Escape velocity

For other uses, see Escape velocity (disambiguation).

In physics, escape velocity is the minimum speed needed for an object to escape from the gravitational attraction of a massive body, without the aid of thrust, or suffering the resistance from friction. The escape velocity from Earth is about 11.186 km/s (40,270 km/h; 25,020 mph)^[1] at the surface. More generally, escape velocity is the speed at which the sum of an object's kinetic energy and its gravitational potential energy is equal to zero.^{[nb 1]} Given escape velocity perpendicular to a massive body, the object will move away from the body, slowing forever and approaching but never reaching zero speed. Once escape velocity is achieved, no further impulse need be applied for it to continue in its escape. In other words, if given escape velocity, the object will move away from the other body, continually slowing and will asymptotically approach zero speed as the object's distance approaches infinity, never to return.^[2]

For a spherically symmetric massive body such as a star or planet, the escape velocity for that body, at a given distance is calculated by the formula^[3]

v_e = \sqrt{\frac{2GM}{r}},

where G is the universal gravitational constant (G = 6.67×10⁻¹¹ m³ kg⁻¹ s⁻²), M the mass of the body to be escaped, and r the distance from the center of mass of the body to the object.^{[nb 2]} The relation is independent of the mass of the object escaping the mass body M. Conversely, a body that falls under the force of gravitational attraction of mass M from infinity, starting with zero velocity, will strike the mass with a velocity equal to its escape velocity.

When given a speed $V$ greater than the escape speed $v_{e},$ the object will asymptotically approach the hyperbolic excess speed $v_{\infty },$ satisfying the equation:^[4]

{v_{\infty }}^{2}=V^{2}-{v_{e}}^{2}.

In these equations atmospheric friction (air drag) is not taken into account. A rocket moving out of a gravity well does not actually need to attain escape velocity to escape, but could achieve the same result (escape) at any speed with a suitable mode of propulsion and sufficient propellant to provide the accelerating force on the object to escape. Escape velocity is only required to send a ballistic object on a trajectory that will allow the object to escape the gravity well of the mass M.

Overview

Luna 1, launched in 1959, was the first man-made object to attain escape velocity from Earth (see below table).^[5]

A barycentric velocity is a velocity of one body relative to the center of mass of a system of bodies. A relative velocity is the velocity of one body with respect to another. Relative escape velocity is defined only in systems with two bodies. For systems of two bodies the term "escape velocity" is ambiguous, but it is usually intended to mean the barycentric escape velocity of the less massive body. In gravitational fields "escape velocity" refers to the escape velocity of zero mass test particles relative to the barycenter of the masses generating the field.

The existence of escape velocity is a consequence of conservation of energy. For an object with a given total energy, which is moving subject to conservative forces (such as a static gravity field) it is only possible for the object to reach combinations of places and speeds which have that total energy; and places which have a higher potential energy than this cannot be reached at all.

For a given gravitational potential energy at a given position, the escape velocity is the minimum speed an object without propulsion needs to be able to "escape" from the gravity (i.e. so that gravity will never manage to pull it back). For the sake of simplicity, unless stated otherwise, we will assume that an object is attempting to escape from a uniform spherical planet by moving directly away from it (along a radial line away from the center of the planet) and that the only significant force acting on the moving object is the planet's gravity.

Escape velocity is actually a speed (not a velocity) because it does not specify a direction: no matter what the direction of travel is, the object can escape the gravitational field (provided its path does not intersect the planet). The simplest way of deriving the formula for escape velocity is to use conservation of energy. Imagine that a spaceship of mass m is at a distance r from the center of mass of the planet, whose mass is M. Its initial speed is equal to its escape velocity, $v_{e}$ . At its final state, it will be an infinite distance away from the planet, and its speed will be negligibly small and assumed to be 0. Kinetic energy K and gravitational potential energy U_g are the only types of energy that we will deal with, so by the conservation of energy,

