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Title: MOTION IN THE PHOTOGRAVITATIONAL ELLIPTIC RESTRICTED THREE-BODY PROBLEM UNDER AN OBLATE PRIMARY

Abstract

This paper studies the motion of an infinitesimal mass around seven equilibrium points in the framework of the elliptic restricted three-body problem under the assumption that the primary of the system is a non-luminous, oblate spheroid and the secondary is luminous. A practical application of this case could be the study of the dynamical evolution of dust particles in orbits around a binary system with a dark degenerate primary and a secondary stellar companion. Conditional stability of the motion around the triangular points exists for 0 < {mu} < {mu}{sub c}, where {mu} is the mass ratio. The critical mass ratio value {mu}{sub c} depends on the combined effect of radiation pressure, oblateness, eccentricity, and the semimajor axis of the elliptic orbits; an increase in any of these parameters has destabilizing results on the orbits of the test particles. The overall effect is therefore that the size of the region of stability decreases when the value of these parameters increases. The collinear points and the out-of-plane equilibrium points are found to be unstable for any combination of the parameters considered here. Further, a numerical exploration computing the positions of the triangular points and the critical mass ratio of two binariesmore » RX J0450.1-5856 and Nova Cen 1969 (Cen X-4) is given.« less

Authors:
;  [1]
  1. Department of Mathematics, Faculty of Science, Ahmadu Bello University, Zaria (Nigeria)
Publication Date:
OSTI Identifier:
22034646
Resource Type:
Journal Article
Journal Name:
Astronomical Journal (New York, N.Y. Online)
Additional Journal Information:
Journal Volume: 143; Journal Issue: 5; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 1538-3881
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTRONOMY; ASTROPHYSICS; COSMIC DUST; CRITICAL MASS; EQUILIBRIUM; EVOLUTION; MECHANICS; ORBITS; PARTICLES; PULSARS; RADIATION PRESSURE; SPHEROIDS; STABILITY; TEST PARTICLES; THREE-BODY PROBLEM; WHITE DWARF STARS

Citation Formats

Singh, Jagadish, and Umar, Aishetu. MOTION IN THE PHOTOGRAVITATIONAL ELLIPTIC RESTRICTED THREE-BODY PROBLEM UNDER AN OBLATE PRIMARY. United States: N. p., 2012. Web. doi:10.1088/0004-6256/143/5/109.
Singh, Jagadish, & Umar, Aishetu. MOTION IN THE PHOTOGRAVITATIONAL ELLIPTIC RESTRICTED THREE-BODY PROBLEM UNDER AN OBLATE PRIMARY. United States. https://doi.org/10.1088/0004-6256/143/5/109
Singh, Jagadish, and Umar, Aishetu. 2012. "MOTION IN THE PHOTOGRAVITATIONAL ELLIPTIC RESTRICTED THREE-BODY PROBLEM UNDER AN OBLATE PRIMARY". United States. https://doi.org/10.1088/0004-6256/143/5/109.
@article{osti_22034646,
title = {MOTION IN THE PHOTOGRAVITATIONAL ELLIPTIC RESTRICTED THREE-BODY PROBLEM UNDER AN OBLATE PRIMARY},
author = {Singh, Jagadish and Umar, Aishetu},
abstractNote = {This paper studies the motion of an infinitesimal mass around seven equilibrium points in the framework of the elliptic restricted three-body problem under the assumption that the primary of the system is a non-luminous, oblate spheroid and the secondary is luminous. A practical application of this case could be the study of the dynamical evolution of dust particles in orbits around a binary system with a dark degenerate primary and a secondary stellar companion. Conditional stability of the motion around the triangular points exists for 0 < {mu} < {mu}{sub c}, where {mu} is the mass ratio. The critical mass ratio value {mu}{sub c} depends on the combined effect of radiation pressure, oblateness, eccentricity, and the semimajor axis of the elliptic orbits; an increase in any of these parameters has destabilizing results on the orbits of the test particles. The overall effect is therefore that the size of the region of stability decreases when the value of these parameters increases. The collinear points and the out-of-plane equilibrium points are found to be unstable for any combination of the parameters considered here. Further, a numerical exploration computing the positions of the triangular points and the critical mass ratio of two binaries RX J0450.1-5856 and Nova Cen 1969 (Cen X-4) is given.},
doi = {10.1088/0004-6256/143/5/109},
url = {https://www.osti.gov/biblio/22034646}, journal = {Astronomical Journal (New York, N.Y. Online)},
issn = {1538-3881},
number = 5,
volume = 143,
place = {United States},
year = {Tue May 15 00:00:00 EDT 2012},
month = {Tue May 15 00:00:00 EDT 2012}
}