Creating a black hole with any mass?

Nickj800
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If you can some how accelerate any starting mass closer and closer to the speed of light, can the mass become so great that it will form a black hole?
 
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No, it's the rest mass that counts. And the rest mass of an object is always the same, no matter how fast its going.
 
Nickj800 said:
If you can some how accelerate any starting mass closer and closer to the speed of light, can the mass become so great that it will form a black hole?
See this entry from the Usenet Physics FAQ. Also some posts from pervect on the gravitational field from an object moving relative to the observer [post=1630186]here[/post], [post=1168136]here[/post], and [post=689706]here[/post].
 
Pervect's discussion starts off by saying that a moving object increases in mass and flattens out. He then goes on to talk about 'transverse mass' and 'longitudinal mass'. Well. Forgive me for saying so, but the concept of relativistic mass is outmoded and misguided, and it is startling to encounter it. It is precisely what leads to the confusion between formalism and physical reality illustrated by this current question.

It's a simple exercise to apply a Lorentz transformation to the Schwarzschild solution, and an even simpler one to realize that nothing unusual happens.
 
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...

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