The evolution of the Earth-Moon system based on the dark matter field fluid model

Hongjun Pan

Home/Archive/arXiv

arXiv · 0704.0003

The evolution of the Earth-Moon system based on the dark matter field fluid model

Hongjun Pan

View original source ↗Read source document ↗Export metadata ↓

Abstract

The evolution of Earth-Moon system is described by the dark matter field fluid model proposed in the Meeting of Division of Particle and Field 2004, American Physical Society. The current behavior of the Earth-Moon system agrees with this model very well and the general pattern of the evolution of the Moon-Earth system described by this model agrees with geological and fossil evidence. The closest distance of the Moon to Earth was about 259000 km at 4.5 billion years ago, which is far beyond the Roche's limit. The result suggests that the tidal friction may not be the primary cause for the evolution of the Earth-Moon system. The average dark matter field fluid constant derived from Earth-Moon system data is 4.39 x 10^(-22) s^(-1)m^(-1). This model predicts that the Mars's rotation is also slowing with the angular acceleration rate about -4.38 x 10^(-22) rad s^(-2).

Explore related subjects

physics.gen-ph

Keep this discovery

Explore connections, maps & timelines

BibTeX RIS

Hongjun Pan. 2008-01-13. The evolution of the Earth-Moon system based on the dark matter field fluid model. https://arxiv.org/abs/0704.0003

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Constraints on redshift-evolving Hubble constant models with early- and late-time diagnostics

We systematically investigate four cosmological models within a parameterized framework that allows for a redshift dependence of $H_0$: three phenomenological models ($αΛ$CDM, $αw$CDM, and $αw_0w_a$CDM), and the $J$CDM model motivated by big bang quantum cosmology. Using cosmic microwave background (CMB) data, baryon acoustic oscillations (BAO), cosmic chronometer (CC) measurements of the Hubble parameter, and three Type Ia supernova samples (PantheonPlus, DESY5, and Union3), we perform Markov chain Monte Carlo (MCMC) analyses to obtain posterior distributions of the model parameters. We also perform separate analyses using early-time and late-time data to assess how each observational epoch affects the model constraints. For the three phenomenological models, the parameter $α$ describing the redshift evolution of $H_0$ is consistent with zero within $2σ$. The Hubble constant inferred from the $αΛ$CDM model is consistent with CMB results, while the $J$CDM model yields a larger Hubble constant but is strongly disfavored by model comparison criteria. Using the Akaike Information Criterion (AIC) and the Bayesian Information Criterion (BIC) for model comparison, we find that the standard $Λ$CDM model remains the most favored by the data. Among the four models, the $αw_0w_a$CDM model shows a marginal AIC advantage ($\rm ΔAIC \sim$ -2 to -13). However, this preference does not translate into a reduction of the Hubble tension, which is consistent with existing studies supporting dynamical dark energy. Moreover, none of the models can simultaneously satisfy both the early- and late-time constraints, and the combined datasets alone are insufficient to conclusively determine whether these parametrizations can resolve the tension.

physics.gen-ph↗

arXiv2026

Descartes Curvature Geometry, Compact-Cycle Amplitudes, and the GST Cabibbo Seed

Several apparently distinct formulations of the charged-lepton mass relation $p_2/e_1^2 = 2/3$ share a common algebraic object: the ratio of flavor-breaking to flavor-symmetric amplitude components on an internal family space. We show that (i) the relation expressed as a Fourier-mode constraint on Shulga's compact cycle, (ii) the same relation as a Descartes curvature condition in the sense of Kocik, and (iii) the Soddy completion of the resulting circle configuration are related by exact algebra, with no approximations. The Soddy completion defines a companion scale $F^2 = α^2 μ_\star$ with $α= \sqrt{3/2} - 1$ and $μ_\star = \sum_\ell m_\ell$; identifying this scale with $\bar{m}^{\rm MS}_s(μ_\star)$ yields a light-quark mass cascade with the ratio $m_d/m_s = 5/2 - \sqrt{6}$. Combined with the leading Gatto-Sartori-Tonin relation, this gives the down-sector Cabibbo seed $\sqrt{m_d/m_s} = \sqrt{3/2} - 1 = 0.22474\ldots$, numerically close to the measured $|V_{us}| = 0.22503 \pm 0.00068$ ($0.4σ$). A full CKM evaluation requires the up-sector phase correction, which we defer. The correspondence is testable by future lattice QCD+QED determinations of $m_d/m_s$; explicit failure modes are listed.

physics.gen-ph↗

arXiv2026

Structure of Logarithmically-Corrected Starobinsky Fuzzy Dark Matter Black Holes

This work constructs an anisotropic, Einasto-profile fuzzy dark matter (DM) black hole (BH) using a logarithmically-corrected Starobinsky gravity, $f(R)=R+βR^2+γR^2\ln(R/μ^2)$, a form motivated by one-loop quantum corrections to the gravitational action rather than by the pure quadratic term alone. We derive the generalized trace equation for this action, show that its $β$- and $γ$-dependence collapses to a single compact source term, and solve the resulting field equations perturbatively about an exact general-relativistic (GR) background for two distinct anisotropic equations of state: a de~Sitter-type branch and a non-local branch, the latter worked through to a closed tangential-pressure profile rather than left incomplete. The logarithmic correction is found to raise the extremal (zero-temperature) threshold relative to pure quadratic gravity and to increase the core tangential pressure noticeably in the non-local branch.

physics.gen-ph↗