Rigid body angular velocity limit

bob900
Messages
40
Reaction score
0
Suppose a rigid body (say a sphere) ofis rotating with angular velocity A. Any point at a distance r from the axis of rotation has tangential velocity v=A*r and that v must be less than c. Does this mean that :

1. The rigid body can only be a certain maximum (radial) size r, where r<A/c?
2. If you try to increase its angular velocity, it will no longer stay rigid?
 
Physics news on Phys.org
The speed of sound in an ideal rigid body would be infinite, which is not compatible with relativity, which limits the speed of sound to something less than 'c'.

For any sort of normal matter, (say steel, or even buckytubes, the strongest material known) the speed of sound is much less than c You'd also find that you couldn't build anything strong enough to even approach a tangential velocity of 'c' with available materials.

You can create a notion of rigidity that is compatible with special relativity called "Born Rigidity", however it turns out that you can't make something that's Born rigid rotate at all while still satisfying the defining conditions.

See for instance http://math.ucr.edu/home/baez/physics/Relativity/SR/rigid_disk.html and the references therin,
 
In Philippe G. Ciarlet's book 'An introduction to differential geometry', He gives the integrability conditions of the differential equations like this: $$ \partial_{i} F_{lj}=L^p_{ij} F_{lp},\,\,\,F_{ij}(x_0)=F^0_{ij}. $$ The integrability conditions for the existence of a global solution ##F_{lj}## is: $$ R^i_{jkl}\equiv\partial_k L^i_{jl}-\partial_l L^i_{jk}+L^h_{jl} L^i_{hk}-L^h_{jk} L^i_{hl}=0 $$ Then from the equation: $$\nabla_b e_a= \Gamma^c_{ab} e_c$$ Using cartesian basis ## e_I...
Thread 'Dirac's integral for the energy-momentum of the gravitational field'
See Dirac's brief treatment of the energy-momentum pseudo-tensor in the attached picture. Dirac is presumably integrating eq. (31.2) over the 4D "hypercylinder" defined by ##T_1 \le x^0 \le T_2## and ##\mathbf{|x|} \le R##, where ##R## is sufficiently large to include all the matter-energy fields in the system. Then \begin{align} 0 &= \int_V \left[ ({t_\mu}^\nu + T_\mu^\nu)\sqrt{-g}\, \right]_{,\nu} d^4 x = \int_{\partial V} ({t_\mu}^\nu + T_\mu^\nu)\sqrt{-g} \, dS_\nu \nonumber\\ &= \left(...
Abstract The gravitational-wave signal GW250114 was observed by the two LIGO detectors with a network matched-filter signal-to-noise ratio of 80. The signal was emitted by the coalescence of two black holes with near-equal masses ## m_1=33.6_{-0.8}^{+1.2} M_{⊙} ## and ## m_2=32.2_{-1. 3}^{+0.8} M_{⊙}##, and small spins ##\chi_{1,2}\leq 0.26 ## (90% credibility) and negligible eccentricity ##e⁢\leq 0.03.## Postmerger data excluding the peak region are consistent with the dominant quadrupolar...
Back
Top