of Taking Into Account the Variable Eccentricity E(f...mentioning

confidence: 99%

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On the Motion of Small Satellite near the Planet in ER3BP

2021

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“…Equations of the restricted three-body problem R3BP present the dynamical model of motion of a mini-planetoid with a small mass under the governing combined action of Newtonian gravity by two large bodies (called primaries in celestial mechanics), dancing in their mutual celestial motion on Kepler planar orbits around a barycenter. The celestial mechanics community has seen many modern and old studies presenting outstanding results in R3BP (e.g., [1][2][3][4][5][6][7][8][9][10], but not limited to these).…”

Section: Introductionmentioning

confidence: 99%

Finite-Sized Orbiter’s Motion around the Natural Moons of Planets with Slow-Variable Eccentricity of Their Orbit in ER3BP

et al. 2023

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This article is devoted to the study of the stability of movement of a satellite of finite size around the natural satellites of the planets in the solar system, using the new concept of ER3BP with variable eccentricity. This concept was introduced earlier for the variable spin state of a secondary planet correlated implicitly to the motion of the satellite for its trapped orbit near the secondary planet (which is involved in the Kepler duet “Sun-planet”). But it is of real interest to explore another kind of this problem, plane ER3BP “planet-moon-satellite”. Here, we consider two primary celestial bodies, a planet and a moon, the latter revolves around its common barycenter in a quasi-elliptical orbit in a fixed plane (invariable plane) around the planet with a slowly varying eccentricity on a large time scale due to tidal phenomena. This study presents both new theoretical and numerical results for various cases of the “planet-moon-satellite” trio.

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“…The part of the sun that is often observed directly is the surface or atmosphere, which consists of 3 layers: the photosphere, chromosphere, and corona. Meanwhile, solar activities that can be easily observed from the Earth are sunspot and flare [2].…”

Section: Introductionmentioning

confidence: 99%

Analysis of Flare Occurring Based on Sunspot Changing Patterns Using Zurich Method in February – April 2022 at the Astronomy Laboratory of Physics FMIPA State University of Malang

Yogihati

Shofi²,

Heriyanto³

2022

J. Phys.: Conf. Ser.

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The star closest to our Earth is the sun with an average distance of 149,680,000 km. The sun is plasma with a very high temperature. The most easily observed solar activity from Earth are sunspots and flares, where flares on the sun can affect the Earth’s atmosphere. Therefore with this, research was carried out in February - April 2022 at the Laboratory of Astronomy Physics, State University of Malang with a geographical location of 07° 57’ 39” South Latitude, 112° 37’ 9.2” East Longitude, and 7.9607° North Latitude at an altitude of 465 meters with using the Celestron telescope. This study aims to determine the pattern of changes in sunspots until the occurrence of flare, and to find out how to determine the occurrence of flare. This study used a descriptive approach based on the daily data that had been observed. In classifying sunspots, the Zurich method is used. The development of sunspots obtained in daily data shows changes in sunspot development patterns and data on the influence of flares that occur on the surface of the Earth such as satellite damage and auroras reported by NASA show that flare occur on the surface of the sun. Based on the analysis of sunspot classification, it shows that flares occur in classes C, D, E, and F. The occurrence of these flares can be seen in the news released by NOAA. It can be concluded that flares do not always occur in large class sunspot classifications. However, the small class was able to produce a flare.

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Analysis of nominal halo orbits in the Sun–Earth system

Cited by 13 publications

References 41 publications

On the Motion of Small Satellite near the Planet in ER3BP

On the Motion of Small Satellite near the Planet in ER3BP

Finite-Sized Orbiter’s Motion around the Natural Moons of Planets with Slow-Variable Eccentricity of Their Orbit in ER3BP

Analysis of Flare Occurring Based on Sunspot Changing Patterns Using Zurich Method in February – April 2022 at the Astronomy Laboratory of Physics FMIPA State University of Malang

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