Scaling Behavior for the Susceptibility of the Vacuum

• 作者: Christopher Pilot
• 来源期刊: 天文学与天体物理学国际期刊(英文)
• 学科: 物理学
• 关键词: Extended Model of Gravity Dark Matter Dark Energy Cosmic Evolution of Density Parameters Gravitational Susceptibility of the Vacuum Vacuum Energy Polarization of Space
• 年，卷（期）: 2021,（1）
• 页码范围: 11-36
• 页数: 26页
• 分类号: O57

摘要

Using the two-component superfluid model of Winterberg for space, two models for the susceptibility of the cosmic vacuum as a function of the cosmic scale parameter, a, are presented. We also consider the possibility that Newton’s constant can scale,<em> i.e.</em>, <span style="white-space:nowrap;"><em>G</em>^-1=<em>G</em>^-1(<em>a</em>)</span>, to form the most general scaling laws for polarization of the vacuum. The positive and negative values for the Planckion mass, which form the basis of the Winterberg model, are inextricably linked to the value of G, and as such, both G and Planck mass are intrinsic properties of the vacuum. Scaling laws for the non-local, smeared, cosmic susceptibility, <img src="Edit_bd58a08a-5d33-4e33-b5c0-62650c0b1918.bmp" alt="" />, the cosmic polarization, <img src="Edit_56bd1950-09ae-49fa-bd34-e4ff13b30c56.bmp" alt="" />, the cosmic macroscopic gravitational field, <img src="Edit_1e22ee4f-7755-4b29-8f8d-66f20f98aaa7.bmp" alt="" />, and the cosmic gravitational field mass density, <img src="Edit_aabb0cf4-080e-4452-ba73-8f3d50e95363.bmp" alt="" />, are worked out, with specific examples. At the end of recombination,<em> i.e.</em>, the era of last scattering, using the polarization to explain dark matter, and the gravitational field mass density to explain dark energy, we find that, <img src="Edit_b4b9804e-a8db-4c86-a1ad-1bc5f8ec72fa.bmp" alt="" />. While this is an unconventional assignment, differing from the ΛCDM model, we believe this is correct, as localized dark matter (LDM) contributions can be much higher in this epoch than cosmic smeared values for susceptibility. All density parameter assignments in Friedmanns’ equation are cosmic averages, valid for distance scales in excess of 100 Mpc in the current epoch. We also evaluate the transition from ordinary matter dominance, to dark matter dominance, for the cosmos as a whole. We obtain for the transition points, <em>z</em>=1.66, for susceptibility model I, and, <em style="white-space:normal;">z</em><span