Acceleration | |
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Common symbols | a |

SI unit | m/s^{2}, m·s^{−2}, m s^{−2} |

Derivations from other quantities | |

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Classical mechanics |
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In mechanics, **acceleration** is the rate of change of the velocity of an object with respect to time. Accelerations are vector quantities (in that they have magnitude and direction).^{ [1] }^{ [2] } The orientation of an object's acceleration is given by the orientation of the *net* force acting on that object. The magnitude of an object's acceleration, as described by Newton's Second Law,^{ [3] } is the combined effect of two causes:

- Definition and properties
- Average acceleration
- Instantaneous acceleration
- Units
- Other forms
- Tangential and centripetal acceleration
- Special cases
- Uniform acceleration
- Circular motion
- Relation to relativity
- Special relativity
- General relativity
- Conversions
- See also
- References
- External links

- the net balance of all external forces acting onto that object — magnitude is directly proportional to this net resulting force;
- that object's mass, depending on the materials out of which it is made — magnitude is inversely proportional to the object's mass.

The SI unit for acceleration is metre per second squared (m⋅s^{−2}, ).

For example, when a vehicle starts from a standstill (zero velocity, in an inertial frame of reference) and travels in a straight line at increasing speeds, it is accelerating in the direction of travel. If the vehicle turns, an acceleration occurs toward the new direction and changes its motion vector. The acceleration of the vehicle in its current direction of motion is called a linear (or tangential during circular motions) acceleration, the reaction to which the passengers on board experience as a force pushing them back into their seats. When changing direction, the effecting acceleration is called radial (or centripetal during circular motions) acceleration, the reaction to which the passengers experience as a centrifugal force. If the speed of the vehicle decreases, this is an acceleration in the opposite direction and mathematically a negative, sometimes called **deceleration or retardation**, and passengers experience the reaction to deceleration as an inertial force pushing them forward. Such negative accelerations are often achieved by retrorocket burning in spacecraft.^{ [4] } Both acceleration and deceleration are treated the same, as they are both changes in velocity. Each of these accelerations (tangential, radial, deceleration) is felt by passengers until their relative (differential) velocity are neutralized in reference to the acceleration due to change in speed.

An object's average acceleration over a period of time is its change in velocity, , divided by the duration of the period, . Mathematically,

Instantaneous acceleration, meanwhile, is the limit of the average acceleration over an infinitesimal interval of time. In the terms of calculus, instantaneous acceleration is the derivative of the velocity vector with respect to time:

As acceleration is defined as the derivative of velocity, **v**, with respect to time t and velocity is defined as the derivative of position, **x**, with respect to time, acceleration can be thought of as the second derivative of **x** with respect to t:

(Here and elsewhere, if motion is in a straight line, vector quantities can be substituted by scalars in the equations.)

By the fundamental theorem of calculus, it can be seen that the integral of the acceleration function *a*(*t*) is the velocity function *v*(*t*); that is, the area under the curve of an acceleration vs. time (a vs. t) graph corresponds to the change of velocity.

Likewise, the integral of the jerk function *j*(*t*), the derivative of the acceleration function, can be used to find the change of acceleration at a certain time:

Acceleration has the dimensions of velocity (L/T) divided by time, i.e. L T ^{−2}. The SI unit of acceleration is the metre per second squared (m s^{−2}); or "metre per second per second", as the velocity in metres per second changes by the acceleration value, every second.

An object moving in a circular motion—such as a satellite orbiting the Earth—is accelerating due to the change of direction of motion, although its speed may be constant. In this case it is said to be undergoing *centripetal* (directed towards the center) acceleration.

Proper acceleration, the acceleration of a body relative to a free-fall condition, is measured by an instrument called an accelerometer.

In classical mechanics, for a body with constant mass, the (vector) acceleration of the body's center of mass is proportional to the net force vector (i.e. sum of all forces) acting on it (Newton’s second law):

where **F** is the net force acting on the body, m is the mass of the body, and **a** is the center-of-mass acceleration. As speeds approach the speed of light, relativistic effects become increasingly large.

The velocity of a particle moving on a curved path as a function of time can be written as:

with *v*(*t*) equal to the speed of travel along the path, and

a unit vector tangent to the path pointing in the direction of motion at the chosen moment in time. Taking into account both the changing speed *v*(*t*) and the changing direction of **u**_{t}, the acceleration of a particle moving on a curved path can be written using the chain rule of differentiation^{ [5] } for the product of two functions of time as:

where **u**_{n} is the unit (inward) normal vector to the particle's trajectory (also called *the principal normal*), and **r** is its instantaneous radius of curvature based upon the osculating circle at time t. These components are called the tangential acceleration and the normal or radial acceleration (or centripetal acceleration in circular motion, see also circular motion and centripetal force).

