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  2. Orbit equation - Wikipedia

    en.wikipedia.org/wiki/Orbit_equation

    In astrodynamics, an orbit equation defines the path of orbiting body around central body relative to , without specifying position as a function of time.Under standard assumptions, a body moving under the influence of a force, directed to a central body, with a magnitude inversely proportional to the square of the distance (such as gravity), has an orbit that is a conic section (i.e. circular ...

  3. Orbital mechanics - Wikipedia

    en.wikipedia.org/wiki/Orbital_mechanics

    Orbital mechanics is a core discipline within space-mission design and control. Celestial mechanics treats more broadly the orbital dynamics of systems under the influence of gravity, including both spacecraft and natural astronomical bodies such as star systems, planets, moons, and comets.

  4. Circular orbit - Wikipedia

    en.wikipedia.org/wiki/Circular_orbit

    The formula is dimensionless ... (7.5% of the orbital period in a circular orbit) The fact that the formulas ... the orbital velocity for a circular orbit with radius ...

  5. Orbital period - Wikipedia

    en.wikipedia.org/wiki/Orbital_period

    If the same sphere were made of lead the small body would need to orbit just 6.7 mm above the surface for sustaining the same orbital period. When a very small body is in a circular orbit barely above the surface of a sphere of any radius and mean density ρ (in kg/m 3), the above equation simplifies to (since M = Vρ = ⁠ 4 / 3 ⁠ π a 3 ρ)

  6. Clohessy–Wiltshire equations - Wikipedia

    en.wikipedia.org/wiki/Clohessy–Wiltshire_equations

    Early results about relative orbital motion were published by George William Hill in 1878. [3] Hill's paper discussed the orbital motion of the moon relative to the Earth.. In 1960, W. H. Clohessy and R. S. Wiltshire published the Clohessy–Wiltshire equations to describe relative orbital motion of a general satellite for the purpose of designing control systems to achieve orbital rendezvous.

  7. True anomaly - Wikipedia

    en.wikipedia.org/wiki/True_anomaly

    In celestial mechanics, true anomaly is an angular parameter that defines the position of a body moving along a Keplerian orbit.It is the angle between the direction of periapsis and the current position of the body, as seen from the main focus of the ellipse (the point around which the object orbits).

  8. Hill sphere - Wikipedia

    en.wikipedia.org/wiki/Hill_sphere

    The following table and logarithmic plot show the radius of the Hill spheres of some bodies of the Solar System calculated with the first formula stated above (including orbital eccentricity), using values obtained from the JPL DE405 ephemeris and from the NASA Solar System Exploration website. [15]

  9. Lambert's problem - Wikipedia

    en.wikipedia.org/wiki/Lambert's_problem

    Stated another way, Lambert's problem is the boundary value problem for the differential equation ¨ = ^ of the two-body problem when the mass of one body is infinitesimal; this subset of the two-body problem is known as the Kepler orbit.