About Solar system escape velocity
Escape velocity calculations are typically used to determine whether an object will remain in the gravitational sphere of influence of a given body. For example, in solar system exploration it is useful to know whether a probe will continue to orbit the Earth or escape to a heliocentric orbit.
In , escape velocity or escape speed is the minimum speed needed for an object to escape from contact with or orbit of a , assuming:• .
From the surface of a bodyAn alternative expression for the escape velocity $${\displaystyle v_{e}}$$ particularly useful at.
In this table, the left-hand half gives the escape velocity from the visible surface (which may be gaseous as with Jupiter for example), relative to the centre of the planet or moon (that.
•– an object with an escape velocity greater than the speed of light•(C3)•– speed needed to perform maneuvers.•– a technique for changing trajectory .
Escape speed at a distance d from the center of a spherically symmetric primary body (such as a star or a planet) with mass M is given by the formula$${\displaystyle v_{e}={\sqrt {\frac {2GM}{d}}}={\sqrt {2gd}}}$$where: .
If an object attains exactly escape velocity, but is not directed straight away from the planet, then it will follow a curved path or trajectory. Although this trajectory does not form a closed shape.
Let G be theand let M be the(or other gravitating body) and m be the mass of the escaping body or.
To put the distances in the table in context, 's average distance () is about 40 AU. Note: Data above as of June 24, 2024. Source: JPL,NASA SSD Simulator,and for New Horizons.Solar is a function of distance (r) from the Sun's center, given by
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