scholarly journals Effect of Oblateness of the Secondary up to J4 on L4,5 in the Photogravitaional ER3BP

2020 ◽  
Vol 13 ◽  
pp. 1-16
Author(s):  
Rukkayat Suleiman ◽  
Jagadish Singh ◽  
Aishetu Umar
Keyword(s):  
Radiation Pressure ◽  
Secular Perturbation ◽  
Triangular Points ◽  
Effects Of Radiation ◽  
Oblate Secondary ◽  
Dimensionless Coordinate

In a synodic-pulsating dimensionless coordinate, with a luminous primary and an oblate secondary, we examine the effects of radiation pressure, oblateness (quadruple and octupolar i.e. ) and eccentricity of the orbits of the primaries on the triangular points in the ER3BP. have been shown to disturb the motion of an infinitesimal body and particularly has significant effects on a satellite’s secular perturbation and orbital precessions. The influence of these parameters on the triangular points of Zeta Cygni, 54 Piscium and Procyon A/B are highlighted in this study. Triangular points are stable in the range and their stability is affected by said parameters.

Optomechanical Interactions

2020 ◽  
pp. 105-128
Author(s):  
Ivan Favero
Keyword(s):  
Radiation Pressure ◽  
Hamiltonian Formulation ◽  
Mechanical Action ◽  
Gradient Force ◽  
Optical Forces ◽  
Hamiltonian Description ◽  
Optomechanical Systems ◽  
Equal Footing ◽  
Scientific Potential ◽  
Effects Of Radiation

Light exerts mechanical action on matter through various mechanisms, the most famous being radiation pressure, with the associated picture of a photon bouncing on a perfectly reflective movable mirror and transferring twice its momentum. But still today, unambiguously observing the effects of radiation pressure remains a challenge. In the quantum domain, the radiation pressure interaction between a moving mirror and light stored in a cavity accepts a simple Hamiltonian formulation. But this Hamiltonian description is sometimes oversimplified and underestimates or misses other mechanical effects of light accompanying radiation pressure in experiments. In this chapter, we will not only address radiation pressure but also other relevant optical forces such as the optical gradient force, electrostriction, or the photothermal and optoelectronic forces, which are key in micro- and nanoscale devices and must all be controlled on an equal footing to fully harness the technological and scientific potential of miniature optomechanical systems.

scholarly journals Unveiling Perturbing Effects of P-R Drag on Motion around Triangular Lagrangian Points of the Photogravitational Restricted Problem of Three Oblate Bodies

2021 ◽  
pp. 10-31
Author(s):  
Tajudeen Oluwafemi Amuda ◽  
Oni Leke ◽  
Abdulrazaq Abdulraheem
Keyword(s):  
Radiation Pressure ◽  
Equilibrium Points ◽  
Three Body Problem ◽  
Small Perturbations ◽  
Lagrangian Points ◽  
Triangular Points ◽  
Oblate Spheroids ◽  
The Stability ◽  
Zero Velocity Surfaces ◽  
Three Body

The perturbing effects of the Poynting-Robertson drag on motion of an infinitesimal mass around triangular Lagrangian points of the circular restricted three-body problem under small perturbations in the Coriolis and centrifugal forces when the three bodies are oblate spheroids and the primaries are emitters of radiation pressure, is the focus of this paper. The equations governing the dynamical system have been derived and locations of triangular Lagrangian points are determined. It is seen that the locations are influenced by the perturbing forces of centrifugal perturbation and the oblateness, radiation pressure and, P-R drag of the primaries. Using the software Mathematica, numerical analysis are carried out to demonstrate how the dynamical elements: mass ratio, oblateness, radiation pressure, P-R drag and centrifugal perturbation influence the positions of triangular equilibrium points, zero velocity surfaces and the stability. Our investigation reveals that, though the radiation pressure, oblateness and centrifugal perturbation decrease region of stability when motion is stable, however, they are not the influential forces of instability but the P-R drag. In the region when motion around the triangular points are stable an inclusion of the P-R drag of the bigger primary even by an almost negligible value of 1.04548*10-9 overrides other effect and changes stability to instability. Hence, we conclude that the P-R drag is a strong perturbing force which changes stability to instability and motion around triangular Lagrangian points remain unstable in the presence of the P-R drag.

