Production of defects in molybdenum by a deuterium glow discharge plasma

Chernikov, V.N.; Arutyunova, G. A.; Sokurskii, Yu. N.; Захаров, А.П.

doi:10.1007/bf01142146

Cited by 4 publications

(2 citation statements)

References 16 publications

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“…In order to make CRTBP model closer to the reality, various adjustments have been made, including the incorporation of additional parameters. For instance, the radiation pressure has to be incorporated when the primaries emit radiation such as the stars [4,5,6]. The non-spherical nature of stars and planets, referred to as oblateness, has been taken into account [7,8,9].…”

Section: Introductionmentioning

confidence: 99%

Stability Analysis of Modified Circular Restricted Three Body Problem by Lyapunov Exponent Indicators

Nugraha,

Nurul Huda,

Kuntjoro

et al. 2024

J. Phys.: Conf. Ser.

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The circular restricted three body problem (CRTBP) is a well-known problem that has a very important contribution to understand the dynamics of celestial objects, including the binary stars and planetary system. In this study, we extend the classical version of CRTBP by assuming both primaries emit radiation and have oblate shape. We also consider the potential from a disk like structure that surrounds this three-body system. The stability of the infinitesimal body is investigated by using Lyapunov Exponent Indicators (LEI). First, we have done a numerical survey by testing several initial locations of the infinitesimal body that have chaotic or regular orbital behaviour. Second, we estimated the stability of triangular equilibrium points and show that the equilibrium points are conditionally stable with respect to the critical mass parameter (μc ). We found that the determined μc from LEI method match μc from linear stability analysis.

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Section: Introductionmentioning

confidence: 99%

Stability Analysis of Modified Circular Restricted Three Body Problem by Lyapunov Exponent Indicators

Nugraha,

Nurul Huda,

Kuntjoro

et al. 2024

J. Phys.: Conf. Ser.

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“…They also found four additional out of plane equilibrium points L 6 , L 7 , L 8 and L 9 . Many researchers (Chernikov 1970;Meyer & Schmidt 1986;Liou et al 1995;Ragos & Zafiropoulos 1995;Haque & Ishwar 1995;Goździewski 1998;Abouelmagd & El-Shaboury 2012;Singh & Taura 2013) have discussed the dynamical behavior in the photo-gravitational restricted three body problem. The effect of radiation pressure and PR-Drag are examined by (Das et al 2008) during the study of motion of dust particles in the steller binary systems: RW-Monocerotis and Krüger 60.…”

Section: Introductionmentioning

confidence: 99%

Effects of the albedo and disc on the zero velocity curves and linear stability of equilibrium points in the generalized restricted three-body problem

Yousuf

Kishor

2019

Monthly Notices of the Royal Astronomical Society

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The most important aspects of a dynamical system are its stability and the factors which affects the stability property. This paper presents the analysis of the effects of albedo and disc on the zero velocity curves, existence of equilibrium points and on their linear stability in a generalized restricted three body problem that consists of motion of an infinitesimal mass under the uniform gravity field of radiating-oblate primary, oblate secondary and a disc, which is rotating about the common center of the mass of the system. A significant effect of albedo and disc are observed on the zero velocity curves, positions of equilibrium points and on the stability region. Linear stability analysis of collinear equilibrium points is performed with respect to mass ratio µ and albedo parameter of secondary, separately and it is found that these are unstable in both the cases. On the other hand, non-collinear equilibrium point is stable in a certain range of mass ratio. After analyzing individual as well as combined effect of radiation pressure force of the primary, albedo of secondary, oblateness of both the massive bodies and the disc, it is found that these perturbations play a significant on the motion of infinitesimal mass in the vicinity of equilibrium points. These results may be help to analyze more generalized problem of few bodies under the influence of different kind of perturbations such as P-R drag, solar wind drag etc. Present study is limited to the regular symmetric disc which will extend later.

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