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The following are also concurrent: (1) the circle that is centered at the hyperbola's center and that passes through the hyperbola's vertices; (2) either directrix; and (3) either of the asymptotes. [22] Since both the transverse axis and the conjugate axis are axes of symmetry, the symmetry group of a hyperbola is the Klein four-group.
A hyperbolic trajectory is depicted in the bottom-right quadrant of this diagram, where the gravitational potential well of the central mass shows potential energy, and the kinetic energy of the hyperbolic trajectory is shown in red. The height of the kinetic energy decreases as the speed decreases and distance increases according to Kepler's laws.
The distance to the focal point is a function of the polar angle relative to the horizontal line as given by the equation In celestial mechanics , a Kepler orbit (or Keplerian orbit , named after the German astronomer Johannes Kepler ) is the motion of one body relative to another, as an ellipse , parabola , or hyperbola , which forms a two ...
The linear eccentricity of an ellipse or hyperbola, denoted c (or sometimes f or e), is the distance between its center and either of its two foci. The eccentricity can be defined as the ratio of the linear eccentricity to the semimajor axis a : that is, e = c a {\displaystyle e={\frac {c}{a}}} (lacking a center, the linear eccentricity for ...
r is the distance between the two bodies' centers of mass; a is the length of the semi-major axis (a > 0 for ellipses, a = ∞ or 1/a = 0 for parabolas, and a < 0 for hyperbolas) G is the gravitational constant; M is the mass of the central body; The product of GM can also be expressed as the standard gravitational parameter using the Greek ...
The semi-major axis of a hyperbola is, depending on the convention, plus or minus one half of the distance between the two branches; if this is a in the x-direction the equation is: [3] ( x − h ) 2 a 2 − ( y − k ) 2 b 2 = 1. {\displaystyle {\frac {\left(x-h\right)^{2}}{a^{2}}}-{\frac {\left(y-k\right)^{2}}{b^{2}}}=1.}
r p is the radius at periapsis (or "perifocus" etc.), the closest distance. The semi-major axis, a, is also the path-averaged distance to the centre of mass, [2]: 24–25 while the time-averaged distance is a(1 + e e / 2).
Adding equations (1) and results in an equation describing the center of mass motion. By contrast, subtracting equation (2) from equation (1) results in an equation that describes how the vector r = x 1 − x 2 between the masses changes with time.