In physics, angular momentum (rarely, moment of momentum or rotational momentum) is the rotational equivalent of linear momentum. It is an important quantity in physics because it is a conserved quantity—the total angular momentum of a closed system remains constant.
In three dimensions, the angular momentum for a point particle is a pseudovector , the cross product of the particle's position vector r (relative to some origin) and its momentum vector; the latter is in Newtonian mechanics. This definition can be applied to each point in continua like solids or fluids, or physical fields. Unlike momentum, angular momentum does depend on where the origin is chosen, since the particle's position is measured from it.
Just like for angular velocity, there are two special types of angular momentum: the spin angular momentum and orbital angular momentum. The spin angular momentum of an object is defined as the angular momentum about its centre of mass coordinate. The orbital angular momentum of an object about a chosen origin is defined as the angular momentum of the centre of mass about the origin. The total angular momentum of an object is the sum of the spin and orbital angular momenta. The orbital angular momentum vector of a point particle is always parallel and directly proportional to the orbital angular velocity vector ω of the particle, where the constant of proportionality depends on both the mass of the particle and its distance from origin. The spin angular momentum vector of a rigid body is proportional but not always parallel to the spin angular velocity vector Ω, making the constant of proportionality a second-rank tensor rather than a scalar.
Angular momentum is an extensive quantity; i.e. the total angular momentum of any composite system is the sum of the angular momenta of its constituent parts. For a continuous rigid body, the total angular momentum is the volume integral of angular momentum density (i.e. angular momentum per unit volume in the limit as volume shrinks to zero) over the entire body.
Torque can be defined as the rate of change of angular momentum, analogous to force. The net ''external'' torque on any system is always equal to the ''total'' torque on the system; in other words, the sum of all internal torques of any system is always 0 (this is the rotational analogue of Newton's Third Law). Therefore, for a ''closed'' system (where there is no net external torque), the ''total'' torque on the system must be 0, which means that the total angular momentum of the system is constant. The conservation of angular momentum helps explain many observed phenomena, for example the increase in rotational speed of a spinning figure skater as the skater's arms are contracted, the high rotational rates of neutron stars, the Coriolis effect, and the precession of gyroscopes. In general, conservation does limit the possible motion of a system, but does not uniquely determine what the exact motion is.
In quantum mechanics, angular momentum (like other quantities) is expressed as an operator, and its one-dimensional projections have quantized eigenvalues. Angular momentum is subject to the Heisenberg uncertainty principle, implying that at any time, only one projection (also called "component") can be measured with definite precision; the other two then remain uncertain. Because of this, the notion of a quantum particle literally "spinning" about an axis does not exist. Quantum particles ''do'' possess a type of non-orbital angular momentum called "spin", but this angular momentum does not correspond to actual physical spinning motion.

Definition in classical mechanics

** Orbital angular momentum in two dimensions **

Angular momentum is a vector quantity (more precisely, a pseudovector) that represents the product of a body's rotational inertia and rotational velocity (in radians/sec) about a particular axis. However, if the particle's trajectory lies in a single plane, it is sufficient to discard the vector nature of angular momentum, and treat it as a scalar (more precisely, a pseudoscalar). Angular momentum can be considered a rotational analog of linear momentum. Thus, where linear momentum is proportional to mass and linear speed
:$p\; =\; mv,$
angular momentum is proportional to moment of inertia and angular speed measured in radians per second.
:$L\; =\; I\backslash omega.$
Unlike mass, which depends only on amount of matter, moment of inertia is also dependent on the position of the axis of rotation and the shape of the matter. Unlike linear velocity, which does not depend upon the choice of origin, orbital angular velocity is always measured with respect to a fixed origin. Therefore, strictly speaking, should be referred to as the angular momentum ''relative to that center''.
Because $I\; =\; r^2m$ for a single particle and $\backslash omega\; =\; \backslash frac$ for circular motion, angular momentum can be expanded, $L\; =\; r^2\; m\; \backslash cdot\; \backslash frac,$ and reduced to,
:$L\; =\; rmv,$
the product of the radius of rotation and the linear momentum of the particle $p\; =\; mv$, where in this case is the equivalent linear (tangential) speed at the radius ($=\; r\backslash omega$).
This simple analysis can also apply to non-circular motion if only the component of the motion which is perpendicular to the radius vector is considered. In that case,
:$L\; =\; rmv\_\backslash perp,$
where $v\_\backslash perp\; =\; v\backslash sin(\backslash theta)$ is the perpendicular component of the motion. Expanding, $L\; =\; rmv\backslash sin(\backslash theta),$ rearranging, $L\; =\; r\backslash sin(\backslash theta)mv,$ and reducing, angular momentum can also be expressed,
:$L\; =\; r\_\backslash perp\; mv,$
where $r\_\backslash perp\; =\; r\backslash sin(\backslash theta)$ is the length of the ''moment arm'', a line dropped perpendicularly from the origin onto the path of the particle. It is this definition, to which the term ''moment of momentum'' refers.

** Scalar—angular momentum from Lagrangian mechanics **

Another approach is to define angular momentum as the conjugate momentum (also called canonical momentum) of the angular coordinate $\backslash phi$ expressed in the Lagrangian of the mechanical system. Consider a mechanical system with a mass $m$ constrained to move in a circle of radius $a$ in the absence of any external force field. The kinetic energy of the system is
:$T\; =\; \backslash fracma^2\; \backslash omega^2\; =\; \backslash fracma^2\; \backslash dot^2.$
And the potential energy is
:$U\; =\; 0.$
Then the Lagrangian is
:$\backslash mathcal\backslash left(\backslash phi,\; \backslash dot\backslash right)\; =\; T\; -\; U\; =\; \backslash fracma^2\; \backslash dot^2.$
The ''generalized momentum'' "canonically conjugate to" the coordinate $\backslash phi$ is defined by
:$p\_\backslash phi\; =\; \backslash frac\; =\; ma^2\; \backslash dot\; =\; I\backslash omega\; =\; L.$