(K + U_g)_i = (K + U_g)_f \,

K_ƒ = 0 because final velocity is zero, and U_gƒ = 0 because its final distance is infinity, so

\frac{1}{2}mv_e^2 + \frac{-GMm}{r} = 0 + 0

v_{e}={\sqrt {\frac {2GM}{r}}}

The same result is obtained by a relativistic calculation, in which case the variable r represents the radial coordinate or reduced circumference of the Schwarzschild metric.^[6]^[7]

Defined a little more formally, "escape velocity" is the initial speed required to go from an initial point in a gravitational potential field to infinity and end at infinity with a residual speed of zero, without any additional acceleration.^[8] All speeds and velocities measured with respect to the field. Additionally, the escape velocity at a point in space is equal to the speed that an object would have if it started at rest from an infinite distance and was pulled by gravity to that point. 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 km/s, which is approximately 33 times the speed of sound (Mach 33) and several times the muzzle velocity of a rifle bullet (up to 1.7 km/s). However, at 9,000 km altitude in "space", it is slightly less than 7.1 km/s.

The escape velocity relative to the surface of a rotating body depends on direction in which the escaping body travels. For example, as the Earth's rotational velocity is 465 m/s at the equator, a rocket launched tangentially from the Earth's equator to the east requires an initial velocity of about 10.735 km/s relative to Earth to escape whereas a rocket launched tangentially from the Earth's equator to the west requires an initial velocity of about 11.665 km/s relative to Earth. The surface velocity decreases with the cosine of the geographic latitude, so space launch facilities are often located as close to the equator as feasible, e.g. the American Cape Canaveral (latitude 28°28' N) and the French Guiana Space Centre (latitude 5°14' N).

The barycentric escape velocity is independent of the mass of the escaping object. It does not matter if the mass is 1 kg or 1,000 kg, what differs is the amount of energy required. For an object of mass $m$ the energy required to escape the Earth's gravitational field is GMm / r, a function of the object's mass (where r is the radius of the Earth, G is the gravitational constant, and M is the mass of the Earth, M=5.9736×10²⁴ kg).

For a mass equal to a Saturn V rocket, the escape velocity relative to the launch pad is 253.5 am/s (8 nanometers per year) faster than the escape velocity relative to the mutual center of mass. When the mass reaches the Andromeda Galaxy, Earth will have recoiled 500 m away from the mutual center of mass.

Ignoring all factors other than the gravitational force between the body and the object, an object projected vertically at speed $v$ from the surface of a spherical body with escape velocity $v_{e}$ and radius $R$ will attain a maximum height $h$ satisfying the equation^[9]

v=v_{e}{\sqrt {\frac {h}{R+h}}}\ ,

which, solving for h results in

h={\frac {x^{2}}{1-x^{2}}}\ R\ ,

where $x={\frac {v}{v_{e}}}$ is the ratio of the original speed $v$ to the escape velocity $v_{e}.$

Orbit

If an object attains escape velocity, but is not directed straight away from the planet, then it will follow a curved path. Although this path does not form a closed shape, it is still considered an orbit. Assuming that gravity is the only significant force in the system, this object's speed at any point in the orbit will be equal to the escape velocity at that point (due to the conservation of energy, its total energy must always be 0, which implies that it always has escape velocity; see the derivation above). The shape of the orbit will be a parabola whose focus is located at the center of mass of the planet. An actual escape requires a course with an orbit that does not intersect with the planet, or its atmosphere, since this would cause the object to crash. When moving away from the source, this path is called an escape orbit. Escape orbits are known as C3 = 0 orbits. C3 is the characteristic energy, = −GM/a, where a is the semi-major axis, which is infinite for parabolic orbits.

When there are many gravitating bodies, such as in the solar system, a rocket that travels at escape velocity from one body, say Earth, will not travel to an infinite distance because it needs an even higher speed to escape the Sun's gravity. Near the Earth, the rocket's orbit will appear parabolic, but will become an ellipse around the Sun, except when it is perturbed by the Earth, whose orbit it must still intersect, and other bodies.