scholarly journals Location of triangular equilibrium points in the perturbed CR3BP with laser radiation pressure and oblateness

2018 ◽  
Vol 6 (1) ◽  
pp. 8
Author(s):  
Nabawia Khalifa
Keyword(s):  
Laser Radiation ◽  
Radiation Pressure ◽  
Analytical Study ◽  
Equilibrium Points ◽  
Laser Beam Propagation ◽  
Three Body Problem ◽  
Numerical Application ◽  
Triangular Points ◽  
First Order ◽  
Three Body

This paper represents a semi-analytical study of the effect of ground-based laser radiation pressure on the location of triangular points in the framework of the planar circular restricted three-body problem (CR3BP). The formulation includes both the effects of oblateness of J2 in addition to laser radiation pressure, where laser’s disturbing function expanded in Legendre polynomials up to the first order. Earth-Moon system is considered in which a laser station is located on Earth and sends laser beams toward the infinitesimal body. The model takes into account the effect of Earth's atmosphere on laser beam propagation. The numerical application emphasis that the location of the triangular points affected by the considered perturbations.

scholarly journals Angular Velocity Distribution in Rotating Massive Stars

1967 ◽  
Vol 20 (6) ◽  
pp. 651
Author(s):  
MPC Legg
Keyword(s):  
Angular Velocity ◽  
Velocity Distribution ◽  
Radiation Pressure ◽  
Electron Scattering ◽  
Differential Rotation ◽  
Meridional Circulation ◽  
Massive Stars ◽  
Effects Of Radiation ◽  
Uniform Composition

The angular velocity distribution in rotating massive stars with uniform composition and opacity due to electron scattering is calculated on the assumption that meridional circulation is neglible. The effects of radiation pressure are taken into account in the determination of the differential rotation and the angularvelocity is assumed to be ndependent of latitude.

The effects of radiation pressure on stellar stability

1988 ◽  
Vol 327 ◽  
pp. 801 ◽  
Author(s):  
R. F. Stellingwerf ◽  
A. Gautschy
Keyword(s):  
Radiation Pressure ◽  
Stellar Stability ◽  
Effects Of Radiation

scholarly journals Problems of Gas Dynamics in Planetary Nebulae

1968 ◽  
Vol 34 ◽  
pp. 236-248
Author(s):  
F.D. Kahn
Keyword(s):  
Simple Model ◽  
Radiation Pressure ◽  
Spherical Symmetry ◽  
Planetary Nebula ◽  
Gas Dynamics ◽  
Ionization Front ◽  
Expansion Velocity ◽  
Recoil Pressure ◽  
Initial Acceleration ◽  
Effects Of Radiation

The expansion of a typical planetary nebula is studied by means of a simple model, with spherical symmetry. It is shown that there is a build-up of radiation pressure, due to Lyman-α photons trapped in the nebula, and that this causes the initial acceleration outwards. After some 1·5 × 1011 sec the nebula will have a radius of the order of 1017 cm, and an expansion velocity of about 2 × 106 cm/sec. At roughly this time the dynamical effects of radiation pressure begin to be superseded by those of the recoil pressure at the ionization front, which continues to dominate until the nebula is fully ionized.Finally some reasons are considered why most nebulae do not have spherically symmetrical shapes, but why so often they appear to be ring-like or butterfly-shaped.

scholarly journals Effects of radiation pressure and earth’s oblatness on high altitude artificial satellite orbit

10.4081/708 ◽  
2011 ◽  
Vol 1 (1) ◽  
pp. e2
Author(s):  
Khalil I. Khalil ◽  
Mohamed N.S. Ismail
Keyword(s):  
High Altitude ◽  
Radiation Pressure ◽  
Artificial Satellite ◽  
Equations Of Motion ◽  
Satellite Orbit ◽  
Artificial Satellites ◽  
Runge Kutta Method ◽  
Ks Variables ◽  
Effects Of Radiation ◽  
Earth’S Oblateness

This paper is devoted to study the effects of radiation pressure together with tesseral and zonal harmonics on the high altitude artificial satellites orbits. The equations of motion were regularized by using the KS variables and the problem was solved numerically using the fourth order of Runge Kutta method. A numerical testing was performed on Lageos-1 satellite in order to analyze its orbital changes due to effects of both radiation pressure and Earth's oblateness.

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