** Orbital angular momentum in three dimensions **

To completely define orbital angular momentum in three dimensions, it is required to know the rate at which the position vector sweeps out angle, the direction perpendicular to the instantaneous plane of angular displacement, and the mass involved, as well as how this mass is distributed in space. By retaining this vector nature of angular momentum, the general nature of the equations is also retained, and can describe any sort of three-dimensional motion about the center of rotation – circular, linear, or otherwise. In vector notation, the orbital angular momentum of a point particle in motion about the origin can be expressed as:
:$\backslash mathbf\; =\; I\backslash boldsymbol,$
where
::$I\; =\; r^2m$ is the moment of inertia for a point mass,
::$\backslash boldsymbol=\backslash frac$ is the orbital angular velocity in radians/sec (units 1/sec) of the particle about the origin,
::$\backslash mathbf$ is the position vector of the particle relative to the origin, $r=\backslash left\backslash vert\backslash mathbf\backslash right\backslash vert$,
::$\backslash mathbf$ is the linear velocity of the particle relative to the origin, and
::$m$ is the mass of the particle.
This can be expanded, reduced, and by the rules of vector algebra, rearranged:
:$\backslash begin\; \backslash mathbf\; \&=\; \backslash left(r^2m\backslash right)\backslash left(\backslash frac\backslash right)\; \backslash \backslash \; \&=\; m\backslash left(\backslash mathbf\backslash times\backslash mathbf\backslash right)\; \backslash \backslash \; \&=\; \backslash mathbf\backslash times\; m\backslash mathbf\; \backslash \backslash \; \&=\; \backslash mathbf\backslash times\backslash mathbf,\; \backslash end$
which is the cross product of the position vector $\backslash mathbf$ and the linear momentum $\backslash mathbf\; =\; m\backslash mathbf$ of the particle. By the definition of the cross product, the $\backslash mathbf$ vector is perpendicular to both $\backslash mathbf$ and $\backslash mathbf$. It is directed perpendicular to the plane of angular displacement, as indicated by the right-hand rule – so that the angular velocity is seen as counter-clockwise from the head of the vector. Conversely, the $\backslash mathbf$ vector defines the plane in which $\backslash mathbf$ and $\backslash mathbf$ lie.
By defining a unit vector $\backslash mathbf$ perpendicular to the plane of angular displacement, a scalar angular speed $\backslash omega$ results, where
:$\backslash omega\backslash mathbf\; =\; \backslash boldsymbol,$ and
:$\backslash omega\; =\; \backslash frac,$ where $v\_\backslash perp$ is the perpendicular component of the motion, as above.
The two-dimensional scalar equations of the previous section can thus be given direction:
:$\backslash begin\; \backslash mathbf\; \&=\; I\backslash boldsymbol\backslash \backslash \; \&=\; I\backslash omega\backslash mathbf\backslash \backslash \; \&=\; \backslash left(r^2m\backslash right)\backslash omega\backslash mathbf\backslash \backslash \; \&=\; rmv\_\backslash perp\; \backslash mathbf\backslash \backslash \; \&=\; r\_\backslash perp\; mv\backslash mathbf,\; \backslash end$
and $\backslash mathbf\; =\; rmv\backslash mathbf$ for circular motion, where all of the motion is perpendicular to the radius $r$.
In the spherical coordinate system the angular momentum vector expresses as
: $\backslash mathbf\; =\; m\; \backslash mathbf\; \backslash times\; \backslash mathbf\; =\; m\; r^2\; \backslash left(\backslash dot\backslash theta\backslash ,\backslash hat\; -\; \backslash dot\backslash varphi\; \backslash sin\backslash theta\backslash ,\backslash mathbf\backslash right).$

** Analogy to linear momentum **

Angular momentum can be described as the rotational analog of linear momentum. Like linear momentum it involves elements of mass and displacement. Unlike linear momentum it also involves elements of position and shape.
Many problems in physics involve matter in motion about some certain point in space, be it in actual rotation about it, or simply moving past it, where it is desired to know what effect the moving matter has on the point—can it exert energy upon it or perform work about it? Energy, the ability to do work, can be stored in matter by setting it in motion—a combination of its inertia and its displacement. Inertia is measured by its mass, and displacement by its velocity. Their product,
:$\backslash begin\; (\backslash text)\; \backslash times\; (\backslash text)\&=\backslash text\backslash \backslash \; \backslash text\; \backslash times\; \backslash text\; \&=\; \backslash text\backslash \backslash \; m\; \backslash times\; v\; \&=\; p\backslash \backslash \; \backslash end$
is the matter's momentum. Referring this momentum to a central point introduces a complication: the momentum is not applied to the point directly. For instance, a particle of matter at the outer edge of a wheel is, in effect, at the end of a lever of the same length as the wheel's radius, its momentum turning the lever about the center point. This imaginary lever is known as the ''moment arm''. It has the effect of multiplying the momentum's effort in proportion to its length, an effect known as a ''moment''. Hence, the particle's momentum referred to a particular point,
:$\backslash begin\; (\backslash text)\; \backslash times\; (\backslash text)\; \backslash times\; (\backslash text)\&=\backslash text\backslash \backslash \; \backslash text\; \backslash times\; \backslash text\; \backslash times\; \backslash text\; \&=\; \backslash text\backslash \backslash \; r\; \backslash times\; m\; \backslash times\; v\; \&=\; L\backslash \backslash \; \backslash end$
is the ''angular momentum'', sometimes called, as here, the ''moment of momentum'' of the particle versus that particular center point. The equation $L=rmv$ combines a moment (a mass $m$ turning moment arm $r$) with a linear (straight-line equivalent) speed $v$. Linear speed referred to the central point is simply the product of the distance $r$ and the angular speed $\backslash omega$ versus the point: $v=r\backslash omega,$ another moment. Hence, angular momentum contains a double moment: $L=rmr\backslash omega.$ Simplifying slightly, $L=r^2m\backslash omega,$ the quantity $r^2m$ is the particle's moment of inertia, sometimes called the second moment of mass. It is a measure of rotational inertia.
Because moment of inertia is a crucial part of the spin angular momentum, the latter necessarily includes all of the complications of the former, which is calculated by multiplying elementary bits of the mass by the squares of their distances from the center of rotation. Therefore, the total moment of inertia, and the angular momentum, is a complex function of the configuration of the matter about the center of rotation and the orientation of the rotation for the various bits.
For a rigid body, for instance a wheel or an asteroid, the orientation of rotation is simply the position of the rotation axis versus the matter of the body. It may or may not pass through the center of mass, or it may lie completely outside of the body. For the same body, angular momentum may take a different value for every possible axis about which rotation may take place. It reaches a minimum when the axis passes through the center of mass.
For a collection of objects revolving about a center, for instance all of the bodies of the Solar System, the orientations may be somewhat organized, as is the Solar System, with most of the bodies' axes lying close to the system's axis. Their orientations may also be completely random.
In brief, the more mass and the farther it is from the center of rotation (the longer the moment arm), the greater the moment of inertia, and therefore the greater the angular momentum for a given angular velocity. In many cases the moment of inertia, and hence the angular momentum, can be simplified by,
:$I=k^2m,$
:where $k$ is the radius of gyration, the distance from the axis at which the entire mass $m$ may be considered as concentrated.
Similarly, for a point mass $m$ the moment of inertia is defined as,
:$I=r^2m$
:where $r$ is the radius of the point mass from the center of rotation,
and for any collection of particles $m\_i$ as the sum,
:$\backslash sum\_i\; I\_i\; =\; \backslash sum\_i\; r\_i^2m\_i$
Angular momentum's dependence on position and shape is reflected in its units versus linear momentum: kg⋅m^{2}/s, N⋅m⋅s, or J⋅s for angular momentum versus kg⋅m/s or N⋅s for linear momentum. When calculating angular momentum as the product of the moment of inertia times the angular velocity, the angular velocity must be expressed in radians per second, where the radian assumes the dimensionless value of unity. (When performing dimensional analysis, it may be productive to use orientational analysis which treats radians as a base unit, but this is outside the scope of the International system of units). Angular momentum's units can be interpreted as torque⋅time or as energy⋅time per angle. An object with angular momentum of can be reduced to zero rotation (all of the rotational energy can be transferred out of it) by an angular impulse of or equivalently, by torque or work of for one second, or energy of for one second.
The plane perpendicular to the axis of angular momentum and passing through the center of mass is sometimes called the ''invariable plane'', because the direction of the axis remains fixed if only the interactions of the bodies within the system, free from outside influences, are considered. One such plane is the invariable plane of the Solar System.

