Physics:Born rigidity

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Born rigidity is a concept in special relativity. It is one answer to the question of what, in special relativity, corresponds to the rigid body of non-relativistic classical mechanics. The concept was introduced by Max Born (1909),[1][2] who gave a detailed description of the case of constant proper acceleration which he called hyperbolic motion. When subsequent authors such as Paul Ehrenfest (1909)[3] tried to incorporate rotational motions as well, it became clear that Born rigidity is a very restrictive sense of rigidity, leading to the Herglotz–Noether theorem, according to which there are severe restrictions on rotational Born rigid motions. It was formulated by Gustav Herglotz (1909, who classified all forms of rotational motions)[4] and in a less general way by Fritz Noether (1909).[5] As a result, Born (1910)[6] and others gave alternative, less restrictive definitions of rigidity.

Definition

Born rigidity is satisfied if the orthogonal spacetime distance between infinitesimally separated curves or worldlines is constant,[7] or equivalently, if the length of the rigid body in momentary co-moving inertial frames measured by standard measuring rods (i.e. the proper length) is constant and is therefore subjected to Lorentz contraction in relatively moving frames.[8] Born rigidity is a constraint on the motion of an extended body, achieved by careful application of forces to different parts of the body. A body rigid in itself would violate special relativity, as its speed of sound would be infinite.

A classification of all possible Born rigid motions can be obtained using the Herglotz–Noether theorem. This theorem states, that all irrotational Born rigid motions (class A) consist of hyperplanes rigidly moving through spacetime, while any rotational Born rigid motion (class B) must be isometric Killing motions. This implies that a Born rigid body only has three degrees of freedom. Thus a body can be brought in a Born rigid way from rest into any translational motion, but it cannot be brought in a Born rigid way from rest into rotational motion.[9]

Stresses and Born rigidity

It was shown by Herglotz (1911),[10] that a relativistic theory of elasticity can be based on the assumption, that stresses arise when the condition of Born rigidity is broken.[11]

An example of breaking Born rigidity is the Ehrenfest paradox: Even though the state of uniform circular motion of a body is among the allowed Born rigid motions of class B, a body cannot be brought from any other state of motion into uniform circular motion without breaking the condition of Born rigidity during the phase in which the body undergoes various accelerations. But if this phase is over and the centripetal acceleration becomes constant, the body can be uniformly rotating in agreement with Born rigidity. Likewise, if it is now in uniform circular motion, this state cannot be changed without again breaking the Born rigidity of the body.

Another example is Bell's spaceship paradox: If the endpoints of a body are accelerated with constant proper accelerations in rectilinear direction, then the leading endpoint must have a lower proper acceleration in order to leave the proper length constant so that Born rigidity is satisfied. It will also exhibit an increasing Lorentz contraction in an external inertial frame, that is, in the external frame the endpoints of the body are not accelerating simultaneously. However, if a different acceleration profile is chosen by which the endpoints of the body are simultaneously accelerated with same proper acceleration as seen in the external inertial frame, its Born rigidity will be broken, because constant length in the external frame implies increasing proper length in a comoving frame due to relativity of simultaneity. In this case, a fragile thread spanned between two rockets will experience stresses (which are called Herglotz–Dewan–Beran stresses[8]) and will consequently break.

Born rigid motions

A classification of allowed, in particular rotational, Born rigid motions in flat Minkowski spacetime was given by Herglotz,[4] which was also studied by Friedrich Kottler (1912, 1914),[12] Georges Lemaître (1924),[13] Adriaan Fokker (1940),[14] George Salzmann & Abraham H. Taub (1954).[7] Herglotz pointed out that a continuum is moving as a rigid body when the world lines of its points are equidistant curves in [math]\displaystyle{ \mathbf{R}^{4} }[/math]. The resulting worldliness can be split into two classes:

Class A: Irrotational motions

Herglotz defined this class in terms of equidistant curves which are the orthogonal trajectories of a family of hyperplanes, which also can be seen as solutions of a Riccati equation[15] (this was called "plane motion" by Salzmann & Taub[7] or "irrotational rigid motion" by Boyer[16][17]). He concluded, that the motion of such a body is completely determined by the motion of one of its points.