Geometrical analysis of three-dimensional space curves, which explains tangent, (principal) normal and binormal, is described by the Frenet–Serret formulas.^{ [6] }^{ [7] }

*Uniform* or *constant* acceleration is a type of motion in which the velocity of an object changes by an equal amount in every equal time period.

A frequently cited example of uniform acceleration is that of an object in free fall in a uniform gravitational field. The acceleration of a falling body in the absence of resistances to motion is dependent only on the gravitational field strength g (also called *acceleration due to gravity*). By Newton's Second Law the force acting on a body is given by:

Because of the simple analytic properties of the case of constant acceleration, there are simple formulas relating the displacement, initial and time-dependent velocities, and acceleration to the time elapsed:^{ [8] }

where

- is the elapsed time,
- is the initial displacement from the origin,
- is the displacement from the origin at time ,
- is the initial velocity,
- is the velocity at time , and
- is the uniform rate of acceleration.

In particular, the motion can be resolved into two orthogonal parts, one of constant velocity and the other according to the above equations. As Galileo showed, the net result is parabolic motion, which describes, e. g., the trajectory of a projectile in a vacuum near the surface of Earth.^{ [9] }

In uniform circular motion, that is moving with constant *speed* along a circular path, a particle experiences an acceleration resulting from the change of the direction of the velocity vector, while its magnitude remains constant. The derivative of the location of a point on a curve with respect to time, i.e. its velocity, turns out to be always exactly tangential to the curve, respectively orthogonal to the radius in this point. Since in uniform motion the velocity in the tangential direction does not change, the acceleration must be in radial direction, pointing to the center of the circle. This acceleration constantly changes the direction of the velocity to be tangent in the neighboring point, thereby rotating the velocity vector along the circle.

- For a given speed , the magnitude of this geometrically caused acceleration (centripetal acceleration) is inversely proportional to the radius of the circle, and increases as the square of this speed:
- Note that, for a given angular velocity , the centripetal acceleration is directly proportional to radius . This is due to the dependence of velocity on the radius .

Expressing centripetal acceleration vector in polar components, where is a vector from the centre of the circle to the particle with magnitude equal to this distance, and considering the orientation of the acceleration towards the center, yields

As usual in rotations, the speed of a particle may be expressed as an *angular speed* with respect to a point at the distance as

Thus

This acceleration and the mass of the particle determine the necessary centripetal force, directed *toward* the centre of the circle, as the net force acting on this particle to keep it in this uniform circular motion. The so-called 'centrifugal force', appearing to act outward on the body, is a so-called pseudo force experienced in the frame of reference of the body in circular motion, due to the body's linear momentum, a vector tangent to the circle of motion.

In a nonuniform circular motion, i.e., the speed along the curved path is changing, the acceleration has a non-zero component tangential to the curve, and is not confined to the principal normal, which directs to the center of the osculating circle, that determines the radius for the centripetal acceleration. The tangential component is given by the angular acceleration , i.e., the rate of change of the angular speed times the radius . That is,

The sign of the tangential component of the acceleration is determined by the sign of the angular acceleration (), and the tangent is always directed at right angles to the radius vector.

The special theory of relativity describes the behavior of objects traveling relative to other objects at speeds approaching that of light in a vacuum. Newtonian mechanics is exactly revealed to be an approximation to reality, valid to great accuracy at lower speeds. As the relevant speeds increase toward the speed of light, acceleration no longer follows classical equations.

As speeds approach that of light, the acceleration produced by a given force decreases, becoming infinitesimally small as light speed is approached; an object with mass can approach this speed asymptotically, but never reach it.