** Angular momentum and torque **

Newton's second law of motion can be expressed mathematically,
:$\backslash mathbf\; =\; m\backslash mathbf,$
or force = mass × acceleration. The rotational equivalent for point particles may be derived as follows:
:$\backslash mathbf\; =\; I\backslash boldsymbol$
which means that the torque (i.e. the time derivative of the angular momentum) is
:$\backslash boldsymbol\; =\; \backslash frac\backslash boldsymbol\; +\; I\backslash frac.$
Because the moment of inertia is $mr^2$, it follows that $\backslash frac\; =\; 2mr\backslash frac\; =\; 2rp\_$, and $\backslash frac\; =\; I\backslash frac\; +\; 2rp\_\backslash boldsymbol,$ which, reduces to
:$\backslash boldsymbol\; =\; I\backslash boldsymbol\; +\; 2rp\_\backslash boldsymbol.$
This is the rotational analog of Newton's Second Law. Note that the torque is not necessarily proportional or parallel to the angular acceleration (as one might expect). The reason for this is that the moment of inertia of a particle can change with time, something that cannot occur for ordinary mass.

Conservation of angular momentum

General considerations

A rotational analog of Newton's third law of motion might be written, "In a closed system, no torque can be exerted on any matter without the exertion on some other matter of an equal and opposite torque." Hence, ''angular momentum can be exchanged between objects in a closed system, but total angular momentum before and after an exchange remains constant (is conserved).'' Seen another way, a rotational analogue of Newton's first law of motion might be written, "A rigid body continues in a state of uniform rotation unless acted by an external influence." Thus ''with no external influence to act upon it, the original angular momentum of the system remains constant''. The conservation of angular momentum is used in analyzing ''central force motion''. If the net force on some body is directed always toward some point, the ''center'', then there is no torque on the body with respect to the center, as all of the force is directed along the radius vector, and none is perpendicular to the radius. Mathematically, torque $\backslash boldsymbol\; =\; \backslash mathbf\; \backslash times\; \backslash mathbf\; =\; \backslash mathbf,$ because in this case $\backslash mathbf$ and $\backslash mathbf$ are parallel vectors. Therefore, the angular momentum of the body about the center is constant. This is the case with gravitational attraction in the orbits of planets and satellites, where the gravitational force is always directed toward the primary body and orbiting bodies conserve angular momentum by exchanging distance and velocity as they move about the primary. Central force motion is also used in the analysis of the Bohr model of the atom. For a planet, angular momentum is distributed between the spin of the planet and its revolution in its orbit, and these are often exchanged by various mechanisms. The conservation of angular momentum in the Earth–Moon system results in the transfer of angular momentum from Earth to Moon, due to tidal torque the Moon exerts on the Earth. This in turn results in the slowing down of the rotation rate of Earth, at about 65.7 nanoseconds per day, and in gradual increase of the radius of Moon's orbit, at about 3.82 centimeters per year. The conservation of angular momentum explains the angular acceleration of an ice skater as she brings her arms and legs close to the vertical axis of rotation. By bringing part of the mass of her body closer to the axis, she decreases her body's moment of inertia. Because angular momentum is the product of moment of inertia and angular velocity, if the angular momentum remains constant (is conserved), then the angular velocity (rotational speed) of the skater must increase. The same phenomenon results in extremely fast spin of compact stars (like white dwarfs, neutron stars and black holes) when they are formed out of much larger and slower rotating stars. Decrease in the size of an object ''n'' times results in increase of its angular velocity by the factor of ''n''^{2}.
Conservation is not always a full explanation for the dynamics of a system but is a key constraint. For example, a spinning top is subject to gravitational torque making it lean over and change the angular momentum about the nutation axis, but neglecting friction at the point of spinning contact, it has a conserved angular momentum about its spinning axis, and another about its precession axis. Also, in any planetary system, the planets, star(s), comets, and asteroids can all move in numerous complicated ways, but only so that the angular momentum of the system is conserved.
Noether's theorem states that every conservation law is associated with a symmetry (invariant) of the underlying physics. The symmetry associated with conservation of angular momentum is rotational invariance. The fact that the physics of a system is unchanged if it is rotated by any angle about an axis implies that angular momentum is conserved.

Relation to Newton's second law of motion

While angular momentum total conservation can be understood separately from Newton's laws of motion as stemming from Noether's theorem in systems symmetric under rotations, it can also be understood simply as an efficient method of calculation of results that can also be otherwise arrived at directly from Newton's second law, together with laws governing the forces of nature (such as Newton's third law, Maxwell's equations and Lorentz force). Indeed, given initial conditions of position and velocity for every point, and the forces at such a condition, one may use Newton's second law to calculate the second derivative of position, and solving for this gives full information on the development of the physical system with time. Note, however, that this is no longer true in quantum mechanics, due to the existence of particle spin, which is angular momentum that cannot be described by the cumulative effect of point-like motions in space. As an example, consider decreasing of the moment of inertia, e.g. when a figure skater is pulling in her/his hands, speeding up the circular motion. In terms of angular momentum conservation, we have, for angular momentum ''L'', moment of inertia ''I'' and angular velocity ''ω'': :$0\; =\; dL\; =\; d\; (I\backslash cdot\; \backslash omega)\; =\; dI\; \backslash cdot\; \backslash omega\; +\; I\; \backslash cdot\; d\backslash omega$ Using this, we see that the change requires an energy of: :$dE\; =\; d\; \backslash left(\backslash frac\; I\backslash cdot\; \backslash omega^2\backslash right)\; =\; \backslash frac\; dI\; \backslash cdot\; \backslash omega^2\; +\; I\; \backslash cdot\; \backslash omega\; \backslash cdot\; d\backslash omega\; =\; -\backslash frac\; dI\; \backslash cdot\; \backslash omega^2$ so that a decrease in the moment of inertia requires investing energy. This can be compared to the work done as calculated using Newton's laws. Each point in the rotating body is accelerating, at each point of time, with radial acceleration of: :$-r\backslash cdot\; \backslash omega^2$ Let us observe a point of mass ''m'', whose position vector relative to the center of motion is parallel to the z-axis at a given point of time, and is at a distance ''z''. The centripetal force on this point, keeping the circular motion, is: :$-m\backslash cdot\; z\backslash cdot\; \backslash omega^2$ Thus the work required for moving this point to a distance ''dz'' farther from the center of motion is: :$dW\; =\; -m\backslash cdot\; z\backslash cdot\; \backslash omega^2\backslash cdot\; dz\; =\; -m\backslash cdot\; \backslash omega^2\backslash cdot\; d\backslash left(\backslash frac\; z^2\backslash right)$ For a non-pointlike body one must integrate over this, with ''m'' replaced by the mass density per unit ''z''. This gives: :$dW\; =\; -\; \backslash fracdI\; \backslash cdot\; \backslash omega^2$ which is exactly the energy required for keeping the angular momentum conserved. Note, that the above calculation can also be performed per mass, using kinematics only. Thus the phenomena of figure skater accelerating tangential velocity while pulling her/his hands in, can be understood as follows in layman's language: The skater's palms are not moving in a straight line, so they are constantly accelerating inwards, but do not gain additional speed because the accelerating is always done when their motion inwards is zero. However, this is different when pulling the palms closer to the body: The acceleration due to rotation now increases the speed; but because of the rotation, the increase in speed does not translate to a significant speed inwards, but to an increase of the rotation speed.

