Escape velocity Guide, Meaning , Facts, Information and Description
- For the video game title, see Escape Velocity (computer game).
One somewhat counterintuitive feature of escape velocity is that it is independent of direction, so that "velocity" is a misnomer; it is a scalar quantity and would more accurately be called "escape speed". The simplest way of deriving the formula for escape velocity is to use conservation of energy, thus: in order to escape, an object must have at least as much kinetic energy as the increase of potential energy required to move to infinite height.
Defined a bit more formally, "escape velocity" is the initial speed required to go from an initial point in a gravitational potential field to infinity with a residual velocity of zero, relative to the field. Conversely, an object starting at rest and at infinity, dropping towards the attracting mass, would reach its surface moving at the escape velocity. In common usage, the initial point is on the surface of a planet or moon. On the surface of the Earth the escape velocity is about 11.2 kilometres per second. However, at 9000 km altitude in "space", it is slightly less than 7.1 km/s.
For a body rotating about its axis the escape velocity with respect to the surface does depend on direction. E.g., for the Earth the rotational velocity is 465 m/s to the east at the equator, and the escape velocity to the east, with respect to the Earth's surface, is ca. 10.7 km/s.
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2 Calculating an escape velocity 3 Mathematical derivation 4 Multiple sources 5 Orbit 6 See also 7 External link |
Due to the atmosphere it is not useful and hardly possible to give an object near the surface of the Earth a speed of 11.2 km/s, as these speeds are too far in the hypersonic regime for most practical propulsion systems. For an actual escape orbit a spacecraft is first placed in low Earth orbit and then accelerated to the escape velocity at that altitude, which is a little less, ca. 10.9 km/s.
In the simple case of the escape velocity from a single body, it can be calculated as follows:
The escape velocity at a given height is √2 times the speed in a circular orbit at the same height, compare (14) in circular motion. This corresponds to the fact that the potential energy with respect to infinity of an object in such an orbit is minus two times its kinetic energy, while to escape the sum of potential and kinetic energy needs to be at least zero.
For a body with a spherically-symmetric distribution of mass, the escape velocity from the surface (in m/s) is approximately 2.364×10−5 m1.5kg-0.5s-1 times the radius (in metres) times the square root of the average density (in kg/m3), or:
List of escape velocities
Location
with respect to
Ve
on the Sun,
the Sun's gravity:
617.5 km/s
on Mercury,
Mercury's gravity:
4.4 km/s
at Mercury,
the Sun's gravity:
67.7 km/s
on Venus,
Venus' gravity:
10.4 km/s
at Venus,
the Sun's gravity:
49.5 km/s
at the Earth,
the Earth's gravity:
11.2 km/s
on the Moon,
the Moon's gravity:
2.4 km/s
at the Moon,
the Earth's gravity:
1.4 km/s
at the Earth/Moon,
the Sun's gravity:
42.1 km/s
on Mars,
Mars' gravity:
5.0 km/s
at Mars,
the Sun's gravity:
34.1 km/s
on Jupiter,
Jupiter's gravity:
59.5 km/s
at Jupiter,
the Sun's gravity:
18.5 km/s
on Saturn,
Saturn's gravity:
35.5 km/s
at Saturn,
the Sun's gravity:
13.6 km/s
on Uranus,
Uranus' gravity:
21.3 km/s
at Uranus,
the Sun's gravity:
9.6 km/s
on Neptune,
Neptune's gravity:
23.5 km/s
at Neptune,
the Sun's gravity:
7.7 km/s
on Pluto,
Pluto's gravity:
1.3 km/s
at Pluto,
the Sun's gravity:
6.7 km/s
at the solar system,
the Milky Way's gravity:
~1000 km/s
Calculating an escape velocity
where is the escape velocity, G is the gravitational constant, M is the mass of the body being escaped from, m is the mass of the escaping body (factors out), and r is the distance between the centre of the body and the point at which escape velocity is being calculated, and μ is the standard gravitational parameter
.Mathematical derivation
The Earth's escape speed can be derived with nothing more than first-year physics and first-year calculus as developed by Isaac Newton in the 17th century. It is not necessary to know the gravitational constant G or the mass M of the Earth. Let
- r = the Earth's radius, and
- g = the acceleration of gravity at the Earth's surface.
The escape velocity from a position in a field with multiple sources is derived from the total potential energy per kg at that position, relative to infinity. The potential energies for all sources can simply be added. For the escape velocity this results in the square root of the sum of the squares of the escape velocities of all sources separately.
For example, at the Earth's surface the escape velocity for the combination Earth and Sun is (11.2² + 42.1²) = 43.6 km/s. As a result, to leave the solar system requires a speed of 13.6 km/s relative to Earth in the direction of the Earth's orbital motion, since the speed is then added to the speed of 30 km/s of that motion.
If a freefalling body at any position has the escape velocity for that position, this is the case for the whole orbit. If the gravity source is a spherically symmetric body the orbit is (part of) a parabola with the center of the source as focus (parabolic trajectory), or part of a straight line through the source. When moving away from the source it is called an escape orbit, otherwise a capture orbit. Both are also known as C3 = 0 orbit.
If the body has the escape velocity with respect to the Earth, this is not enough to escape the Solar System, so near the Earth the orbit resembles a parabola, but further away it bends into an elliptical orbit around the Sun.
This is an Article on Escape velocity. Page Contains Information, Facts Details or Explanation Guide About Escape velocity Multiple sources
Orbit
See also
External link