| _version_ | 1866901203038765056 |
|---|---|
| author | Boudjerada, Mustafa |
| author_facet | Boudjerada, Mustafa |
| contents | <p>This sixth paper in the MonoField series develops the covariant gravitational sector of the theory, starting from a single classical Skyrme-type field (\Phi:\mathbb{R}^{3,1}\to S^3). By systematically coarse-graining over fast “ripple” modes, the slow “calm” mode (\tau) acquires a field-dependent kinetic term (f(\tau)=1+\beta\tau^2) with (\beta=c_{\rm grav}(\lambda m^2/F^2)). We then construct the simplest scalar–tensor effective action consistent with this structure and derive the relativistic field equations for static, spherically symmetric stars. In the Newtonian limit these equations reduce exactly to the nonlinear Poisson equation obtained in Paper V, providing a self-consistent bridge between the microscopic MonoField dynamics and macroscopic gravity.</p> <p>Mathematically, we prove a self-screening theorem: the effective gravitational charge of any matter distribution decreases linearly with (\beta), with an explicit onset rate. Numerically, we solve the corrected TOV system with a calibrated polytropic EOS and compute mass–radius curves, self-screening factors, and tidal deformabilities for neutron stars, verifying that General Relativity is recovered at (\beta=0) and that current GW170817 constraints still allow (\beta\sim \mathcal{O}(1\text{–}10)). The paper also outlines how a single “master” parameter (\beta_0=\lambda m^2/F^2) could correlate gravitational, decoherence, and electromagnetic tests in future work.</p> |
| format | Recurso digital |
| id | zenodo_https___doi_org_10_5281_zenodo_17677735 |
| institution | Zenodo |
| language | |
| publishDate | 2025 |
| publisher | Zenodo |
| record_format | zenodo |
| spellingShingle | MonoField Theory VI Covariant Scalar-Tensor Formulation and Self-Screening Boudjerada, Mustafa <p>This sixth paper in the MonoField series develops the covariant gravitational sector of the theory, starting from a single classical Skyrme-type field (\Phi:\mathbb{R}^{3,1}\to S^3). By systematically coarse-graining over fast “ripple” modes, the slow “calm” mode (\tau) acquires a field-dependent kinetic term (f(\tau)=1+\beta\tau^2) with (\beta=c_{\rm grav}(\lambda m^2/F^2)). We then construct the simplest scalar–tensor effective action consistent with this structure and derive the relativistic field equations for static, spherically symmetric stars. In the Newtonian limit these equations reduce exactly to the nonlinear Poisson equation obtained in Paper V, providing a self-consistent bridge between the microscopic MonoField dynamics and macroscopic gravity.</p> <p>Mathematically, we prove a self-screening theorem: the effective gravitational charge of any matter distribution decreases linearly with (\beta), with an explicit onset rate. Numerically, we solve the corrected TOV system with a calibrated polytropic EOS and compute mass–radius curves, self-screening factors, and tidal deformabilities for neutron stars, verifying that General Relativity is recovered at (\beta=0) and that current GW170817 constraints still allow (\beta\sim \mathcal{O}(1\text{–}10)). The paper also outlines how a single “master” parameter (\beta_0=\lambda m^2/F^2) could correlate gravitational, decoherence, and electromagnetic tests in future work.</p> |
| title | MonoField Theory VI Covariant Scalar-Tensor Formulation and Self-Screening |
| url | https://doi.org/10.5281/zenodo.17677735 |