In Lagrangian formalism

In Lagrangian mechanics, angular momentum for rotation around a given axis, is the conjugate momentum of the generalized coordinate of the angle around the same axis. For example, $L\_z$, the angular momentum around the z axis, is: :$L\_z\; =\; \backslash frac$ where $\backslash cal$ is the Lagrangian and $\backslash theta\_z$ is the angle around the z axis. Note that $\backslash dot\backslash theta\_z$, the time derivative of the angle, is the angular velocity $\backslash omega\_z$. Ordinarily, the Lagrangian depends on the angular velocity through the kinetic energy: The latter can be written by separating the velocity to its radial and tangential part, with the tangential part at the x-y plane, around the z-axis, being equal to: :$\backslash sum\_i\; \backslash fracm\_i\; \_i^2\; =\; \backslash sum\_i\; \backslash fracm\_i\; (x\_i^2+y\_i^2)\; ^2$ where the subscript i stands for the i-th body, and ''m'', ''v''_{''T''} and ''ω''_{''z''} stand for mass, tangential velocity around the z-axis and angular velocity around that axis, respectively.
For a body that is not point-like, with density ''ρ'', we have instead:
:$\backslash frac\backslash int\; \backslash rho(x,y,z)(x\_i^2+y\_i^2)\; ^2\; =\; \backslash frac\; \_i\; ^2$
where ''I''_{z} is the moment of inertia around the z-axis.
Thus, assuming the potential energy does not depend on ''ω''_{''z''} (this assumption may fail for electromagnetic systems), we have the angular momentum of the i-th object:
:$\backslash begin\; \_i\; \&=\; \backslash frac\; =\; \backslash frac\; \backslash \backslash \; \&=\; \_i\; \backslash cdot\; \_i\; \backslash end$
We have thus far rotated each object by a separate angle; we may also define an overall angle ''θ''_{z} by which we rotate the whole system, thus rotating also each object around the z-axis, and have the overall angular momentum:
:$L\_z\; =\; \backslash sum\_i\; \_i\; \backslash cdot\; \_i$
From Euler-Lagrange equations it then follows that:
:$0\; =\; \backslash frac\; -\; \backslash frac\backslash left(\backslash frac\backslash right)\; =\; \backslash frac\; -\; \backslash frac$
Since the lagrangian is dependent upon the angles of the object only through the potential, we have:
:$\backslash frac\; =\; \backslash frac\; =\; -\backslash frac$
which is the torque on the i-th object.
Suppose the system is invariant to rotations, so that the potential is independent of an overall rotation by the angle ''θ''_{z} (thus it may depend on the angles of objects only through their differences, in the form $V(\_i,\; \_j)\; =\; V(\_i\; -\; \_j)$). We therefore get for the total angular momentum:
:$\backslash frac\; =\; -\backslash frac\; =\; 0$
And thus the angular momentum around the z-axis is conserved.
This analysis can be repeated separately for each axis, giving conversation of the angular momentum vector. However, the angles around the three axes cannot be treated simultaneously as generalized coordinates, since they are not independent; in particular, two angles per point suffice to determine its position. While it is true that in the case of a rigid body, fully describing it requires, in addition to three translational degrees of freedom, also specification of three rotational degrees of freedom; however these cannot be defined as rotations around the Cartesian axes (see Euler angles). This caveat is reflected in quantum mechanics in the non-trivial commutation relations of the different components of the angular momentum operator.

In Hamiltonian formalism

Equivalently, in Hamiltonian mechanics the Hamiltonian can be described as a function of the angular momentum. As before, the part of the kinetic energy related to rotation around the z-axis for the i-th object is: :$\backslash frac\; \_i\; ^2\; =\; \backslash frac$ which is analogous to the energy dependence upon momentum along the z-axis, $\backslash frac$. Hamilton's equations relate the angle around the z-axis to its conjugate momentum, the angular momentum around the same axis: :$\backslash begin\; \backslash frac\; \&=\; \backslash frac\; =\; \backslash frac\; \backslash \backslash \; \backslash frac\; \&=\; -\backslash frac\; =\; -\backslash frac\; \backslash end$ The first equation gives :$\_i\; =\; \_i\; \backslash cdot\; =\; \_i\; \backslash cdot\; \_i$ And so we get the same results as in the Lagrangian formalism. Note, that for combining all axes together, we write the kinetic energy as: :$E\_k\; =\; \backslash frac\backslash sum\_i\; \backslash frac\; =\; \backslash sum\_i\; \backslash left(\backslash frac\; +\; \backslash frac^\backslash textsf^\; \backslash bf\_i\backslash right)$ where ''p''_{r} is the momentum in the radial direction, and the moment of inertia is a 3-dimensional matrix; bold letters stand for 3-dimensional vectors.
For point-like bodies we have:
:$E\_k\; =\; \backslash sum\_i\; \backslash left(\backslash frac\; +\; \backslash frac\backslash right)$
This form of the kinetic energy part of the Hamiltonian is useful in analyzing central potential problems, and is easily transformed to a quantum mechanical work frame (e.g. in the hydrogen atom problem).

** Angular momentum in orbital mechanics **

While in classical mechanics the language of angular momentum can be replaced by Newton's laws of motion, it is particularly useful for motion in central potential such as planetary motion in the solar system. Thus, the orbit of a planet in the solar system is defined by its energy, angular momentum and angles of the orbit major axis relative to a coordinate frame.
In astrodynamics and celestial mechanics, a ''massless'' (or ''per unit mass'') angular momentum is defined
:$\backslash mathbf\; =\; \backslash mathbf\; \backslash times\; \backslash mathbf,$
called ''specific angular momentum''. Note that $\backslash mathbf\; =\; m\backslash mathbf.$ Mass is often unimportant in orbital mechanics calculations, because motion is defined by gravity. The primary body of the system is often so much larger than any bodies in motion about it that the smaller bodies have a negligible gravitational effect on it; it is, in effect, stationary. All bodies are apparently attracted by its gravity in the same way, regardless of mass, and therefore all move approximately the same way under the same conditions.

** Solid bodies **

Angular momentum is also an extremely useful concept for describing rotating rigid bodies such as a gyroscope or a rocky planet.
For a continuous mass distribution with density function ''ρ''(r), a differential volume element ''dV'' with position vector r within the mass has a mass element ''dm'' = ''ρ''(r)''dV''. Therefore, the infinitesimal angular momentum of this element is:
:$d\backslash mathbf\; =\; \backslash mathbf\backslash times\; dm\; \backslash mathbf\; =\; \backslash mathbf\backslash times\; \backslash rho(\backslash mathbf)\; dV\; \backslash mathbf\; =\; dV\; \backslash mathbf\backslash times\; \backslash rho(\backslash mathbf)\; \backslash mathbf$
and integrating this differential over the volume of the entire mass gives its total angular momentum:
:$\backslash mathbf=\backslash int\_V\; dV\; \backslash mathbf\backslash times\; \backslash rho(\backslash mathbf)\; \backslash mathbf$
In the derivation which follows, integrals similar to this can replace the sums for the case of continuous mass.

