TY - MGZN
AU - Cors, J.
AU - Llibre, J.
T2 - Celestial mechanics and dynamical astronomy
Y1 - 2004
VL - 90
IS - 1-2
SP - 13
EP - 33
DO - 10.1007/s10569-004-4917-0
UR - http://link.springer.com/article/10.1007%2Fs10569-004-4917-0
AB - We have two mass points of equal masses m 1=m 2 > 0 moving under Newtonâ€™s law of attraction in a non-collision parabolic orbit while their center of mass is at rest. We consider a third mass point, of mass m 3=0, moving on the straight line L perpendicular to the plane of motion of the first two mass points and passing through their center of mass. Since m 3=0, the motion of m 1 and m 2 is not affected by the third and from the symmetry of the motion it is clear that m 3 will remain on the line L. The parabolic restricted three-body problem describes the motion of m 3. Our main result is the characterization of the global flow of this problem.
TI - The global flow of the parabolic restricted three-body problem
ER -