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General Relativity and Relativistic Cosmology | SpringerLink

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General Relativity and Relativistic Cosmology

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  • First Online:
A Mathematical Journey to Relativity

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Abstract

An imaginary discussion between Newton and Einstein could be the following. Isaac Newton:  Dear Prof. Einstein, my Universe is very simple. I can describe it using vectors and calculus. Between any two objects, a gravitational force is acting and, according to the masses of objects and the distance between them, the gravitational force law is \(F=G\dfrac{mM}{r^2}\). The gravitational field, in this case, is \(A=\dfrac{GM}{r^2}\). However, there exists an artifact, the gravitational potential \(\varPhi =\dfrac{GM}{r}\). After me, the brilliant experimental physicist, Henry Cavendish, measured the gravitational constant \(G = 6,67\times 10^{-11} \textrm{N m}^2/\textrm{kg}^2\), considered “universal”. The potential is related to the gravitational field through the formula \(\triangledown \varPhi =-{\mathop {A}\limits ^{\rightarrow }}\), the vacuum field equation is \(\triangledown ^2\varPhi =0\), as established by Pierre Simon Laplace, and the general gravitational field equation is \(\triangledown ^2\varPhi =4\pi G \rho \) as pointed out by Siméon Denis Poisson, once the density of matter is known. The objects are moving in this gravitational field according to \({\mathop {F}\limits ^{\rightarrow }}=m{\mathop {A}\limits ^{\rightarrow }}\) and the trajectories are conics because my gravitational universal law gives a mathematical proof for the Kepler laws. What do you think?

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Notes

  1. 1.

    This request is an important property that any physical solution has to possess. In fact, very far from the source, a gravitational field has to go to zero. This means that Minkowski space-time has to be recovered. This property is called “asymptotic flatness” and characterizes any physical gravitational field. It is worth noticing that this feature is fundamental for black hole solutions having physical meaning.

  2. 2.

    From observational surveys, the Universe can be considered homogeneous and isotropic beyond scales of the order 100–120 Megaparsecs. See [159] for details. This means that, over these scales, no large-scale structure, like clusters or super-clusters of galaxies are detected. According to these data, matter density can be considered homogeneously distributed in all directions.

  3. 3.

    Actually the recombination of hydrogen happened at a redshift \(z=1089\) corresponding to a period of \(3.79\times 10^5\) years after Big Bang. Here the redshift correspond to the above \(a_{today}/a_{ionized}\). See [198].

  4. 4.

    \(H_0\) is assumed constant because \(\rho _0\) is constant.

  5. 5.

    It is important to note that any form of standard matter, in the interval \(0\le w\le 1\), gives rise to decelerated expansion.

  6. 6.

    It is interesting saying that the paper reporting these results was the first one written by Enrico Fermi when he was student at Scuola Normale Superiore di Pisa [101].

  7. 7.

    The story of this solution is very nice. Kurt Gödel gave it to Albert Einstein as a gift for his 70th birthday when they both lived in Princeton.

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Correspondence to Wladimir-Georges Boskoff .

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Boskoff, WG., Capozziello, S. (2024). General Relativity and Relativistic Cosmology. In: A Mathematical Journey to Relativity. UNITEXT for Physics. Springer, Cham. https://doi.org/10.1007/978-3-031-54823-9_10

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