The stability of inner collinear equilibrium points in the photogravitational elliptic restricted problem

Details The stability of inner collinear equilibrium points in the photogravitational elliptic restricted problem The stability of inner collinear equilibrium points in the photogravitational elliptic restricted problem

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.199..139m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 199, no. 1, p. 139-146.

Astronomy and Astrophysics

Astrophysics

6

Eccentric Orbits, Mass Distribution, Radiation Pressure, Three Body Problem, Collinearity, Equilibrium Equations

Scientific paper

The linear stability of the inner collinear equilibrium point of 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. The case of equal radiation factors of the two primaries is considered, and the full range of values of the common radiation factor is explored, from the case q1 = q2 = q = 1/8 at which the triangular equilibria disappear by coalescing on the rotating axis of the primaries transferring their stability to the collinear point, down to q = 0 at which value the stability regions in the micron plane disappear by shrinking down to zero size. It is found that radiation pressure exerts a significant influence on the stability regions. For certain intervals of radiation values these regions become qualitatively different from the gravitational case as well as the solar system case. There exist values of the common radiation factor, in the range considered, for which the collinear equilibrium point is stable for the entire range of mass distribution among the primaries and for large eccentricities of their orbits.

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