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数日後にはここに重力メッセージが表示されるので、皆さんは待つ必要があります

Four weeks have passed, thank you all for your understanding and anticipation.

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1895. The year of Lorentz’s “Three Possible Explanations for this Relative Contraction,” the year when it should have been understood that space can be deformed along selected (orthogonal) axes. Moreover, this deformation can be positive (a reduction in the longitudinal dimension with the addition of energy) or negative (an increase in the transverse dimensions of a massive body with the reduction of its mass energy). But this understanding never emerged. 1905. The year of Einstein’s Special Theory of Relativity. In fact, this was a theory of only positive deformation of the longitudinal dimension of a material body; negative deformation of the transverse dimensions was not considered. Is this theory acceptable for 2026, and if not, what’s wrong with it? It doesn’t answer the question of the deformation of longitudinal space before and after a material
body (let’s assume the size of such a material body – a nucleon, meson, or electron – is equal to its Compton length). It also fails to recognize the existence of a specific (less than infinity) limit on the Lorentz factor (the limit of the compression of a specific material body under specific conditions). Simply speaking, reaching the stars with Vimanas Nextday has became more difficult in the future. 1908. The year of Spacetime by Minkowski for the Special Theory of Relativity, in which reaching the stars with Vimanas Nextday became virtually impossible. Why? It’s all about the fourth coordinate, which became complex x_4=ict. Another question: was there a chance to restore the real numbers to the time (fourth) coordinate, and if so, who could have done it? Objectively speaking, getting rid of Minkowski’s Spacetime, integrated into Einstein’s Special Theory of Relativity and later into Einstein’s General Theory of Relativity, at least until 1955, was only possible for Einstein himself. 1917. The year of Einstein’s Static Model of the Universe (Cosmological Betrachtungen zur allgemien Relativistatstheorie, Sitzungsber). In this article, calculating the volume of the Universe using the third power of the complex fourth coordinate (and a real number coefficient) could not possibly yield a real number result for the volume of the Universe. This should have created grounds for doubting the complexity of the time coordinate, but it did not do so, neither then, nor before 1955, nor now. 1915. The year of Einstein’s General Theory of Relativity, the year when Einstein first developed the gravitational constant

   

With physical dimensions of m/kg, this constant can be written as

   

allowing Newton’s Law of Universal Gravitation to be written as

   

From this formula, its easy to see that if body M is at rest and body m is moving, the magnitude of their interaction increases proportionally to the increase in the energy of body m and the relativistic decrease in the distance R between them. That is, the combined magnitude of their interaction should be proportional to the Lorentz factor to the third power. This is precisely the relationship (the “longitudinal mass” from the Special Theory of Relativity) that is observed experimentally. And it is precisely this formula (which is not found in textbooks) that could begin to contribute to the understanding that the magnitude of the decrease in gravitational interaction is independent of the spatial dimension. 1916. The year of Schwarzschild’s “Exact Solution in General Relativity,” the year of the beginning of what are now called Black Holes. 1922. The year
of Stern-Gerlach’s “Quantum Spin,” the year of the beginning of what would later correct the Special Theory of Relativity, the General Theory of Relativity, and, among other things, answer the question of the origin of Dark Energy and Dark Matter. 1922. The year of Friedman’s “Nonstatic Model of the Universe.” The year of the beginning of the modern science of cosmology, in the work “Ober die Krümmung des Raumes,” which Lemaître only became familiar with in 1927. Based on Einstein’s 1917 work, Friedman derived two equations for the Nonstatic Model of the Universe. It is these equations, developed by Friedman himself, and not later versions by third-party authors, that form the foundation of modern cosmology.

   

   

These equations contain first and second derivatives of the radius of curvature of the Universe, that is, the velocity and acceleration. Logically, there are two variants of the first derivative being equal to zero (the Einstein and de Sitter worlds): one in which the the first derivative is not equal to zero and the second derivative is equal to zero, the first derivative is not equal to zero and the second derivative is not equal to zero. The mathematician’s desire to immediately obtain a general solution (the first derivative is not equal to zero and the second derivative is not equal to zero) led to a simple physical solution (which you can find yourself) for the variation of the first derivative being not equal to zero and the second derivative being equal to zero being ignored. I’ll discuss the consequences of this for cosmology later. Now you will be interested to know that the backstory of The Mirror-Mirror-Universe Theory began precisely from this work, 1922.

And by the way, just for fun, but seriously. The cosmological constant for Einstein’s universe is 1c^2/R^2, while the cosmological constant for the de Sitter universe is 3c^2/R^2. Did Friedman consider the existence of a solution with a cosmological constant for the universe equal to 2c^2/R^2? Most likely not, because this is an undiscovered solution for the universe. The inequality of the first derivative to zero and the equality of the second derivative – the universe Melia 2011