Linear stability of the triangular equilibrium points in the photogravitational elliptic restricted problem. II

Details Linear stability of the triangular equilibrium points in the photogravitational elliptic restricted problem. II Linear stability of the triangular equilibrium points in the photogravitational elliptic restricted problem. II

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.199...23m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 199, no. 1, p. 23-33.

Astronomy and Astrophysics

Astrophysics

3

Eccentric Orbits, Eigenvalues, Gravitational Effects, Lagrangian Equilibrium Points, Mass Distribution, Radiation Pressure, Three Body Problem, Equations Of Motion, Linearization

Scientific paper

The linear stability of the triangular equilibrium points in the photogravitational elliptic restricted three-body problem is examined, and the stability regions are determined in the space of the parameters of mass, eccentricity, and radiation pressure, in the case of equal radiation factors of the two primaries. The full range of values of the common radiation factor is explored from the gravitational case q1 = q2 = q = 1 down to the critical value of q = 1/8 at which the triangular equilibria disappear by coalescing on the rotating axis of the primaries. It is found that radiation pressure exerts a significant influence on the stability regions. There exist values of the common radiation factor, in the range considered, for which the triangular equilibrium points are stable for the entire range of mass distribution among the primaries and for large eccentricities of their orbits.

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