The general metric for these irrotational motions has been given by Herglotz, whose work was summarized with simplified notation by Lemaître (1924). Also the Fermi metric in the form given by Christian Møller (1952) for rigid frames with arbitrary motion of the origin was identified as the "most general metric for irrotational rigid motion in special relativity".[18] In general, it was shown that irrotational Born motion corresponds to those Fermi congruences of which any worldline can be used as baseline (homogeneous Fermi congruence).[19]

Herglotz
1909 		[math]\displaystyle{ ds^{2}=da^{2}+\varphi(db,dc)-\Theta^{2}d\vartheta^{2} }[/math][20]
Lemaître
1924 		[math]\displaystyle{ \begin{align} & ds^{2}=-dx^{2}-dy^{2}-dz^{2}+\phi^{2}dt^{2}\\ & \quad\left(\phi=lx+my+nz+p\right) \end{align} }[/math][21]
Møller
1952 		[math]\displaystyle{ ds^{2}=dx^{2}+dy^{2}+dz^{2}-c^{2}dt^{2}\left[1+\frac{g_{\kappa}x^{\kappa}}{c^{2}}\right]^{2} }[/math][22]

Already Born (1909) pointed out that a rigid body in translational motion has a maximal spatial extension depending on its acceleration, given by the relation [math]\displaystyle{ b\lt c^{2}/R }[/math], where [math]\displaystyle{ b }[/math] is the proper acceleration and [math]\displaystyle{ R }[/math] is the radius of a sphere in which the body is located, thus the higher the proper acceleration, the smaller the maximal extension of the rigid body.[2] The special case of translational motion with constant proper acceleration is known as hyperbolic motion, with the worldline

Born
1909 		[math]\displaystyle{ \begin{align} & x=-q\xi,\quad y=\eta,\quad z=\zeta,\quad t=\frac{p}{c^{2}}\xi\\ & \quad\left(p=\frac{dx}{d\tau},\quad q=-\frac{dt}{d\tau}=\sqrt{1+p^{2}/c^{2}}\right) \end{align} }[/math][23]
Herglotz
1909 		[math]\displaystyle{ x=x',\quad y=y',\quad t-z=(t'-z')e^{\vartheta},\quad t+z=(t'+z')e^{-\vartheta} }[/math][24]

[math]\displaystyle{ x=x_{0},\quad y=y_{0},\quad z=\sqrt{z_{0}^{2}+t^{2}} }[/math][25]

Sommerfeld
1910 		[math]\displaystyle{ \begin{align} & x=r\cos\varphi,\quad y=y',\quad z=z',\quad l=r\sin\varphi\\ & \quad\left(l=ict,\quad\varphi=i\psi\right) \end{align} }[/math][26]
Kottler
1912, 1914 		[math]\displaystyle{ \begin{align} & x^{(1)}=x_{0}^{(1)},\quad x^{(2)}=x_{0}^{(2)},\quad x^{(3)}=b\cos iu,\quad x^{(4)}=b\sin iu\\ & ds^2=-c^{2}d\tau^{2}=b^{2}(du)^{2} \end{align} }[/math][27]

[math]\displaystyle{ x=x_{0},\quad y=y_{0},\quad z=b\cosh u,\quad ct=b\sinh u }[/math][28]

Class B: Rotational isometric motions

For the corresponding proper reference frames for these rotational motions, see Proper reference frame (flat spacetime)

Herglotz defined this class in terms of equidistant curves which are the trajectories of a one-parameter motion group[29] (this was called "group motion" by Salzmann & Taub[7] and was identified with isometric Killing motion by Felix Pirani & Gareth Williams (1962)[30]). He pointed out that they consist of worldlines whose three curvatures are constant (known as curvature, torsion and hypertorsion), forming a helix.[31] Worldlines of constant curvatures in flat spacetime were also studied by Kottler (1912),[12] Petrův (1964),[32] John Lighton Synge (1967, who called them timelike helices in flat spacetime),[33] or Letaw (1981, who called them stationary worldlines)[34] as the solutions of the Frenet–Serret formulas.

