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Venus has an orbit with a semi-major axis of 0.723 au (108,200,000 km; 67,200,000 mi), and an eccentricity of 0.007. [1] [2] The low eccentricity and comparatively small size of its orbit give Venus the least range in distance between perihelion and aphelion of the planets: 1.46 million km.
A simplified plot of the position of Venus with respect to the Earth (i.e. geocentric perspective). For this graphic, Venus and the Earth are assumed to be in coplanar concentric perfect circular orbits around the sun (with Venus' orbit having a radius of 0.724 AU), and Venus' and Earth's orbital periods are assumed to be in an exact 8:13 ratio.
Description: A simplified plot of the position of Venus with respect to the Earth (i.e. geocentric perspective). For this graphic, Venus and the Earth are assumed to be in coplanar concentric perfect circular orbits around the sun, and Venus' and Earth's orbital periods are assumed to be in an exact 8:13 ratio (so that the size of Venus' orbit with respect to the Earth's is set as the cube ...
In a two-body problem with inverse-square-law force, every orbit is a Kepler orbit. The eccentricity of this Kepler orbit is a non-negative number that defines its shape. The eccentricity may take the following values: Circular orbit: e = 0; Elliptic orbit: 0 < e < 1; Parabolic trajectory: e = 1; Hyperbolic trajectory: e > 1; The eccentricity e ...
The following outline is provided as an overview of and topical guide to Venus: . Venus – second planet from the Sun, orbiting it every 224.7 Earth days. It has the longest rotation period (243 days) of any planet in the Solar System and rotates in the opposite direction to most other planets.
Hyperbolic orbit: An orbit with the eccentricity greater than 1. Such an orbit also has a velocity in excess of the escape velocity and as such, will escape the gravitational pull of the planet and continue to travel infinitely until it is acted upon by another body with sufficient gravitational force.
Simulations of the early solar system orbital dynamics have shown that the eccentricity of the Venus orbit may have been substantially larger in the past, reaching values as high as 0.31 and possibly impacting early climate evolution. [148] Venus and its rotation in respect to its revolution.
Orbital position vector, orbital velocity vector, other orbital elements. In astrodynamics and celestial dynamics, the orbital state vectors (sometimes state vectors) of an orbit are Cartesian vectors of position and velocity that together with their time () uniquely determine the trajectory of the orbiting body in space.