Editing Noether's theorem (section)

==Historical context==
{{main|Constant of motion|conservation law|conserved current}}

A [[conservation law]] states that some quantity ''X'' in the mathematical description of a system's evolution remains constant throughout its motion – it is an [[Invariant (physics)|invariant]].   Mathematically, the rate of change of ''X'' (its [[derivative]] with respect to [[time]]) is zero,

:<math>\frac{dX}{dt} = \dot{X} = 0 ~.</math>

Such quantities are said to be conserved; they are often called [[constant of motion|constants of motion]] (although motion ''per se'' need not be involved, just evolution in time). For example, if the energy of a system is conserved, its energy is invariant at all times, which imposes a constraint on the system's motion and may help in solving for it. Aside from insights that such constants of motion give into the nature of a system, they are a useful calculational tool; for example, an approximate solution can be corrected by finding the nearest state that satisfies the suitable conservation laws.

The earliest constants of motion discovered were [[momentum]] and [[kinetic energy]], which were proposed in the 17th century by [[René Descartes]] and [[Gottfried Leibniz]] on the basis of [[collision]] experiments, and refined by subsequent researchers. [[Isaac Newton]] was the first to enunciate the conservation of momentum in its modern form, and showed that it was a consequence of [[Newton's laws of motion]]. According to [[general relativity]], the conservation laws of linear momentum, energy and angular momentum are only exactly true globally when expressed in terms of the  sum of the [[stress–energy tensor]] (non-gravitational stress–energy) and the [[Stress–energy–momentum pseudotensor#Landau–Lifshitz pseudotensor|Landau–Lifshitz stress–energy–momentum pseudotensor]] (gravitational stress–energy). The local conservation of non-gravitational linear momentum and energy in a free-falling reference frame is expressed by the vanishing of the covariant [[divergence]] of the [[stress–energy tensor]]. Another important conserved quantity, discovered in studies of the [[celestial mechanics]] of astronomical bodies, is the [[Laplace–Runge–Lenz vector]].

In the late 18th and early 19th centuries, physicists developed more systematic methods for discovering invariants. A major advance came in 1788 with the development of [[Lagrangian mechanics]], which is related to the [[principle of least action]]. In this approach, the state of the system can be described by any type of [[generalized coordinate]]s '''q'''; the laws of motion need not be expressed in a [[Cartesian coordinate system]], as was customary in Newtonian mechanics. The [[action (physics)|action]] is defined as the time integral ''I'' of a function known as the [[Lagrangian mechanics|Lagrangian]]&nbsp;''L''

:<math>I = \int L(\mathbf{q}, \dot{\mathbf{q}}, t) \, dt ~,</math>

where the dot over '''q''' signifies the rate of change of the coordinates '''q''',

:<math>\dot{\mathbf{q}} = \frac{d\mathbf{q}}{dt} ~.</math>

[[Hamilton's principle]] states that the physical path '''q'''(''t'')—the one actually taken by the system—is a path for which infinitesimal variations in that path cause no change in ''I'', at least up to first order. This principle results in the [[Euler–Lagrange equation]]s,

:<math>\frac{d}{dt} \left( \frac{\partial L}{\partial \dot{\mathbf{q}}} \right) = \frac{\partial L}{\partial \mathbf{q}}   ~.</math>

Thus, if one of the coordinates, say ''q<sub>k</sub>'', does not appear in the Lagrangian, the right-hand side of the equation is zero, and the left-hand side requires that

:<math>\frac{d}{dt} \left( \frac{\partial L}{\partial \dot{q}_k} \right) = \frac{dp_k}{dt} = 0~,</math>

where the momentum

:<math> p_k = \frac{\partial L}{\partial \dot{q}_k} </math>

is conserved throughout the motion (on the physical path).

Thus, the absence of the '''ignorable''' coordinate ''q<sub>k</sub>'' from the Lagrangian implies that the Lagrangian is unaffected by changes or transformations of ''q<sub>k</sub>''; the Lagrangian is invariant, and is said to exhibit a [[symmetry in physics|symmetry]] under such transformations. This is the seed idea generalized in Noether's theorem.

Several alternative methods for finding conserved quantities were developed in the 19th century, especially by [[William Rowan Hamilton]]. For example, he developed a theory of [[canonical transformation]]s which allowed changing coordinates so that some coordinates disappeared from the Lagrangian, as above, resulting in conserved canonical momenta. Another approach, and perhaps the most efficient for finding conserved quantities, is the [[Hamilton–Jacobi equation]].

Emmy Noether's work on the invariance theorem began in 1915 when she was helping [[Felix Klein]] and David Hilbert with their work  related to [[Albert Einstein]]'s theory of general relativity<ref name="DickNoetherBio1981">{{Cite book |last=Dick |first=Auguste |url=http://link.springer.com/10.1007/978-1-4684-0535-4 |title=Emmy Noether 1882–1935 |date=1981 |publisher=Birkhäuser Boston |isbn=978-1-4684-0537-8 |location=Boston, MA |language=en |doi=10.1007/978-1-4684-0535-4}}</ref>{{rp|31}} By March 1918 she had most of the key ideas for the paper which would be published later in the year.<ref>{{Cite book |last=Rowe |first=David E. |url=https://link.springer.com/10.1007/978-3-030-63810-8 |title=Emmy Noether – Mathematician Extraordinaire |date=2021 |publisher=Springer International Publishing |isbn=978-3-030-63809-2 |location=Cham |language=en |doi=10.1007/978-3-030-63810-8}}</ref>{{rp|81}}