Ostrogradsky instability: Difference between revisions

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In applied mathematics, the '''Ostrogradsky instability''' is a consequence of a theorem of [[Mikhail Ostrogradsky]] in [[classical mechanics]] according to which a non-degenerate [[Lagrangian mechanics|Lagrangian]] dependent on time derivatives higher than the first corresponds to a linearly unstable [[Hamiltonian mechanics#Mathematical formalism|Hamiltonian]] associated with the Lagrangian via a [[Legendre transformation#Hamilton-Lagrange mechanics|Legendre transform]]. The Ostrogradsky instability has been proposed as an explanation as to why no differential equations of higher order than two appear to describe physical phenomena.<ref>{{ cite arxiv |author= Hayato Motohashi, Teruaki Suyama |year=2014|title= Third-order equations of motion and the Ostrogradsky instability |arxiv=1411.3721}}</ref>
In applied mathematics, the '''Ostrogradsky instability''' is a consequence of a theorem of [[Mikhail Ostrogradsky]] in [[classical mechanics]] according to which a non-degenerate [[Lagrangian mechanics|Lagrangian]] dependent on time derivatives higher than the first corresponds to a linearly unstable [[Hamiltonian mechanics#Mathematical formalism|Hamiltonian]] associated with the Lagrangian via a [[Legendre transformation#Hamilton-Lagrange mechanics|Legendre transform]]. The Ostrogradsky instability has been proposed as an explanation as to why no differential equations of higher order than two appear to describe physical phenomena.<ref>{{Cite journal|author= Hayato Motohashi, Teruaki Suyama |title= Third-order equations of motion and the Ostrogradsky instability |journal=Physical Review D|volume=91|issue=8|arxiv=1411.3721|doi=10.1103/PhysRevD.91.085009|year=2015}}</ref>


==Outline of proof <ref>{{ cite arxiv |author= R. P. Woodard |year=2006 |title= Avoiding Dark Energy with 1/R Modifications of Gravity |arxiv=astro-ph/0601672}}</ref>==
==Outline of proof <ref>{{Cite journal|author= R. P. Woodard |title=The Invisible Universe: Dark Matter and Dark Energy |journal=Lect.notes Phys |volume=720 |pages=403–433 |arxiv=astro-ph/0601672|doi=10.1007/978-3-540-71013-4_14 |chapter=Avoiding Dark Energy with 1/R Modifications of Gravity |series=Lecture Notes in Physics |isbn=978-3-540-71012-7 |year=2007 }}</ref>==


The main points of the proof can be made clearer by considering a one-dimensional system with a Lagrangian <math>L(q,{\dot q}, {\ddot q})</math>. The [[Euler-Lagrange equation]] is
The main points of the proof can be made clearer by considering a one-dimensional system with a Lagrangian <math>L(q,{\dot q}, {\ddot q})</math>. The [[Euler-Lagrange equation]] is

Revision as of 04:12, 2 August 2018

In applied mathematics, the Ostrogradsky instability is a consequence of a theorem of Mikhail Ostrogradsky in classical mechanics according to which a non-degenerate Lagrangian dependent on time derivatives higher than the first corresponds to a linearly unstable Hamiltonian associated with the Lagrangian via a Legendre transform. The Ostrogradsky instability has been proposed as an explanation as to why no differential equations of higher order than two appear to describe physical phenomena.[1]

Outline of proof [2]

The main points of the proof can be made clearer by considering a one-dimensional system with a Lagrangian . The Euler-Lagrange equation is

Non-degeneracy of means that the canonical coordinates can be expressed in terms of the derivatives of and vice versa. Thus, is a function of (if it was not, the Jacobian would vanish, which would mean that is degenerate), meaning that we can write or, inverting, . Since the evolution of depends upon four initial parameters, this means that there are four canonical coordinates. We can write those as

and by using the definition of the conjugate momentum,

Due to non-degeneracy, we can write as . Note that only three arguments are needed since the Lagrangian itself only has three free parameters. By Legendre transforming, we find the Hamiltonian to be

We now notice that the Hamiltonian is linear in . This is Ostrogradsky's instability, and it stems from the fact that the Lagrangian depends on fewer coordinates than there are canonical coordinates (which correspond to the initial parameters needed to specify the problem). The extension to higher dimensional systems is analogous, and the extension to higher derivatives simply means that the phase space is of even higher dimension than the configuration space, which exacerbates the instability (since the Hamiltonian is linear in even more canonical coordinates).

Notes

  1. ^ Hayato Motohashi, Teruaki Suyama (2015). "Third-order equations of motion and the Ostrogradsky instability". Physical Review D. 91 (8). arXiv:1411.3721. doi:10.1103/PhysRevD.91.085009.
  2. ^ R. P. Woodard (2007). "The Invisible Universe: Dark Matter and Dark Energy". Lect.notes Phys. Lecture Notes in Physics. 720: 403–433. arXiv:astro-ph/0601672. doi:10.1007/978-3-540-71013-4_14. ISBN 978-3-540-71012-7. {{cite journal}}: |chapter= ignored (help)