** Collection of particles **

For a collection of particles in motion about an arbitrary origin, it is informative to develop the equation of angular momentum by resolving their motion into components about their own center of mass and about the origin. Given,
: $m\_i$ is the mass of particle $i$,
: $\backslash mathbf\_i$ is the position vector of particle $i$ vs the origin,
: $\backslash mathbf\_i$ is the velocity of particle $i$ vs the origin,
: $\backslash mathbf$ is the position vector of the center of mass vs the origin,
: $\backslash mathbf$ is the velocity of the center of mass vs the origin,
: $\backslash mathbf\_i$ is the position vector of particle $i$ vs the center of mass,
: $\backslash mathbf\_i$ is the velocity of particle $i$ vs the center of mass,
The total mass of the particles is simply their sum,
:$M=\backslash sum\_i\; m\_i.$
The position vector of the center of mass is defined by,
:$M\backslash mathbf=\backslash sum\_i\; m\_i\; \backslash mathbf\_i.$
By inspection,
: $\backslash mathbf\_i\; =\; \backslash mathbf\; +\; \backslash mathbf\_i$ and $\backslash mathbf\_i\; =\; \backslash mathbf\; +\; \backslash mathbf\_i.$
The total angular momentum of the collection of particles is the sum of the angular momentum of each particle,
Expanding $\backslash mathbf\_i$,
: $\backslash begin\; \backslash mathbf\; \&=\; \backslash sum\_i\; \backslash leftleft(\backslash mathbf\; +\; \backslash mathbf\_i\backslash right)\; \backslash times\; m\_i\backslash mathbf\_i\; \backslash right\backslash \backslash \; \&=\; \backslash sum\_i\; \backslash left\backslash mathbf\; \backslash times\; m\_i\backslash mathbf\_i\; +\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\_i\; \backslash right\backslash end$
Expanding $\backslash mathbf\_i$,
: $\backslash begin\; \backslash mathbf\; \&=\; \backslash sum\_i\; \backslash left\backslash mathbf\; \backslash times\; m\_i\backslash left(\backslash mathbf\; +\; \backslash mathbf\_i\backslash right)\; +\; \backslash mathbf\_i\; \backslash times\; m\_i(\backslash mathbf\; +\; \backslash mathbf\_i)\; \backslash right\backslash \; \&=\; \backslash sum\_i\; \backslash left\backslash mathbf\; \backslash times\; m\_i\backslash mathbf\; +\; \backslash mathbf\; \backslash times\; m\_i\backslash mathbf\_i\; +\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\; +\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\_i\; \backslash right\backslash \; \&=\; \backslash sum\_i\; \backslash mathbf\; \backslash times\; m\_i\backslash mathbf\; +\; \backslash sum\_i\; \backslash mathbf\; \backslash times\; m\_i\backslash mathbf\_i\; +\; \backslash sum\_i\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\; +\; \backslash sum\_i\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\_i\; \backslash end$
It can be shown that (see sidebar),
: $\backslash sum\_i\; m\_i\backslash mathbf\_i\; =\; \backslash mathbf$ and $\backslash sum\_i\; m\_i\backslash mathbf\_i\; =\; \backslash mathbf,$
therefore the second and third terms vanish,
: $\backslash mathbf\; =\; \backslash sum\_i\; \backslash mathbf\; \backslash times\; m\_i\backslash mathbf\; +\; \backslash sum\_i\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\_i\; .$
The first term can be rearranged,
: $\backslash sum\_i\; \backslash mathbf\; \backslash times\; m\_i\backslash mathbf\; =\; \backslash mathbf\; \backslash times\; \backslash sum\_i\; m\_i\backslash mathbf\; =\; \backslash mathbf\; \backslash times\; M\backslash mathbf,$
and total angular momentum for the collection of particles is finally,
The first term is the angular momentum of the center of mass relative to the origin. Similar to Single particle, below, it is the angular momentum of one particle of mass ''M'' at the center of mass moving with velocity V. The second term is the angular momentum of the particles moving relative to the center of mass, similar to Fixed center of mass, below. The result is general—the motion of the particles is not restricted to rotation or revolution about the origin or center of mass. The particles need not be individual masses, but can be elements of a continuous distribution, such as a solid body.
Rearranging equation () by vector identities, multiplying both terms by "one", and grouping appropriately,
:$\backslash begin\; \backslash mathbf\; \&=\; M(\backslash mathbf\; \backslash times\; \backslash mathbf)\; +\; \backslash sum\_i\; \backslash left\_i\backslash left(\backslash mathbf\_i\; \backslash times\; \backslash mathbf\_i\backslash right)\backslash right\backslash \backslash \; \&=\; \backslash fracM\backslash left(\backslash mathbf\; \backslash times\; \backslash mathbf\backslash right)\; +\; \backslash sum\_i\; \backslash left\backslash fracm\_i\backslash left(\backslash mathbf\_i\; \backslash times\; \backslash mathbf\_i\backslash right)\backslash right,\; \backslash \backslash \; \&=\; R^2M\; \backslash left(\; \backslash frac\; \backslash right)\; +\; \backslash sum\_i\; \backslash leftr\_i^2\; m\_i\; \backslash left(\; \backslash frac\; \backslash right)\; \backslash right,\; \backslash \backslash \; \backslash end$
gives the total angular momentum of the system of particles in terms of moment of inertia $I$ and angular velocity $\backslash boldsymbol$,

** Single particle case **

In the case of a single particle moving about the arbitrary origin,
:$\backslash begin\; \backslash mathbf\_i\; \&=\; \backslash mathbf\_i\; =\; \backslash mathbf,\; \backslash \backslash \; \backslash mathbf\; \&=\; \backslash mathbf,\; \backslash \backslash \; \backslash mathbf\; \&=\; \backslash mathbf,\; \backslash \backslash \; m\; \&=\; M,\; \backslash end$
:$\backslash sum\_i\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\_i\; =\; \backslash mathbf,$
:$\backslash sum\_i\; I\_i\backslash boldsymbol\_i\; =\; \backslash mathbf,$ and equations () and () for total angular momentum reduce to,
:$\backslash mathbf\; =\; \backslash mathbf\; \backslash times\; m\backslash mathbf\; =\; I\_R\backslash boldsymbol\_R.$

** Case of a fixed center of mass **

For the case of the center of mass fixed in space with respect to the origin,
:$\backslash mathbf\; =\; \backslash mathbf,$
:$\backslash mathbf\; \backslash times\; M\backslash mathbf\; =\; \backslash mathbf,$
:$I\_R\backslash boldsymbol\_R\; =\; \backslash mathbf,$ and equations () and () for total angular momentum reduce to,
:$\backslash mathbf\; =\; \backslash sum\_i\; \backslash mathbf\_i\; \backslash times\; m\_i\backslash mathbf\_i\; =\; \backslash sum\_i\; I\_i\backslash boldsymbol\_i.$