Unless the state of motion of an object is known, it is impossible to distinguish whether an observed force is due to gravity or to acceleration—gravity and inertial acceleration have identical effects. Albert Einstein called this the equivalence principle, and said that only observers who feel no force at all—including the force of gravity—are justified in concluding that they are not accelerating.^{ [10] }

Base value | (Gal, or cm/s^{2}) | (ft/s^{2}) | (m/s^{2}) | (Standard gravity, g_{0}) |
---|---|---|---|---|

1 Gal, or cm/s^{2} | 1 | 0.0328084 | 0.01 | 1.01972×10^{−3} |

1 ft/s^{2} | 30.4800 | 1 | 0.304800 | 0.0310810 |

1 m/s^{2} | 100 | 3.28084 | 1 | 0.101972 |

1 g_{0} | 980.665 | 32.1740 | 9.80665 | 1 |

- Acceleration (differential geometry)
- Four-vector: making the connection between space and time explicit
- Gravitational acceleration
- Inertia
- Orders of magnitude (acceleration)
- Shock (mechanics)
- Shock and vibration data logger

measuring 3-axis acceleration - Space travel using constant acceleration
- Specific force

A **centripetal force** is a force that makes a body follow a curved path. Its direction is always orthogonal to the motion of the body and towards the fixed point of the instantaneous center of curvature of the path. Isaac Newton described it as "a force by which bodies are drawn or impelled, or in any way tend, towards a point as to a centre". In Newtonian mechanics, gravity provides the centripetal force causing astronomical orbits.

In physics, **jerk** or **jolt** is the rate at which an object's acceleration changes with respect to time. It is a vector quantity. Jerk is most commonly denoted by the symbol j and expressed in m/s^{3} or standard gravities per second (*g*_{0}/s).

In celestial mechanics, an **orbit** is the curved trajectory of an object such as the trajectory of a planet around a star, or of a natural satellite around a planet, or of an artificial satellite around an object or position in space such as a planet, moon, asteroid, or Lagrange point. Normally, orbit refers to a regularly repeating trajectory, although it may also refer to a non-repeating trajectory. To a close approximation, planets and satellites follow elliptic orbits, with the center of mass being orbited at a focal point of the ellipse, as described by Kepler's laws of planetary motion.

In physics, **equations of motion** are equations that describe the behavior of a physical system in terms of its motion as a function of time. More specifically, the equations of motion describe the behavior of a physical system as a set of mathematical functions in terms of dynamic variables. These variables are usually spatial coordinates and time, but may include momentum components. The most general choice are generalized coordinates which can be any convenient variables characteristic of the physical system. The functions are defined in a Euclidean space in classical mechanics, but are replaced by curved spaces in relativity. If the dynamics of a system is known, the equations are the solutions for the differential equations describing the motion of the dynamics.

**Kinematics** is a subfield of physics, developed in classical mechanics, that describes the motion of points, bodies (objects), and systems of bodies without considering the forces that cause them to move. Kinematics, as a field of study, is often referred to as the "geometry of motion" and is occasionally seen as a branch of mathematics. A kinematics problem begins by describing the geometry of the system and declaring the initial conditions of any known values of position, velocity and/or acceleration of points within the system. Then, using arguments from geometry, the position, velocity and acceleration of any unknown parts of the system can be determined. The study of how forces act on bodies falls within kinetics, not kinematics. For further details, see analytical dynamics.

In physics, **angular acceleration** refers to the time rate of change of angular velocity. As there are two types of angular velocity, namely spin angular velocity and orbital angular velocity, there are naturally also two types of angular acceleration, called spin angular acceleration and orbital angular acceleration respectively. Spin angular acceleration refers to the angular acceleration of a rigid body about its centre of rotation, and orbital angular acceleration refers to the angular acceleration of a point particle about a fixed origin.

In physics, **work** is the energy transferred to or from an object via the application of force along a displacement. In its simplest form, it is often represented as the product of force and displacement. A force is said to do positive work if it has a component in the direction of the displacement of the point of application. A force does negative work if it has a component opposite to the direction of the displacement at the point of application of the force.

In the physical science of dynamics, **rigid-body dynamics** studies the movement of systems of interconnected bodies under the action of external forces. The assumption that the bodies are *rigid* simplifies analysis, by reducing the parameters that describe the configuration of the system to the translation and rotation of reference frames attached to each body. This excludes bodies that display fluid, highly elastic, and plastic behavior.

In physics, **circular motion** is a movement of an object along the circumference of a circle or rotation along a circular path. It can be uniform, with constant angular rate of rotation and constant speed, or non-uniform with a changing rate of rotation. The rotation around a fixed axis of a three-dimensional body involves circular motion of its parts. The equations of motion describe the movement of the center of mass of a body. In circular motion, the distance between the body and a fixed point on the surface remains the same.

In geometry and mechanics, a **displacement** is a vector whose length is the shortest distance from the initial to the final position of a point P undergoing motion. It quantifies both the distance and direction of the net or total motion along a straight line from the initial position to the final position of the point trajectory. A displacement may be identified with the translation that maps the initial position to the final position.

