Gurzadyan theorem

The formula for the force derived in [1] has the form

${\displaystyle F=-{\frac {GMm}{r^{2}}}+{\frac {\Lambda c^{2}mr}{3}},}$

where ${\displaystyle G}$ and ${\displaystyle \Lambda }$ are constants. The first term is the familiar law of universal gravitation, the second one corresponds to the cosmological constant term in general relativity and McCrea-Milne cosmology.[6] Then the field is force-free only in the center of a shell but the confinement (oscillator) term does not change the initial ${\displaystyle O(4)}$ symmetry of the Newtonian field. Also, this field corresponds to the only field possessing the property of the Newtonian one: the closing of orbits at any negative value of energy, i.e. the coincidence of the period of variation of the value of the radius vector with that of its revolution by ${\displaystyle 2\pi }$ (resonance principle) .

Einstein named the cosmological constant as a universal constant, introducing it to define the static cosmological model.[7][8]

From this theorem the cosmological constant ${\displaystyle \Lambda }$ emerges as additional constant of gravity along with the Newton’s gravitational constant ${\displaystyle G}$. Then, the cosmological constant is dimension independent and matter-uncoupled and hence can be considered even more universal than Newton’s gravitational constant.[9]

For ${\displaystyle \Lambda }$ joining the set of fundamental constants ${\displaystyle (G,c,\hbar )}$, the gravitational Newton’s constant, the speed of light and the Planck constant, yields

${\displaystyle [c]=LT^{-1},\quad [G]=M^{-1}L^{3}T^{-2},\quad [\hbar ]=ML^{2}T^{-1},\quad [\Lambda ]=L^{-2},}$

and a dimensionless quantity emerges for the 4-constant set ${\displaystyle (G,\Lambda ,c,\hbar )}$ [10]

${\displaystyle I={\frac {c^{3a}}{\Lambda ^{a}G^{a}\hbar ^{a}}},}$

where ${\displaystyle a}$ is a real number. Note, no dimensionless quantity is possible to construct from the 3 constants ${\displaystyle G,c,\hbar }$.

This within a numerical factor, ${\displaystyle a=1}$, coincides with the information (or entropy) of de Sitter event horizon [11]

${\displaystyle I_{dS}=3\pi {\frac {c^{3}}{\Lambda G\hbar }},}$

and the Bekenstein Bound [12]

${\displaystyle I_{BB}={\frac {3\pi c^{3}}{\Lambda G\hbar ln2}}.}$

This theorem, in the context of nonlocal effects in a system of gravitating particles, leads to the inhomogeneous Dirichlet boundary problem for the Poisson equation [15]

${\displaystyle \Delta \Phi ({\bf {x}})=ANG_{3}S_{3}^{2}{\bigg (}\int _{y\in [0,\infty ]}\exp {\big (}-y^{2}/(2\theta ){\big )}y^{2}dy{\bigg )}\cdot \exp(-\Phi /\theta )-{\frac {c^{2}\Lambda }{2}},}$

where ${\displaystyle R_{\Omega }}$ is the radius of the region, ${\displaystyle A,\theta ,R_{\Omega }\in {\mathbb {R} }^{1}}$. Its solution can be expressed in terms of the double layer potential, which leads to an inhomogeneous nonlinear Hammerstein integral equation for the gravitational potential ${\displaystyle U({\bf {x}})={\widetilde {\lambda }}{\widehat {\mathfrak {G}}}({U})+\alpha (\theta ,\Lambda ){\bf {x}}^{2},~~{\widehat {\mathfrak {G}}}({U})\equiv \int _{\Omega '}{\mathcal {K}}(|{\bf {x}}-{\bf {x}}'|)\exp {\big (}-{U}({\bf {x}}'){\big )}d{{\bf {x}}'},}$

${\displaystyle U({\bf {x}})\equiv (\Phi ({\bf {x}})-C_{0})/\theta ,~~{\widetilde {\lambda }}\equiv {\widetilde {\lambda _{II}}}(\theta )\equiv {\frac {\lambda _{I}}{\theta }}\exp(-C_{0}/\theta ),~~\alpha (\theta ,\Lambda )=-{\frac {\Lambda c^{2}}{12\theta }}.}$

This leads to a linear inhomogeneous 2nd kind Fredholm equation

${\displaystyle \phi ({\bf {x}})=\lambda ^{(0)}\int _{\Omega '}{\mathcal {K}}(|{\bf {x}}-{\bf {x}}'|)\phi ({\bf {x}}')d{\bf {x}}'+{\widehat {\beta }}({\bf {x}}),}$

${\displaystyle {\widehat {\beta }}({\bf {x}})\equiv -\lambda ^{(0)}\int _{\Omega '}{\mathcal {K}}(|{\bf {x}}-{\bf {x}}'|)\alpha |{\bf {x}}'|^{2}d{\bf {x}}'-\alpha |{\bf {x}}|^{2},}$

${\displaystyle {U}({\bf {x}})={U}_{0}-\phi ({\bf {x}}),~~|{\phi }|\ll {U}_{0};~~~\lambda ^{(0)}\equiv -{\widetilde {\lambda }}\exp(-U_{0}).}$

Its solution can be expressed in terms of the resolvent ${\displaystyle \Gamma }$ of the integral kernel and the non-linear (repulsive) term ${\displaystyle \phi ({\bf {x}})=-{\widehat {\beta }}({\bf {x}})+\lambda ^{(0)}\sum _{\bf {n}}\langle -{\widehat {\beta }}({\bf {x}}),\phi _{\bf {n}}\rangle \phi _{\bf {n}}\lambda _{\bf {n}}^{-1}+(\lambda ^{(0)})^{2}\sum _{\bf {n}}\langle -{\widehat {\beta }}({\bf {x}}),\phi _{\bf {n}}\rangle \phi _{\bf {n}}\lambda _{\bf {n}}^{-1}(\lambda _{\bf {n}}-\lambda ^{(0)})^{-1}=}$

${\displaystyle -{\widehat {\beta }}({\bf {x}})+\lambda ^{(0)}\int _{\Omega }\underbrace {{\bigg (}{\mathcal {K}}({\bf {x}},{\bf {x}}')+\lambda ^{(0)}\sum _{\bf {n}}\phi _{\bf {n}}({\bf {x}})\phi _{\bf {n}}({\bf {x}}')\lambda _{\bf {n}}^{-1}(\lambda _{\bf {n}}-\lambda ^{(0)})^{-1}{\bigg )}} _{\Gamma ({\bf {x}},{\bf {x}}',\lambda ^{(0)})}(-{\widehat {\beta }}({\bf {x}}))d{\bf {x}}'.}$

The dynamics of groups and clusters of galaxies are claimed to fit the theorem,[9][16] see also.[17] The possibility of two Hubble flows, a local one, determined by that formula, and a global one, described by Friedmannian cosmological equations was stated in.[18]