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  2. Lambert's problem - Wikipedia

    en.wikipedia.org/wiki/Lambert's_problem

    being known functions of the parameter y the time for the true anomaly to increase with the amount is also a known function of y. If t 2 − t 1 {\displaystyle t_{2}-t_{1}} is in the range that can be obtained with an elliptic Kepler orbit corresponding y value can then be found using an iterative algorithm.

  3. Heliocentrism - Wikipedia

    en.wikipedia.org/wiki/Heliocentrism

    Heliocentrism [a] (also known as the heliocentric model) is a superseded astronomical model in which the Earth and planets orbit around the Sun at the center of the universe. Historically, heliocentrism was opposed to geocentrism , which placed the Earth at the center.

  4. Orbital elements - Wikipedia

    en.wikipedia.org/wiki/Orbital_elements

    The mean anomaly changes linearly with time, scaled by the mean motion, [2] =. where μ is the standard gravitational parameter. Hence if at any instant t 0 the orbital parameters are (e 0, a 0, i 0, Ω 0, ω 0, M 0), then the elements at time t = t 0 + δt is given by (e 0, a 0, i 0, Ω 0, ω 0, M 0 + n δt).

  5. Kepler orbit - Wikipedia

    en.wikipedia.org/wiki/Kepler_orbit

    An elliptic Kepler orbit with an eccentricity of 0.7, a parabolic Kepler orbit and a hyperbolic Kepler orbit with an eccentricity of 1.3. The distance to the focal point is a function of the polar angle relative to the horizontal line as given by the equation ()

  6. Kepler's laws of planetary motion - Wikipedia

    en.wikipedia.org/wiki/Kepler's_laws_of_planetary...

    These laws replaced circular orbits and epicycles in the heliocentric theory of Nicolaus Copernicus with elliptical orbits and explained how planetary velocities vary. The three laws state that: [1] [2] The orbit of a planet is an ellipse with the Sun at one of the two foci.

  7. Standard gravitational parameter - Wikipedia

    en.wikipedia.org/wiki/Standard_gravitational...

    The standard gravitational parameter μ of a celestial body is the product of the gravitational constant G and the mass M of that body. For two bodies, the parameter may be expressed as G ( m 1 + m 2 ) , or as GM when one body is much larger than the other: μ = G ( M + m ) ≈ G M . {\displaystyle \mu =G(M+m)\approx GM.}

  8. Copernican heliocentrism - Wikipedia

    en.wikipedia.org/wiki/Copernican_heliocentrism

    In the heliocentric model the planets' apparent retrograde motions' occurring at opposition to the Sun are a natural consequence of their heliocentric orbits. In the geocentric model, however, these are explained by the ad hoc use of epicycles , whose revolutions are mysteriously tied to that of the Sun. [ 54 ]

  9. 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 ...