List of escape velocities

Location	with respect to	V_e (km/s)^[10]	Location	with respect to	V_e (km/s)^[10]
on the Sun	the Sun's gravity	617.5
on Mercury	Mercury's gravity	4.3^[11]^:230	at Mercury	the Sun's gravity	67.7
on Venus	Venus's gravity	10.3	at Venus	the Sun's gravity	49.5
on Earth	Earth's gravity	11.2^[11]^:200	at the Earth/Moon	the Sun's gravity	42.1
on the Moon	the Moon's gravity	2.4	at the Moon	the Earth's gravity	1.4
on Mars	Mars' gravity	5.0^[11]^:234	at Mars	the Sun's gravity	34.1
on Ceres	Ceres's gravity	0.51
on Jupiter	Jupiter's gravity	59.6^[11]^:236	at Jupiter	the Sun's gravity	18.5
on Io	Io's gravity	2.558
on Europa	Europa's gravity	2.025
on Ganymede	Ganymede's gravity	2.741
on Callisto	Callisto's gravity	2.440
on Saturn	Saturn's gravity	35.6^[11]^:238	at Saturn	the Sun's gravity	13.6
on Titan	Titan's gravity	2.639
on Uranus	Uranus' gravity	21.3^[11]^:240	at Uranus	the Sun's gravity	9.6
on Neptune	Neptune's gravity	23.8^[11]^:240	at Neptune	the Sun's gravity	7.7
on Triton	Triton's gravity	1.455
on Pluto	Pluto's gravity	1.2
at Solar System galactic radius	the Milky Way's gravity	492–594^[12]^[13]
on the event horizon	a black hole's gravity	299,792 (speed of light)

Because of 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 (40,320 km/h), as these speeds are too far in the hypersonic regime for most practical propulsion systems and would cause most objects to burn up due to aerodynamic heating or be torn apart by atmospheric drag. For an actual escape orbit a spacecraft is first placed in low Earth orbit (160–2,000 km) and then accelerated to the escape velocity at that altitude, which is a little less — about 10.9 km/s. The required change in speed, however, is far less because from a low Earth orbit the spacecraft already has a speed of approximately 8 km/s (28,800 km/h).

Calculating an escape velocity

To expand upon the derivation given in the Overview section,

v_e = \sqrt{\frac{2GM}{r}} = \sqrt{\frac{2\mu}{r}} = \sqrt{2gr\,}

where $v_{e}$ is the barycentric escape velocity, G is the gravitational constant, M is the mass of the body being escaped from, r is the distance between the center of the body and the point at which escape velocity is being calculated, g is the gravitational acceleration at that distance, and μ is the standard gravitational parameter.^[14]

The escape velocity at a given height is ${\sqrt {2}}$ times the speed in a circular orbit at the same height, (compare this with the velocity equation in circular orbit). 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. The velocity corresponding to the circular orbit is sometimes called the first cosmic velocity, whereas in this context the escape velocity is referred to as the second cosmic velocity.^[15]

For a body with a spherically-symmetric distribution of mass, the barycentric escape velocity $v_{e}$ from the surface (in m/s) is approximately 2.364×10⁻⁵ m^1.5kg^−0.5s⁻¹ times the radius r (in meters) times the square root of the average density ρ (in kg/m³), or:

v_e \approx 2.364 \times 10^{-5} r \sqrt \rho.\,

Deriving escape velocity using calculus

Let G be the gravitational constant and let M be the mass of the earth (or other gravitating body) and m be the mass of the escaping body or projectile. At a distance r from the centre of gravitation the body feels an attractive force^[16]

F = G\frac{Mm}{r^2}.

The work needed to move the body over a small distance dr against this force is therefore given by

dW = Fdr=-G\frac{Mm}{r^2}\,dr,

where the minus sign indicates the force acts in the opposite sense of $dr$ .