Herglotz further separated class B using four one-parameter groups of Lorentz transformations (loxodromic, elliptic, hyperbolic, parabolic) in analogy to hyperbolic motions (i.e. isometric automorphisms of a hyperbolic space), and pointed out that Born's hyperbolic motion (which follows from the hyperbolic group with [math]\displaystyle{ \alpha=0 }[/math] in the notation of Herglotz and Kottler, [math]\displaystyle{ \lambda=0 }[/math] in the notation of Lemaître, [math]\displaystyle{ q=0 }[/math] in the notation of Synge; see the following table) is the only Born rigid motion that belongs to both classes A and B.

Loxodromic group (combination of hyperbolic motion and uniform rotation)
Herglotz
1909 		[math]\displaystyle{ x+iy=(x'+iy')e^{i\lambda\vartheta},\quad x-iy=(x'-iy')e^{-i\lambda\vartheta},\quad t-z=(t'-z')e^{\vartheta},\quad t+z=(t'+z')e^{-\vartheta} }[/math][35]
Kottler
1912, 1914 		[math]\displaystyle{ \begin{align} & x^{(1)}=a\cos\lambda\left(u-u_{0}\right),\quad x^{(2)}=a\sin\lambda\left(u-u_{0}\right),\quad x^{(3)}=b\cos iu,\quad x^{(4)}=b\sin iu\\ & ds^{2}=-c^{2}d\tau^{2}=-\left(b^{2}-a^{2}\lambda^{2}\right)(du)^{2} \end{align} }[/math][36]
Lemaître
1924 		[math]\displaystyle{ \begin{align} & \xi=x\cos\lambda t-y\sin\lambda t,\quad\eta=x\sin\lambda t+y\cos\lambda t,\quad\zeta=z\cosh t,\quad\tau=z\sinh t\\ & ds^{2}=-dr^{2}-r^{2}d\theta^{2}-dz^{2}-2\lambda r^{2}d\theta\ dt+\left(z^{2}-\lambda^{2}r^{2}\right)dt^{2} \end{align} }[/math][37]
Synge
1967 		[math]\displaystyle{ x=q\omega^{-1}\sin\omega s,\quad y=-q\omega^{-1}\cos\omega s,\quad z=r\chi^{-1}\cosh\chi s,\quad t=r\chi^{-1}\sinh\chi s }[/math][38]
Elliptic group (uniform rotation)
Herglotz
1909 		[math]\displaystyle{ x+iy=(x'+iy')e^{i\vartheta},\quad x-iy=(x'-iy')e^{-i\vartheta},\quad z=z',\quad t=t'+\delta\vartheta }[/math][39]
Kottler
1912, 1914 		[math]\displaystyle{ \begin{align} & x^{(1)}=a\cos\lambda\left(u-u_{0}\right),\quad x^{(2)}=a\sin\lambda\left(u-u_{0}\right),\quad x^{(3)}=x_{0}^{(3)},\quad x^{(4)}=iu\\ & ds^{2}=-c^{2}d\tau^{2}=-\left(1-a^{2}\lambda^{2}\right)(du)^{2} \end{align} }[/math][40]
de Sitter
1916 		[math]\displaystyle{ \begin{align} & \theta'=\theta-\omega ct,\ \left(d\sigma^{\prime2}=dr^{\prime2}+r^{\prime2}d\theta^{\prime2}+dz^{\prime2}\right)\\ & ds^{2}=-d\sigma^{\prime2}-2r^{\prime2}\omega\ d\theta'cdt+\left(1-r^{\prime2}\omega^{2}\right)c^{2}dt^{2} \end{align} }[/math][41]