** Angular momentum in general relativity **

In modern (20th century) theoretical physics, angular momentum (not including any intrinsic angular momentum – see below) is described using a different formalism, instead of a classical pseudovector. In this formalism, angular momentum is the 2-form Noether charge associated with rotational invariance. As a result, angular momentum is not conserved for general curved spacetimes, unless it happens to be asymptotically rotationally invariant.
In classical mechanics, the angular momentum of a particle can be reinterpreted as a plane element:
:$\backslash mathbf\; =\; \backslash mathbf\; \backslash wedge\; \backslash mathbf\; \backslash ,,$
in which the exterior product ∧ replaces the cross product × (these products have similar characteristics but are nonequivalent). This has the advantage of a clearer geometric interpretation as a plane element, defined from the x and p vectors, and the expression is true in any number of dimensions (two or higher). In Cartesian coordinates:
:$\backslash begin\; \backslash mathbf\; \&=\; \backslash left(xp\_y\; -\; yp\_x\backslash right)\backslash mathbf\_x\; \backslash wedge\; \backslash mathbf\_y\; +\; \backslash left(yp\_z\; -\; zp\_y\backslash right)\backslash mathbf\_y\; \backslash wedge\; \backslash mathbf\_z\; +\; \backslash left(zp\_x\; -\; xp\_z\backslash right)\backslash mathbf\_z\; \backslash wedge\; \backslash mathbf\_x\backslash \backslash \; \&=\; L\_\backslash mathbf\_x\; \backslash wedge\; \backslash mathbf\_y\; +\; L\_\backslash mathbf\_y\; \backslash wedge\; \backslash mathbf\_z\; +\; L\_\backslash mathbf\_z\; \backslash wedge\; \backslash mathbf\_x\; \backslash ,,\; \backslash end$
or more compactly in index notation:
:$L\_\; =\; x\_i\; p\_j\; -\; x\_j\; p\_i\backslash ,.$
The angular velocity can also be defined as an antisymmetric second order tensor, with components ''ω_{ij}''. The relation between the two antisymmetric tensors is given by the moment of inertia which must now be a fourth order tensor:
:$L\_\; =\; I\_\; \backslash omega\_\; \backslash ,.$
Again, this equation in L and ω as tensors is true in any number of dimensions. This equation also appears in the geometric algebra formalism, in which L and ω are bivectors, and the moment of inertia is a mapping between them.
In relativistic mechanics, the relativistic angular momentum of a particle is expressed as an antisymmetric tensor of second order:
:$M\_\; =\; X\_\backslash alpha\; P\_\backslash beta\; -\; X\_\backslash beta\; P\_\backslash alpha$
in the language of four-vectors, namely the four position ''X'' and the four momentum ''P'', and absorbs the above L together with the motion of the centre of mass of the particle.
In each of the above cases, for a system of particles, the total angular momentum is just the sum of the individual particle angular momenta, and the centre of mass is for the system.

** Angular momentum in quantum mechanics **

Angular momentum in quantum mechanics differs in many profound respects from angular momentum in classical mechanics. In relativistic quantum mechanics, it differs even more, in which the above relativistic definition becomes a tensorial operator.

** Spin, orbital, and total angular momentum **

The classical definition of angular momentum as $\backslash mathbf\; =\; \backslash mathbf\backslash times\backslash mathbf$ can be carried over to quantum mechanics, by reinterpreting r as the quantum position operator and p as the quantum momentum operator. L is then an operator, specifically called the ''orbital angular momentum operator''. The components of the angular momentum operator satisfy the commutation relations of the Lie algebra so(3). Indeed, these operators are precisely the infinitesimal action of the rotation group on the quantum Hilbert space. (See also the discussion below of the angular momentum operators as the generators of rotations.)
However, in quantum physics, there is another type of angular momentum, called ''spin angular momentum'', represented by the spin operator S. Almost all elementary particles have nonzero spin. Spin is often depicted as a particle literally spinning around an axis, but this is a misleading and inaccurate picture: spin is an intrinsic property of a particle, unrelated to any sort of motion in space and fundamentally different from orbital angular momentum. All elementary particles have a characteristic spin (possibly zero), for example electrons have "spin 1/2" (this actually means "spin ħ/2"), photons have "spin 1" (this actually means "spin ħ"), and pi-mesons have spin 0.
Finally, there is total angular momentum J, which combines both the spin and orbital angular momentum of all particles and fields. (For one particle, .) Conservation of angular momentum applies to J, but not to L or S; for example, the spin–orbit interaction allows angular momentum to transfer back and forth between L and S, with the total remaining constant. Electrons and photons need not have integer-based values for total angular momentum, but can also have fractional values.
In molecules the total angular momentum F is the sum of the rovibronic (orbital) angular momentum N, the electron spin angular momentum S, and the nuclear spin angular momentum I. For electronic singlet states the rovibronic angular momentum is denoted J rather than N. As explained by Van Vleck, the components of the molecular rovibronic angular momentum referred to molecule-fixed axes have different commutation relations from those for the components about space-fixed axes.

** Quantization **

In quantum mechanics, angular momentum is quantized – that is, it cannot vary continuously, but only in "quantum leaps" between certain allowed values. For any system, the following restrictions on measurement results apply, where $\backslash hbar$ is the reduced Planck constant and $\backslash hat$ is any Euclidean vector such as x, y, or z:
(There are additional restrictions as well, see angular momentum operator for details.)
The reduced Planck constant $\backslash hbar$ is tiny by everyday standards, about 10^{−34} J s, and therefore this quantization does not noticeably affect the angular momentum of macroscopic objects. However, it is very important in the microscopic world. For example, the structure of electron shells and subshells in chemistry is significantly affected by the quantization of angular momentum.
Quantization of angular momentum was first postulated by Niels Bohr in his Bohr model of the atom and was later predicted by Erwin Schrödinger in his Schrödinger equation.

** Uncertainty **

In the definition $\backslash mathbf=\backslash mathbf\backslash times\backslash mathbf$, six operators are involved: The position operators $r\_x$, $r\_y$, $r\_z$, and the momentum operators $p\_x$, $p\_y$, $p\_z$. However, the Heisenberg uncertainty principle tells us that it is not possible for all six of these quantities to be known simultaneously with arbitrary precision. Therefore, there are limits to what can be known or measured about a particle's angular momentum. It turns out that the best that one can do is to simultaneously measure both the angular momentum vector's magnitude and its component along one axis.
The uncertainty is closely related to the fact that different components of an angular momentum operator do not commute, for example $L\_xL\_y\; \backslash neq\; L\_yL\_x$. (For the precise commutation relations, see angular momentum operator.)

** Total angular momentum as generator of rotations **

As mentioned above, orbital angular momentum L is defined as in classical mechanics: $\backslash mathbf=\backslash mathbf\backslash times\backslash mathbf$, but ''total'' angular momentum J is defined in a different, more basic way: J is defined as the "generator of rotations". More specifically, J is defined so that the operator
:$R(\backslash hat,\backslash phi)\; \backslash equiv\; \backslash exp\backslash left(-\backslash frac\backslash phi\backslash ,\; \backslash mathbf\backslash cdot\; \backslash hat\backslash right)$
is the rotation operator that takes any system and rotates it by angle $\backslash phi$ about the axis $\backslash hat$. (The "exp" in the formula refers to operator exponential) To put this the other way around, whatever our quantum Hilbert space is, we expect that the rotation group SO(3) will act on it. There is then an associated action of the Lie algebra so(3) of SO(3); the operators describing the action of so(3) on our Hilbert space are the (total) angular momentum operators.
The relationship between the angular momentum operator and the rotation operators is the same as the relationship between Lie algebras and Lie groups in mathematics. The close relationship between angular momentum and rotations is reflected in Noether's theorem that proves that angular momentum is conserved whenever the laws of physics are rotationally invariant.