The total work needed to move the body from the surface r₀ of the gravitating body to infinity is then

W = \int_{r_0}^{\infty} -G\frac{Mm}{r^2}\,dr = -G\frac{Mm}{r_0} = -mgr_0.

This is the minimal required kinetic energy to be able to reach infinity, so the escape velocity v₀ satisfies

W+K = 0 \leftrightarrow \tfrac{1}{2}m v_0^2 = G\frac{Mm}{r_0},

which results in

v_0 = \sqrt\frac{2GM}{r_0} = \sqrt{2gr_0}.

Notes

↑ The gravitational potential energy is negative since gravity is an attractive force and the potential energy has been defined for this purpose to be zero at infinite distance from the centre of gravity.
↑ The value GM is called the standard gravitational parameter, or μ, and is often known more accurately than either G or M separately.

References

Roger R. Bate; Donald D. Mueller; Jerry E. White (1971). Fundamentals of astrodynamics. New York: Dover Publications. ISBN 0-486-60061-0.

↑ Lai, Shu T. (2011). Fundamentals of Spacecraft Charging: Spacecraft Interactions with Space Plasmas. Princeton University Press. p. 240. ISBN 978-1-4008-3909-4. Extract of page 240
↑ Giancoli, Douglas C. (2008). Physics for Scientists and Engineers with Modern Physics. Addison-Wesley. p. 199. ISBN 978-0131495081.
↑ Khatri, Poudel, Gautam, M.K. , P.R. , A.K. (2010). Principles of Physics. Kathmandu: Ayam Publication. pp. 170, 171. ISBN 9789937903844.
↑ Bate, Roger R.; Mueller, Donald D.; White, Jerry E. (1971). Fundamentals of Astrodynamics (illustrated ed.). Courier Corporation. p. 39. ISBN 978-0-486-60061-1. Extract of page 39
↑ NASA – NSSDC – Spacecraft – Details
↑ Taylor, Edwin F.; Wheeler, John Archibald; Bertschinger, Edmund (2010). Exploring Black Holes: Introduction to General Relativity (2nd revised ed.). Addison-Wesley. pp. 2–22. ISBN 978-0-321-51286-4. Sample chapter, page 2-22
↑ Choquet-Bruhat, Yvonne (2015). Introduction to General Relativity, Black Holes, and Cosmology (illustrated ed.). Oxford University Press. pp. 116–117. ISBN 978-0-19-966646-1. Extract of page 116, 117
↑ "escape velocity | physics". Retrieved 2015-08-21.
↑ Bajaj, N. K. (2015). Complete Physics: JEE Main. McGraw-Hill Education. p. 6.12. ISBN 978-93-392-2032-7. Example 21, page 6.12
1 2 "Solar System Data". Georgia State University. Retrieved 2007-01-21.
1 2 3 4 5 6 7 Wimmer, Mark R. Chartrand ; illustrated by Helmut K. (2001). Night sky : a field guide to the heavens. New York: St. Martin's Press. ISBN 9781582381268.
↑ Smith, Martin C.; Ruchti, G. R.; Helmi, A.; Wyse, R. F. G. (2007). "The RAVE Survey: Constraining the Local Galactic Escape Speed". Proceedings of the International Astronomical Union. 2 (S235): 137. doi:10.1017/S1743921306005692.
↑ Kafle, P.R.; Sharma, S.; Lewis, G.F.; Bland-Hawthorn, J. (2014). "On the Shoulders of Giants: Properties of the Stellar Halo and the Milky Way Mass Distribution". The Astrophysical Journal. 794 (1): 17. arXiv:1408.1787. Bibcode:2014ApJ...794...59K. doi:10.1088/0004-637X/794/1/59.
↑ Bate, Mueller and White, p. 35
↑ Teodorescu, P. P. (2007). Mechanical systems, classical models. Springer, Japan. p. 580. ISBN 1-4020-5441-6. , Section 2.2.2, p. 580
↑ Muncaster, Roger (1993). A-level Physics. Nelson Thornes. p. 103. ISBN 0-7487-1584-3. Extract of page 103

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