We know of two very extreme classes of stars out there, plenty of them have been observed and all point to exotic matter, even the mass ranges that the stars inhabit match our theories... so the evidence fits pretty well
These are White dwarfs, and neutron stars
Both of these classes of objects are held up by degeneracy pressure. White dwarfs are held up by electron degeneracy and Chandrasekhar postulated that the maximum mass of a stellar remnant that is electron degenerate is 1.39 Solar masses.
http://en.wikipedia.org/wiki/Chandrasekhar_limit
Now what happens we we pass that limit? well then we delve into neutron degeneracy and neutron stars... the limit of this is analogous to the Chandrasekhar limit. It is known as the Tolman–Oppenheimer–Volkoff limit, and represents matter that has been squeezed so much that the electron orbitals are close to or within the nucleus itself, and the protons begin to interact with the electrons and convert into neutrons via inverse beta decay. The limit is about 3 solar masses.
http://en.wikipedia.org/wiki/Tolman–Oppenheimer–Volkoff_limit
So we have models for these two classes of extreme object, and indeed we do not see any white dwarfs bigger than this 1.4 Solar Mass limit, nor neutron stars greater than 3 solar masses. So our understanding of quantum mechanics and Atomic physics appears validated. So what happens when you go further than 3 solar masses in a compressed space? Well we don't really know. BUT what we do know is that for the density of the objects in excess of 3 solar masses, that are neutron degenerate, the solution of the now rather simple treatment of newtonian physics, setting C to the escape velocity of a massive object, and you do come close to the conditions set out above.
We also do have evidence for massive invisible/unobserved objects in the milky way, the biggest being at the centre of the milkyway. To flat out deny their existence is to sweep so much supporting evidence under the rug and simply to shake your head at a wealth of data Vladimar Rubicon...
All theories and things that do this don't appear to hold up to scrutiny in all cases and do not explain our observations.
These are White dwarfs, and neutron stars
Both of these classes of objects are held up by degeneracy pressure. White dwarfs are held up by electron degeneracy and Chandrasekhar postulated that the maximum mass of a stellar remnant that is electron degenerate is 1.39 Solar masses.
http://en.wikipedia.org/wiki/Chandrasekhar_limit
Now what happens we we pass that limit? well then we delve into neutron degeneracy and neutron stars... the limit of this is analogous to the Chandrasekhar limit. It is known as the Tolman–Oppenheimer–Volkoff limit, and represents matter that has been squeezed so much that the electron orbitals are close to or within the nucleus itself, and the protons begin to interact with the electrons and convert into neutrons via inverse beta decay. The limit is about 3 solar masses.
http://en.wikipedia.org/wiki/Tolman–Oppenheimer–Volkoff_limit
So we have models for these two classes of extreme object, and indeed we do not see any white dwarfs bigger than this 1.4 Solar Mass limit, nor neutron stars greater than 3 solar masses. So our understanding of quantum mechanics and Atomic physics appears validated. So what happens when you go further than 3 solar masses in a compressed space? Well we don't really know. BUT what we do know is that for the density of the objects in excess of 3 solar masses, that are neutron degenerate, the solution of the now rather simple treatment of newtonian physics, setting C to the escape velocity of a massive object, and you do come close to the conditions set out above.
We also do have evidence for massive invisible/unobserved objects in the milky way, the biggest being at the centre of the milkyway. To flat out deny their existence is to sweep so much supporting evidence under the rug and simply to shake your head at a wealth of data Vladimar Rubicon...
All theories and things that do this don't appear to hold up to scrutiny in all cases and do not explain our observations.