** Angular momentum in electrodynamics **

When describing the motion of a charged particle in an electromagnetic field, the canonical momentum P (derived from the Lagrangian for this system) is not gauge invariant. As a consequence, the canonical angular momentum L = r × P is not gauge invariant either. Instead, the momentum that is physical, the so-called ''kinetic momentum'' (used throughout this article), is (in SI units)
:$\backslash mathbf\; =\; m\backslash mathbf\; =\; \backslash mathbf\; -\; e\; \backslash mathbf$
where ''e'' is the electric charge of the particle and A the magnetic vector potential of the electromagnetic field. The gauge-invariant angular momentum, that is ''kinetic angular momentum'', is given by
:$\backslash mathbf=\; \backslash mathbf\; \backslash times\; (\; \backslash mathbf\; -\; e\backslash mathbf\; )$
The interplay with quantum mechanics is discussed further in the article on canonical commutation relations.

** Angular momentum in optics **

In ''classical Maxwell electrodynamics'' the Poynting vector
is a linear momentum density of electromagnetic field.
:$\backslash mathbf(\backslash mathbf,\; t)\; =\; \backslash epsilon\_0\; c^2\; \backslash mathbf(\backslash mathbf,\; t)\; \backslash times\; \backslash mathbf(\backslash mathbf,\; t).$
The angular momentum density vector $\backslash mathbf(\backslash mathbf,\; t)$ is given by a vector product
as in classical mechanics:
:$\backslash mathbf(\backslash mathbf,\; t)\; =\; \backslash mathbf\; \backslash times\; \backslash mathbf(\backslash mathbf,\; t).$
The above identities are valid ''locally'', i.e. in each space point $\backslash mathbf$ in a given moment $t$.

** History **

Newton, in the ''Principia'', hinted at angular momentum in his examples of the First Law of Motion,
:''A top, whose parts by their cohesion are perpetually drawn aside from rectilinear motions, does not cease its rotation, otherwise than as it is retarded by the air. The greater bodies of the planets and comets, meeting with less resistance in more free spaces, preserve their motions both progressive and circular for a much longer time.''
He did not further investigate angular momentum directly in the ''Principia'',
:''From such kind of reflexions also sometimes arise the circular motions of bodies about their own centres. But these are cases which I do not consider in what follows; and it would be too tedious to demonstrate every particular that relates to this subject.''
However, his geometric proof of the law of areas is an outstanding example of Newton's genius, and indirectly proves angular momentum conservation in the case of a central force.

** The Law of Areas **

** Newton's derivation **

As a planet orbits the Sun, the line between the Sun and the planet sweeps out equal areas in equal intervals of time. This had been known since Kepler expounded his second law of planetary motion. Newton derived a unique geometric proof, and went on to show that the attractive force of the Sun's gravity was the cause of all of Kepler's laws.
During the first interval of time, an object is in motion from point A to point B. Undisturbed, it would continue to point c during the second interval. When the object arrives at B, it receives an impulse directed toward point S. The impulse gives it a small added velocity toward S, such that if this were its only velocity, it would move from B to V during the second interval. By the rules of velocity composition, these two velocities add, and point C is found by construction of parallelogram BcCV. Thus the object's path is deflected by the impulse so that it arrives at point C at the end of the second interval. Because the triangles SBc and SBC have the same base SB and the same height Bc or VC, they have the same area. By symmetry, triangle SBc also has the same area as triangle SAB, therefore the object has swept out equal areas SAB and SBC in equal times.
At point C, the object receives another impulse toward S, again deflecting its path during the third interval from d to D. Thus it continues to E and beyond, the triangles SAB, SBc, SBC, SCd, SCD, SDe, SDE all having the same area. Allowing the time intervals to become ever smaller, the path ABCDE approaches indefinitely close to a continuous curve.
Note that because this derivation is geometric, and no specific force is applied, it proves a more general law than Kepler's second law of planetary motion. It shows that the Law of Areas applies to any central force, attractive or repulsive, continuous or non-continuous, or zero.

** Conservation of angular momentum in the Law of Areas **

The proportionality of angular momentum to the area swept out by a moving object can be understood by realizing that the bases of the triangles, that is, the lines from S to the object, are equivalent to the radius , and that the heights of the triangles are proportional to the perpendicular component of velocity . Hence, if the area swept per unit time is constant, then by the triangular area formula , the product and therefore the product are constant: if and the base length are decreased, and height must increase proportionally. Mass is constant, therefore angular momentum is conserved by this exchange of distance and velocity.
In the case of triangle SBC, area is equal to (SB)(VC). Wherever C is eventually located due to the impulse applied at B, the product (SB)(VC), and therefore remain constant. Similarly so for each of the triangles.

** After Newton **

Leonhard Euler, Daniel Bernoulli, and Patrick d'Arcy all understood angular momentum in terms of conservation of areal velocity, a result of their analysis of Kepler's second law of planetary motion. It is unlikely that they realized the implications for ordinary rotating matter.
In 1736 Euler, like Newton, touched on some of the equations of angular momentum in his ''Mechanica'' without further developing them.
Bernoulli wrote in a 1744 letter of a "moment of rotational motion", possibly the first conception of angular momentum as we now understand it.
In 1799, Pierre-Simon Laplace first realized that a fixed plane was associated with rotation—his ''invariable plane''.
Louis Poinsot in 1803 began representing rotations as a line segment perpendicular to the rotation, and elaborated on the "conservation of moments".
In 1852 Léon Foucault used a gyroscope in an experiment to display the Earth's rotation.
William J. M. Rankine's 1858 ''Manual of Applied Mechanics'' defined angular momentum in the modern sense for the first time:
:''...a line whose length is proportional to the magnitude of the angular momentum, and whose direction is perpendicular to the plane of motion of the body and of the fixed point, and such, that when the motion of the body is viewed from the extremity of the line, the radius-vector of the body seems to have right-handed rotation.''
In an 1872 edition of the same book, Rankine stated that "The term ''angular momentum'' was introduced by Mr. Hayward," probably referring to R.B. Hayward's article ''On a Direct Method of estimating Velocities, Accelerations, and all similar Quantities with respect to Axes moveable in any manner in Space with Applications,'' which was introduced in 1856, and published in 1864. Rankine was mistaken, as numerous publications feature the term starting in the late 18th to early 19th centuries. However, Hayward's article apparently was the first use of the term and the concept seen by much of the English-speaking world. Before this, angular momentum was typically referred to as "momentum of rotation" in English.see, for instance,

** See also **

** Footnotes **

** References **

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** External links **

Conservation of Angular Momentum

– a chapter from an online textbook

– derivation of the three-dimensional case

Angular Momentum and Rolling Motion

– more momentum theory {{Authority control Category:Physical quantities Category:Rotation Category:Conservation laws

