| black hole predicament Pauli Exclusion Principle does not allow the formation of black holes. Yet news about them keeps popping up in Scientific American, Discover, Astronomy, Sky and Telescope, and many other science news magazines. A large volume of research papers have titles containing the word ‘black hole’. However, observationally, only strong evidence suggested their existence, mainly in binary stars systems and intense x-ray sources. Do they really exist? One will never know unless one gets close to it. As much as the desire to come in contact with it, theorists already set a point of no return as the ‘event horizon’. This control volume is at a Schwarzschild radius off the center. Once the approach is less it is supposedly downhill all the way. Now, this also seems analogous to free fall and Einstein’s principle of equivalence says that the falling body should feel weightless or the same as no force of attraction. Again, this contradicts Newton’s 3rd law if there is no action there cannot be any reaction. So where does the body really go? More embarrassing is the fact that general relativity is based on the idea of mass derived from neutral atoms. However, matter at the singular level of elementary particles possesses not only electric charge but color charge as well. Neutron stars are supposedly made of neutrons and they are steps closer to becoming black holes. Nevertheless, at smaller distances, neutrons are made from quarks having both electric and color charge. Fortunately, there are three elementary particles belonging to the lepton families that are all neutral (no electric nor color charge) and their existence verified by high energy experiments with the exception that theory says they don’t congregate at low temperature. But at extremely high temperature they should but there is no theory to describe it. These are the electron neutrinos, the muon neutrinos, and the tau neutrinos. The problem is that nobody really knows how much they weigh?
__________________ Time independence: [∂E(g)]²=[∂F(a)×∂r(a)]·[∂F(b)×∂r(b)] and Mass independence: ¶a(t)·¶r(t)=c² |