A **fictitious force** is a force that appears to act on a mass whose motion is described using a non-inertial frame of reference, such as an accelerating or rotating reference frame. An example is seen in a passenger vehicle that is accelerating in the forward direction – passengers perceive that they are acted upon by a force in the backward direction pushing them back into their seats. An example in a rotating reference frame is the force that appears to push objects outwards towards the rim of a centrifuge. These apparent forces are examples of fictitious forces.

**Spacecraft flight dynamics** is the application of mechanical dynamics to model how the external forces acting on a space vehicle or spacecraft determine its flight path. These forces are primarily of three types: propulsive force provided by the vehicle's engines; gravitational force exerted by the Earth and other celestial bodies; and aerodynamic lift and drag.

In a compressible sound transmission medium - mainly air - air particles get an accelerated motion: the **particle acceleration** or sound acceleration with the symbol a in metre/second^{2}. In acoustics or physics, **acceleration** is defined as the rate of change of velocity. It is thus a vector quantity with dimension length/time^{2}. In SI units, this is m/s^{2}.

A **time derivative** is a derivative of a function with respect to time, usually interpreted as the rate of change of the value of the function. The variable denoting time is usually written as .

In physics, the **Thomas precession**, named after Llewellyn Thomas, is a relativistic correction that applies to the spin of an elementary particle or the rotation of a macroscopic gyroscope and relates the angular velocity of the spin of a particle following a curvilinear orbit to the angular velocity of the orbital motion.

**Rotation around a fixed axis** is a special case of rotational motion. The fixed-axis hypothesis excludes the possibility of an axis changing its orientation and cannot describe such phenomena as wobbling or precession. According to Euler's rotation theorem, simultaneous rotation along a number of stationary axes at the same time is impossible; if two rotations are forced at the same time, a new axis of rotation will appear.

**Linear motion**, also called **rectilinear motion**, is one-dimensional motion along a straight line, and can therefore be described mathematically using only one spatial dimension. The linear motion can be of two types: uniform linear motion with constant velocity or zero acceleration; and non-uniform linear motion with variable velocity or non-zero acceleration. The motion of a particle along a line can be described by its position , which varies with (time). An example of linear motion is an athlete running 100m along a straight track.

**Velocity** is the directional speed of a object in motion as an indication of its rate of change in position as observed from a particular frame of reference and as measured by a particular standard of time. Velocity is a fundamental concept in kinematics, the branch of classical mechanics that describes the motion of bodies.

In classical mechanics, the **central-force problem** is to determine the motion of a particle in a single central potential field. A central force is a force that points from the particle directly towards a fixed point in space, the center, and whose magnitude only depends on the distance of the object to the center. In many important cases, the problem can be solved analytically, i.e., in terms of well-studied functions such as trigonometric functions.

- ↑ Bondi, Hermann (1980).
*Relativity and Common Sense*. Courier Dover Publications. pp. 3. ISBN 978-0-486-24021-3. - ↑ Lehrman, Robert L. (1998).
*Physics the Easy Way*. Barron's Educational Series. pp. 27. ISBN 978-0-7641-0236-3. - ↑ Crew, Henry (2008).
*The Principles of Mechanics*. BiblioBazaar, LLC. p. 43. ISBN 978-0-559-36871-4. - ↑ Raymond A. Serway; Chris Vuille; Jerry S. Faughn (2008).
*College Physics, Volume 10*. Cengage. p. 32. ISBN 9780495386933. - ↑ Weisstein, Eric W. "Chain Rule".
*Wolfram MathWorld*. Wolfram Research. Retrieved 2 August 2016. - ↑ Larry C. Andrews; Ronald L. Phillips (2003).
*Mathematical Techniques for Engineers and Scientists*. SPIE Press. p. 164. ISBN 978-0-8194-4506-3. - ↑ Ch V Ramana Murthy; NC Srinivas (2001).
*Applied Mathematics*. New Delhi: S. Chand & Co. p. 337. ISBN 978-81-219-2082-7. - ↑ Keith Johnson (2001).
*Physics for you: revised national curriculum edition for GCSE*(4th ed.). Nelson Thornes. p. 135. ISBN 978-0-7487-6236-1. - ↑ David C. Cassidy; Gerald James Holton; F. James Rutherford (2002).
*Understanding physics*. Birkhäuser. p. 146. ISBN 978-0-387-98756-9. - ↑ Brian Greene,
*The Fabric of the Cosmos: Space, Time, and the Texture of Reality*, page 67. Vintage ISBN 0-375-72720-5

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