Definition in classical mechanics

Conservation of angular momentum

General considerations

A rotational analog of Newton's third law of motion might be written, "In a closed system, no torque can be exerted on any matter without the exertion on some other matter of an equal and opposite torque." Hence, ''angular momentum can be exchanged between objects in a closed system, but total angular momentum before and after an exchange remains constant (is conserved).'' Seen another way, a rotational analogue of Newton's first law of motion might be written, "A rigid body continues in a state of uniform rotation unless acted by an external influence." Thus ''with no external influence to act upon it, the original angular momentum of the system remains constant''. The conservation of angular momentum is used in analyzing ''central force motion''. If the net force on some body is directed always toward some point, the ''center'', then there is no torque on the body with respect to the center, as all of the force is directed along the radius vector, and none is perpendicular to the radius. Mathematically, torque $\backslash boldsymbol\; =\; \backslash mathbf\; \backslash times\; \backslash mathbf\; =\; \backslash mathbf,$ because in this case $\backslash mathbf$ and $\backslash mathbf$ are parallel vectors. Therefore, the angular momentum of the body about the center is constant. This is the case with gravitational attraction in the orbits of planets and satellites, where the gravitational force is always directed toward the primary body and orbiting bodies conserve angular momentum by exchanging distance and velocity as they move about the primary. Central force motion is also used in the analysis of the Bohr model of the atom. For a planet, angular momentum is distributed between the spin of the planet and its revolution in its orbit, and these are often exchanged by various mechanisms. The conservation of angular momentum in the Earth–Moon system results in the transfer of angular momentum from Earth to Moon, due to tidal torque the Moon exerts on the Earth. This in turn results in the slowing down of the rotation rate of Earth, at about 65.7 nanoseconds per day, and in gradual increase of the radius of Moon's orbit, at about 3.82 centimeters per year. The conservation of angular momentum explains the angular acceleration of an ice skater as she brings her arms and legs close to the vertical axis of rotation. By bringing part of the mass of her body closer to the axis, she decreases her body's moment of inertia. Because angular momentum is the product of moment of inertia and angular velocity, if the angular momentum remains constant (is conserved), then the angular velocity (rotational speed) of the skater must increase. The same phenomenon results in extremely fast spin of compact stars (like white dwarfs, neutron stars and black holes) when they are formed out of much larger and slower rotating stars. Decrease in the size of an object ''n'' times results in increase of its angular velocity by the factor of ''n''

Relation to Newton's second law of motion

While angular momentum total conservation can be understood separately from Newton's laws of motion as stemming from Noether's theorem in systems symmetric under rotations, it can also be understood simply as an efficient method of calculation of results that can also be otherwise arrived at directly from Newton's second law, together with laws governing the forces of nature (such as Newton's third law, Maxwell's equations and Lorentz force). Indeed, given initial conditions of position and velocity for every point, and the forces at such a condition, one may use Newton's second law to calculate the second derivative of position, and solving for this gives full information on the development of the physical system with time. Note, however, that this is no longer true in quantum mechanics, due to the existence of particle spin, which is angular momentum that cannot be described by the cumulative effect of point-like motions in space. As an example, consider decreasing of the moment of inertia, e.g. when a figure skater is pulling in her/his hands, speeding up the circular motion. In terms of angular momentum conservation, we have, for angular momentum ''L'', moment of inertia ''I'' and angular velocity ''ω'': :$0\; =\; dL\; =\; d\; (I\backslash cdot\; \backslash omega)\; =\; dI\; \backslash cdot\; \backslash omega\; +\; I\; \backslash cdot\; d\backslash omega$ Using this, we see that the change requires an energy of: :$dE\; =\; d\; \backslash left(\backslash frac\; I\backslash cdot\; \backslash omega^2\backslash right)\; =\; \backslash frac\; dI\; \backslash cdot\; \backslash omega^2\; +\; I\; \backslash cdot\; \backslash omega\; \backslash cdot\; d\backslash omega\; =\; -\backslash frac\; dI\; \backslash cdot\; \backslash omega^2$ so that a decrease in the moment of inertia requires investing energy. This can be compared to the work done as calculated using Newton's laws. Each point in the rotating body is accelerating, at each point of time, with radial acceleration of: :$-r\backslash cdot\; \backslash omega^2$ Let us observe a point of mass ''m'', whose position vector relative to the center of motion is parallel to the z-axis at a given point of time, and is at a distance ''z''. The centripetal force on this point, keeping the circular motion, is: :$-m\backslash cdot\; z\backslash cdot\; \backslash omega^2$ Thus the work required for moving this point to a distance ''dz'' farther from the center of motion is: :$dW\; =\; -m\backslash cdot\; z\backslash cdot\; \backslash omega^2\backslash cdot\; dz\; =\; -m\backslash cdot\; \backslash omega^2\backslash cdot\; d\backslash left(\backslash frac\; z^2\backslash right)$ For a non-pointlike body one must integrate over this, with ''m'' replaced by the mass density per unit ''z''. This gives: :$dW\; =\; -\; \backslash fracdI\; \backslash cdot\; \backslash omega^2$ which is exactly the energy required for keeping the angular momentum conserved. Note, that the above calculation can also be performed per mass, using kinematics only. Thus the phenomena of figure skater accelerating tangential velocity while pulling her/his hands in, can be understood as follows in layman's language: The skater's palms are not moving in a straight line, so they are constantly accelerating inwards, but do not gain additional speed because the accelerating is always done when their motion inwards is zero. However, this is different when pulling the palms closer to the body: The acceleration due to rotation now increases the speed; but because of the rotation, the increase in speed does not translate to a significant speed inwards, but to an increase of the rotation speed.

In Lagrangian formalism

In Lagrangian mechanics, angular momentum for rotation around a given axis, is the conjugate momentum of the generalized coordinate of the angle around the same axis. For example, $L\_z$, the angular momentum around the z axis, is: :$L\_z\; =\; \backslash frac$ where $\backslash cal$ is the Lagrangian and $\backslash theta\_z$ is the angle around the z axis. Note that $\backslash dot\backslash theta\_z$, the time derivative of the angle, is the angular velocity $\backslash omega\_z$. Ordinarily, the Lagrangian depends on the angular velocity through the kinetic energy: The latter can be written by separating the velocity to its radial and tangential part, with the tangential part at the x-y plane, around the z-axis, being equal to: :$\backslash sum\_i\; \backslash fracm\_i\; \_i^2\; =\; \backslash sum\_i\; \backslash fracm\_i\; (x\_i^2+y\_i^2)\; ^2$ where the subscript i stands for the i-th body, and ''m'', ''v''

In Hamiltonian formalism

Equivalently, in Hamiltonian mechanics the Hamiltonian can be described as a function of the angular momentum. As before, the part of the kinetic energy related to rotation around the z-axis for the i-th object is: :$\backslash frac\; \_i\; ^2\; =\; \backslash frac$ which is analogous to the energy dependence upon momentum along the z-axis, $\backslash frac$. Hamilton's equations relate the angle around the z-axis to its conjugate momentum, the angular momentum around the same axis: :$\backslash begin\; \backslash frac\; \&=\; \backslash frac\; =\; \backslash frac\; \backslash \backslash \; \backslash frac\; \&=\; -\backslash frac\; =\; -\backslash frac\; \backslash end$ The first equation gives :$\_i\; =\; \_i\; \backslash cdot\; =\; \_i\; \backslash cdot\; \_i$ And so we get the same results as in the Lagrangian formalism. Note, that for combining all axes together, we write the kinetic energy as: :$E\_k\; =\; \backslash frac\backslash sum\_i\; \backslash frac\; =\; \backslash sum\_i\; \backslash left(\backslash frac\; +\; \backslash frac^\backslash textsf^\; \backslash bf\_i\backslash right)$ where ''p''

Conservation of Angular Momentum

– a chapter from an online textbook

– derivation of the three-dimensional case

Angular Momentum and Rolling Motion

– more momentum theory {{Authority control Category:Physical quantities Category:Rotation Category:Conservation laws