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A radial hyperbolic trajectory is a non-periodic trajectory on a straight line where the relative speed of the two objects always exceeds the escape velocity. There are two cases: the bodies move away from each other or towards each other. This is a hyperbolic orbit with semi-minor axis = 0 and eccentricity = 1.
Hyperbolic equilibrium point p is a fixed point, or equilibrium point, of f, such that (Df) p has no eigenvalue with absolute value 1. In this case, Λ = {p}.More generally, a periodic orbit of f with period n is hyperbolic if and only if Df n at any point of the orbit has no eigenvalue with absolute value 1, and it is enough to check this condition at a single point of the orbit.
Such an orbit also has a velocity equal to the escape velocity and therefore will escape the gravitational pull of the planet. If the speed of a parabolic orbit is increased it will become a hyperbolic orbit. Escape orbit: A parabolic orbit where the object has escape velocity and is moving away from the planet.
For an elliptic orbit the specific orbital energy is the negative of the additional energy required to accelerate a mass of one kilogram to escape velocity (parabolic orbit). For a hyperbolic orbit , it is equal to the excess energy compared to that of a parabolic orbit.
Radial hyperbolic trajectory: a non-periodic orbit where the relative speed of the two objects always exceeds the escape velocity. There are two cases: the bodies move away from each other or towards each other. This is a hyperbolic orbit with semi-minor axis = 0 and eccentricity = 1. Although the eccentricity is 1 this is not a parabolic orbit.
Strogatz notes that "hyperbolic is an unfortunate name—it sounds like it should mean 'saddle point'—but it has become standard." [1] Several properties hold about a neighborhood of a hyperbolic point, notably [2] Orbits near a two-dimensional saddle point, an example of a hyperbolic equilibrium. A stable manifold and an unstable manifold exist,
A spacecraft that is leaving the central body on a hyperbolic trajectory has more than enough energy to escape: = | | > where = is the standard gravitational parameter, is the semi-major axis of the orbit's hyperbola (which may be negative in some convention).
There are many useful features of the effective potential, such as . To find the radius of a circular orbit, simply minimize the effective potential with respect to , or equivalently set the net force to zero and then solve for : = After solving for , plug this back into to find the maximum value of the effective potential .