Infinite Curvature: Understanding Black Holes

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What does it mean for something to have an infinite curvature (like a black hole?)?
 
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Black holes do not necessarily have to have infinite curvature, but enough mass to prevent light from escaping its gravitational pull. Infinite curvature would require an infinitely massive object; it's only a theoretical idea and is probably not possible. Einstein didn't believe that space time could rip, but only bend.

If it could exist, it would mean that the space-time continuum was bent to infinity. In case you don't know, the space time continuum can be thought of as a soft surface (such as a mattress), that curves when a mass is on it, and that gives us the impression of gravitational acceleration. It’s a pretty “sketchy” way of thinking about it, but it works.
 
I checked for the definition of curvature, thinking I could come up with a good answer. I found many definitions of curvature! So I am leaving this one alone
 
In GR, curvature referes to one of several "curvatuare tensors". The most fundamental of these is the Riemann curvature tensor - if you know the values of the components of the Riemann curvature tensor, you can calculate the values of the other tensors (most notably the Ricci, Einstein, and perhaps the Weyl).

A tensor is not just a single number, but an "array" of related numbers.

"Infinite" means that the value of at least one of the components of said tensor (remember, a tensor is not just a single number) increases without bound as one approaches a point, such as the singularity of a black hole. This is usually taken to imply that the theory itself breaks down and is not valid at that singular point.

Unfortunatly, there isn't any really super-simple way to describe what the Riemann curvature measures, though this is discussed in, for instance:

http://math.ucr.edu/home/baez/gr/outline2.html
http://math.ucr.edu/home/baez/einstein/node9.html
 
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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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