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International Journal of Current Science and Technology Vol.7, Issue, 3(A), pp. 691-694, March, 2019
ISSN: 2320-8090 RESEARCH ARTICLE
ZERO VELOCITY CURVE IN ELLIPTIC RESTRICTED THREE BODY PROBLEM WITH RADIATING PRIMARY AND OBLATE SECONDARY
Sunil Kumar Pandit
Department of Mathematics Jai Prakash University, Sadhapur, Chapra (Saran), Bihar 841301
ARTICLE INFO ABSTRACT
Article History: This paper deals with the generalized photogravitational elliptic restricted three body problem. We
Received 06th December, 2018 have supposed that bigger primary is radiating and smaller one an oblate spheroid. The stability of out Received in revised form 14th of plane libration points has been examined numerically. This model is applied on three extra solar January, 2019 planetary systems with planets in habitable zone. We conclude that these libration points are unstable Accepted 23rd February, 2019 for all three planetary systems. The Zero Velocity Curve in x-z plane is are also plotted. Published online 28th March, 2019
Key words:
Photogravitational/ ERTBP/ Oblate/ Exoplanets/ ZVC.
Copyright © 2019 Sunil Kumar Pandit,., This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
INTRODUCTION Ragos and Zagouras [11] have studied the region of stability of these equilibrium points extensively by studying periodic Radiation pressure plays a key role in the dynamical behavior solution of the system and presented the out of plane points as of sub-micrometer size grains in a star’s radiation and the saddle point of zero velocity surfaces [10]. Das etal [3] gravitational fields. The circular Restricted Three Body presented a new approach by discussing the existence and Problem (CRTBP) with the effect of the radiation pressure, stability of out of plane equilibrium points, taking the radiation when one or both primaries of the system are the source of parameter β_2 not as an independent parameter but as the radiation was discussed by Radzievsky [8,9]. The rotation of parameter dependent upon β_1, mass ratio and luminosity of celestial bodies produces an equatorial bulge, which results in the binary of P-R drag on the system. the oblateness of the body. In classical problems the primaries are taken strictly as spheres but some planets and stars are The elliptic restricted three body problem (ERTBP) sufficiently oblate to make departure form sphericity generalizes the CRTBP. by also considering the non-zero significant in the study of celestial systems. The stability of the eccentricity of the orbits of the primary. Thus the ERTBP has a triangular liberation points when PR-effect is considered in the wider applicability, although some outstanding properties of generalized photo gravitational restricted three body problem the circular model can still be adopted to the elliptical case. was studied by Kushvah and Iswar [6]. Farther they studied the Many authors ([2],[14],[7]) etc have studied the elliptical problem taking the second primary as oblate spheroid [5]. restricted three body problem in detail. Singh and Umar [13] studied the out of plane equilibrium points and their stability Simmnons etal.[12] extended the work in the circular restricted for ERTBP when both the primaries are radiating oblate problem of three bodies taking both the gravitating bodies to spheroids. be radiating. They obtained a complete solution of problem of existence and linear stability of the equilibrium points for all In this paper we have studied the equations of motion of our values of radiation pressure of both luminous bodies and all problem and found the coordinates in section 2. In section 3, values of mass ratios. It was found that there exits nine we have described Numerical application of three planetary libration points, three collinear, two triangular and four out of systems. We have examined the stability of motion and found Plane when the radiation pressure of the smaller mass is very that they are unstable. In section 4 Zero Velocity Curves have high. They have shown that L8 and L9 are always linearly been plotted in figure 4-7. Conclusions have given in section 5.nThen we write some References and at last added figures. unstable, whereas L6 and L7 are stable for small range of radiation pressure provided that both large masses are Equations of Motion luminous.
Corresponding author: Sunil Kumar Pandit The equations of Motion of an infinitesimal mass under the Department of Mathematics Jai Prakash University, Sadhapur, combined influence of oblateness of primary and radiation Chapra (Saran), Bihar 841301 pressure in a non-dimensional rotating –pulsating barycentric co-ordinate system (x, y, z) [13], are given as follows: International Journal of Current Science and Technology Vol.7, Issue, 3(A), pp. 691-694, March, 2019
″ ′ ∂Ω Stability of the Planetary Systems x − 2y = ∂ We have numerically calculated the roots characteristic Ω y″ + 2x′ = (1) equation for different values A2 for the three planetary systems shown in Table 2, 3 and 4, and found that out of plane Ω z″ = libration points are unstable for all the three planetary systems considered. Where, Φ Ω = (1 − e ) + (2)