Lemaître
1924 		[math]\displaystyle{ \begin{align} & \xi=x\cos\lambda t-y\sin\lambda t,\quad\eta=x\sin\lambda t+y\cos\lambda t,\quad\zeta=z,\quad\tau=t\\ & ds^{2}=-dr^{2}-r^{2}d\theta^{2}-dz^{2}-2\lambda r^{2}d\theta\ dt+\left(1-\lambda^{2}r^{2}\right)dt^{2} \end{align} }[/math][42]
Synge
1967 		[math]\displaystyle{ x=q\omega^{-1}\sin\omega s,\quad y=-q\omega^{-1}\cos\omega s,\quad z=0,\quad t=sr }[/math][43]
Hyperbolic group (hyperbolic motion plus spacelike translation)
Herglotz
1909 		[math]\displaystyle{ x=x'+\alpha\vartheta,\quad y=y',\quad t-z=(t'-z')e^{\vartheta},\quad t+z=(t'+z')e^{-\vartheta} }[/math][44]
Kottler
1912, 1914 		[math]\displaystyle{ \begin{align} & x^{(1)}=x_{0}^{(1)}+\alpha u,\quad x^{(2)}=x_{0}^{(2)},\quad x^{(3)}=b\cos iu,\quad x^{(4)}=b\sin iu\\ & ds^{2}=-c^{2}d\tau^{2}=-\left(b^{2}-\alpha^{2}\right)(du)^{2} \end{align} }[/math][45]
Lemaître
1924 		[math]\displaystyle{ \begin{align} & \xi=x+\lambda t,\quad\eta=y,\quad\zeta=z\cosh t,\quad\tau=z\sinh t\\ & ds^{2}=-dx^{2}-dy^{2}-dz^{2}-2\lambda dx\ dt+\left(z^{2}-\lambda^{2}\right)dt^{2} \end{align} }[/math][46]
Synge
1967 		[math]\displaystyle{ x=sq,\quad y=0,\quad z=r\chi^{-1}\cosh\chi s,\quad t=r\chi^{-1}\sinh\chi s }[/math][47]
Parabolic group (describing a semicubical parabola)
Herglotz
1909 		[math]\displaystyle{ x=x_{0}+\frac{1}{2}\delta\vartheta^{2},\quad y=y_{0}+\beta\vartheta,\quad z=z_{0}+x_{0}\vartheta+\frac{1}{6}\delta\vartheta^{3},\quad t-z=\delta\vartheta }[/math][25]
Kottler
1912, 1914 		[math]\displaystyle{ \begin{align} & x^{(1)}=x_{0}^{(1)}+\frac{1}{2}\alpha u^{2},\quad x^{(2)}=x_{0}^{(2)},\quad x^{(3)}=x_{0}^{(3)}+x_{0}^{(1)}u+\frac{1}{6}\alpha u^{3},\quad x^{(4)}=ix^{(3)}+i\alpha u\\ & ds^{2}=-c^{2}d\tau^{2}=-\left(\alpha^{2}+2x_{0}^{(1)}\right)(du)^{2} \end{align} }[/math][48]
Lemaître
1924 		[math]\displaystyle{ \begin{align} & \xi=x+\frac{1}{2}\lambda t^{2},\quad\eta=y+\mu t,\quad\zeta=z+xt+\frac{1}{6}\lambda t^{3},\quad\tau=\lambda t+z+xt+\frac{1}{6}\lambda t^{3}\\ & ds^{2}=-dx^{2}-dy^{2}-2\mu\ dy\ dt+2\lambda\ dz\ dt+\left(2\lambda x+\lambda^{2}-\mu^{2}\right)dt^{2} \end{align} }[/math][37]
Synge
1967 		[math]\displaystyle{ x=\frac{1}{6}b^{2}s^{3},\quad y=0,\quad z=\frac{1}{2}bs^{2},\quad t=s+\frac{1}{6}b^{2}s^{3} }[/math][49]

