Analysis of nominal halo orbits in the Sun–Earth system

2021 ◽  
Author(s):  
Elbaz I. Abouelmagd ◽  
Ashok Kumar Pal ◽  
Juan Luis García Guirao
Keyword(s):  
The Sun ◽  
Earth System ◽  
Halo Orbits

Halo orbits in the vicinity of the L 2 libration point in the Sun-Earth system

2014 ◽  
Vol 52 (3) ◽  
pp. 189-204 ◽  
Author(s):  
I. S. Ilyin ◽  
V. V. Sazonov ◽  
A. G. Tuchin
Keyword(s):  
Libration Point ◽  
The Sun ◽  
Earth System ◽  
Halo Orbits

scholarly journals The Second Earth Trojan 2020 XL5

2021 ◽  
Vol 922 (2) ◽  
pp. L25
Author(s):  
Man-To Hui ◽  
Paul A. Wiegert ◽  
David J. Tholen ◽  
Dora Föhring
Keyword(s):  
Fifteenth Century ◽  
The Sun ◽  
Earth System ◽  
Eccentric Orbit ◽  
Dynamical Study ◽  
Lagrange Points ◽  
Close Encounters ◽  
Numerical Studies ◽  
The Earth

Abstract The Earth Trojans are coorbitals librating around the Lagrange points L 4 or L 5 of the Sun–Earth system. Although many numerical studies suggest that they can maintain their dynamical status and be stable on timescales up to a few tens of thousands of years or even longer, they remain an elusive population. Thus far only one transient member (2010 TK7) has been discovered serendipitously. Here, we present a dynamical study of asteroid 2020 XL5. With our meticulous follow-up astrometric observations of the object, we confirmed that it is a new Earth Trojan. However, its eccentric orbit brings it close encounters with Venus on a frequent basis. Based on our N-body integration, we found that the asteroid was captured into the current Earth Trojan status in the fifteenth century, and then it has a likelihood of 99.5% to leave the L 4 region within the next ∼10 kyr. Therefore, it is most likely that 2020 XL5 is dynamically unstable over this timescale.

Longevity of moons around habitable planets

2014 ◽  
Vol 13 (4) ◽  
pp. 324-336 ◽  
Author(s):  
Takashi Sasaki ◽  
Jason W. Barnes
Keyword(s):  
Orbital Period ◽  
Extrasolar Planets ◽  
The Sun ◽  
Habitable Zone ◽  
Evolution Theory ◽  
Earth System ◽  
The Moon ◽  
Tidal Dissipation ◽  
Habitable Planets ◽  
Rocky Planets

AbstractWe consider tidal decay lifetimes for moons orbiting habitable extrasolar planets using the constant Q approach for tidal evolution theory. Large moons stabilize planetary obliquity in some cases, and it has been suggested that large moons are necessary for the evolution of complex life. We find that the Moon in the Sun–Earth system must have had an initial orbital period of not slower than 20 h rev−1 for the moon's lifetime to exceed a 5 Gyr lifetime. We assume that 5 Gyr is long enough for life on planets to evolve complex life. We show that moons of habitable planets cannot survive for more than 5 Gyr if the stellar mass is less than 0.55 and 0.42 M⊙ for Qp=10 and 100, respectively, where Qp is the planetary tidal dissipation quality factor. Kepler-62e and f are of particular interest because they are two actually known rocky planets in the habitable zone. Kepler-62e would need to be made of iron and have Qp=100 for its hypothetical moon to live for longer than 5 Gyr. A hypothetical moon of Kepler-62f, by contrast, may have a lifetime greater than 5 Gyr under several scenarios, and particularly for Qp=100.

Fleet of satellites and ground-based instruments probes the Sun-Earth System

Eos ◽  
1996 ◽  
Vol 77 (16) ◽  
pp. 149-154 ◽  
Author(s):  
R. A. Hoffman ◽  
K. W. Ogilvie ◽  
M. H. Acuña
Keyword(s):  
The Sun ◽  
Earth System

scholarly journals Impacts of Poynting–Robertson Drag and Dynamical Flattening Parameters on Motion around the Triangular Equilibrium Points of the Photogravitational ER3BP

2021 ◽  
Vol 2021 ◽  
pp. 1-11
Author(s):  
Aishetu Umar ◽  
Aminu Abubakar Hussain
Keyword(s):  
Numerical Study ◽  
Equilibrium Points ◽  
Equations Of Motion ◽  
Research Work ◽  
Radial Component ◽  
The Sun ◽  
Earth System ◽  
Elliptic Restricted Problem ◽  
Pressure Factor ◽  
Infinitesimal Mass

Using an analytical and numerical study, this paper investigates the equilibrium state of the triangular equilibrium points L 4 ,     5 of the Sun-Earth system in the frame of the elliptic restricted problem of three bodies subject to the radial component of Poynting–Robertson (P–R) drag and radiation pressure factor of the bigger primary as well as dynamical flattening parameters of both primary bodies (i.e., Sun and Earth). The equations of motion are presented in a dimensionless-pulsating coordinate system ξ − η , and the positions of the triangular equilibrium points are found to depend on the mass ratio μ and the perturbing forces involved in the equations of motion. A numerical analysis of the positions and stability of the triangular equilibrium points of the Sun-Earth system shows that the perturbing forces have no significant effect on the positions of the triangular equilibrium points and their stability. Hence, this research work concludes that the motion of an infinitesimal mass near the triangular equilibrium points of the Sun-Earth system remains linearly stable in the presence of the perturbing forces.

scholarly journals Passive Remote Study of the Aerosol in the Upper Atmosphere of the Earth

2019 ◽  
pp. 1-6
Author(s):  
Oleksandr Zbrutskyi ◽  
◽  
Nevodovskyi P ◽  
Anatoliy Vid’machenko ◽  
◽  
...  
Keyword(s):  
Global Warming ◽  
Energy Balance ◽  
Climate Changes ◽  
Upper Atmosphere ◽  
Anthropogenic Factors ◽  
The Sun ◽  
Earth System ◽  
Relative Contribution ◽  
The Earth

Climate changes on planet Earth are mainly caused by disturbances in the energy balance of the Sun-Earth system. This process is the result of both natural changes in nature and the influence of anthropogenic factors. The combined effect of these factors can lead to threatening phenomena for mankind - a decrease in the power of the ozone layer, the formation of “ozone holes” and global warming on the planet and other disasters. The study of the causes of these factors and the determination of their relative contribution is one of the pressing problems of our time.

Sign in / Sign up

Export Citation Format

Share Document