Tisserand's parameter

For a small body with semi-major axis a\,\!, orbital eccentricity e\,\!, and orbital inclination i\,\!, relative to the orbit of a perturbing larger body with semimajor axis a_P, the parameter is defined as follows: :T_P\ = \frac{a_P}{a} + 2\cos i\sqrt{\frac{a}{a_P} (1-e^2)} == Tisserand invariant conservation ==

In the three-body problem, the quasi-conservation of Tisserand's invariant is derived as the limit of the Jacobi integral away from the main two bodies (usually the star and planet). == Applications ==

The Tisserand parameter's conservation was originally used by Tisserand to determine whether or not an observed orbiting body is the same as one previously observed. This is usually known as the Tisserand's criterion. Orbit classification The value of the Tisserand parameter with respect to the planet that most perturbs a small body in the Solar System can be used to delineate groups of objects that may have similar origins. • TJ, Tisserand's parameter with respect to Jupiter as perturbing body, is frequently used to distinguish asteroids (typically T_J > 3) from Jupiter-family comets (typically 2). • The minor planet group of damocloids are defined by a Jupiter Tisserand's parameter of 2 or less (). == Related notions ==

The parameter is derived from one of the so-called Delaunay standard variables, used to study the perturbed Hamiltonian in a three-body system. Ignoring higher-order perturbation terms, the following value is conserved: : \sqrt{a (1-e^2)} \cos i Consequently, perturbations may lead to the resonance between the orbital inclination and eccentricity, known as Kozai resonance. Near-circular, highly inclined orbits can thus become very eccentric in exchange for lower inclination. For example, such a mechanism can produce sungrazing comets, because a large eccentricity with a constant semimajor axis results in a small perihelion. == See also ==