General relativity

Attempts to extend the concept of Born rigidity to general relativity have been made by Salzmann & Taub (1954),[7] C. Beresford Rayner (1959),[50] Pirani & Williams (1962),[30] Robert H. Boyer (1964).[16] It was shown that the Herglotz–Noether theorem is not completely satisfied, because rigid rotating frames or congruences are possible which do not represent isometric Killing motions.[30]

Alternatives

Several weaker substitutes have also been proposed as rigidity conditions, such as by Noether (1909)[5] or Born (1910) himself.[6]

A modern alternative was given by Epp, Mann & McGrath.[51] In contrast to the ordinary Born rigid congruence consisting of the "history of a spatial volume-filling set of points", they recover the six degrees of freedom of classical mechanics by using a quasilocal rigid frame by defining a congruence in terms of the "history of the set of points on the surface bounding a spatial volume".

References

  1. ↑ Born (1909a)
  2. ↑ 2.0 2.1 Born (1909b)
  3. ↑ Ehrenfest (1909)
  4. ↑ 4.0 4.1 Herglotz (1909)
  5. ↑ 5.0 5.1 Noether (1909)
  6. ↑ 6.0 6.1 Born (1910)
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Salzmann & Taub (1954)
  8. ↑ 8.0 8.1 Gron (1981)
  9. ↑ Giulini (2008)
  10. ↑ Herglotz (1911)
  11. ↑ Pauli (1921)
  12. ↑ 12.0 12.1 Kottler (1912); Kottler (1914a)
  13. ↑ Lemaître (1924)
  14. ↑ Fokker (1940)
  15. ↑ Herglotz (1909), pp. 401, 415
  16. ↑ 16.0 16.1 Boyer (1965)
  17. ↑ Giulini (2008), Theorem 18
  18. ↑ Boyer (1965), p. 354
  19. ↑ Bel (1995), theorem 2
  20. ↑ Herglotz (1909), p. 401
  21. ↑ Lemaître (1924), p. 166, 170
  22. ↑ (1952), p. 254
  23. ↑ Born (1909), p. 25
  24. ↑ Herglotz (1909), p. 408
  25. ↑ 25.0 25.1 Herglotz (1909), p. 414
  26. ↑ Sommerfled (1910), p. 670
  27. ↑ Kottler (1912), p. 1714; Kottler (1914a), table 1, case IIIb
  28. ↑ Kottler (1914b), p. 488
  29. ↑ Herglotz (1909), pp. 402, 409-415
  30. ↑ 30.0 30.1 30.2 Pirani & Willims (1962)
  31. ↑ Herglotz (1909), p. 403
  32. ↑ Petrův (1964)
  33. ↑ Synge (1967)
  34. ↑ Letaw (1981)
  35. ↑ Herglotz (1909), p. 411
  36. ↑ Kottler (1912), p. 1714; Kottler (1914a), table 1, case I
  37. ↑ 37.0 37.1 Lemaître (1924), p. 175
  38. ↑ Synge (1967), Type I
  39. ↑ Herglotz (1909), p. 412
  40. ↑ Kottler (1912), p. 1714; Kottler (1914a), table 1, case IIb
  41. ↑ DeSitter (1916), p. 178
  42. ↑ Lemaître (1924), p. 173
  43. ↑ Synge (1967), Type IIc
  44. ↑ Herglotz (1909), p. 413
  45. ↑ Kottler (1912), p. 1714; Kottler (1914a), table 1, case IIIa
  46. ↑ Lemaître (1924), p. 174
  47. ↑ Synge (1967), Type IIa
  48. ↑ Kottler (1912), p. 1714; Kottler (1914a), table 1, case IV
  49. ↑ Synge (1967), Type IIb
  50. ↑ Rayner (1959)
  51. ↑ Epp, Mann & McGrath (2009)

Bibliography

In English: Pauli, W. (1981). Theory of Relativity. 165. Dover Publications. ISBN 0-486-64152-X. 

External links



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