arXiv subjects

Luciano Lorenzi

Publications and source records attributed to Luciano Lorenzi.

5 recordsLinked to original sources

arXiv2012

A crucial dipole test of the expansion center Universe - based on high-z SCP Union & Union2 supernovae

The expansion center Universe (ECU) gives a dipole anisotropy to the Hubble ratio, at any Hubble depth D. After a long series of successful dipole tests, here is a crucial multiple dipole test at z bins centred on the mean =z0=1, or Hubble depth D=c/H0, and based on data from SCP Union & Union2 compilation. Table 5abc lists data of two main samples, with 48 SCPU SNe Ia and 58 SCPU2 SNe Ia respectively. The confirmed dipole anisotropy, shown by 6 primary sample tests and by another 27 from 9 encapsulated z bins with DL=D(1+z) assumed and the Hubble Magnitude definition, gives a model independent result, in full accordance with the expansion center model (ECM). That means a maximum cz range of about 50000 km/s at the central redshift z0=1. As a complement to the dipole tests, here is a new computation of the relativistic deceleration parameter q0, based on the extrapolated total M spread, that is the deviation of the Hubble Magnitude M of high-z SCP Union supernovae at a normal or central redshift =z0=z << 1 from the absolute magnitude M0 at z0=0 (cf. parallel paper XVI). A total M spread according to ECM is derived from 249 high-z SCPU SNe listed in paper XVI. In a concordance test with the expansion center model, the obtained new relativistic q0 agrees with the value q0=+2 inferred from the ECM paper I eq. (41), when R0 is the proper distance at t0 of the expansion center from the Galaxy.

physics.gen-ph↗

arXiv2012

Dipole & absolute magnitude analysis of the SCP Union supernovae within the expansion center model

1743 data calculated for 249 high-z SCP Union supernovae are analysed according to the expansion center model (ECM). The analysis in Hubble units begins with 13 listed normal points corresponding to 13 z-bin samples at as many Hubble depths. The novel finding is a clear drop in the average scattering of the SNe Ia Hubble Magnitude M with the ECM Hubble depth D, after using the average trend computed in paper IX. Other correlations of the M scattering with the position in the sky are proposed. Consequently, 13 ECM dipole tests on the 13 z-bin samples were carried out both with unweighted and weighted fittings. A further check was made with Hubble depths D obtained by assuming M= according to paper IX and XV. In conclusion the analysis of 249 SCPU SNe confirms once again the expansion center model at any Hubble depth, including a strengthening perturbation effect of the M scattering at decreasing z<0.5. A new successful dipole test introduces the absolute magnitude analysis of 398 SCPU supernovae. After testing 14 high-z normal points from paper IX Table 2, a trend analysis of another 15 and 30 normal points of the Hubble Magnitude M and a new absolute magnitude M*, at increasing =z0 corresponding to a different series of z bins, leads to the discovery of the magnitude anomaly of the low points. When the low points are excluded, the best fittings make it possible to extrapolate the SNe Ia absolute magnitude M0 at a central redshift z0=0, with M0=-17.9+-0.1 and a few final ECM solutions of the SNe Ia and M*. The magnitude anomaly is here interpreted as due to a deficiency in the magnitude formulas used; these produce a maximum peak of deviation in the range 0.04 < < 0.08. That is a proof of the Universe rotation within the expansion center model.

physics.gen-ph↗

arXiv2010

The New Wedge-Shaped Hubble Diagram of 398 SCP Supernovae According to the Expansion Center Model

Following the successful dipole test on 53 SCP SNe Ia presented at SAIt2004 in Milan, this 9th contribution to the ECM series beginning in 1999 in Naples (43th SAIt meeting: "Revolutions in Astronomy") deals with the construction of the new wedge-shaped Hubble diagram obtained with 398 supernovae of the SCP Union Compilation (Kowalski et al. 2008) by applying a calculated correlation between SNe Ia absolute blue magnitude MB and central redshift z0, according to the expansion center model. The ECM distance D of the Hubble diagram (cz versus D) is computed as the ratio between the luminosity distance DL and 1 + z. Mathematically D results to be a power series of the light-space r run inside the expanding cosmic medium or Hubble flow; thus its expression is independent of the corresponding z. In addition one can have D = D(z, h) from the ECM Hubble law by using the h convention with an anisotropic HX. It is proposed to the meeting that the wedge-shape of this new Hubble diagram be confirmed independently as mainly due to the ECM dipole anisotropy of the Hubble ratio cz/D.

physics.gen-ph↗

arXiv1999

I-The Expanding Universe from the Huge Void Center: Theory & Modelling

To add to and refine the model presented at the Grado3 meeting, of a radial Hubble expansion from the Bahcall & Soneira huge void center, it is here outlined a formal analytical formulation of the theory and modelling on which the previous check work based itself. The new Hubble Law contains the distance R from the expansion center, multiplied by an angular function, and the H's variation, whose meaning and expression have been obtained and examined through a Galaxy Hubble law analysis based on derivatives with respect to light-space. This H's variation, as predicted by the model, is due to a combination of two dominant effects, respectively time (TE) and space (SE). Structurally the scattering noise of the nearby Universe Hubble ratios seems to be partially caused by a perturbative term. In conclusion a fundamental confirmation test of the model is presented. As a physical result, one obtains a higher matter density of the Universe.

astro-ph↗

arXiv1999

II-Local Solution of a Spherical Homogeneous and Isotropic Universe Radially Decelerated towards the Expansion Center: Tests on Historic Data Sets

The topic of the paper is the mathematical analysis of a radially decelerated Hubble expansion from the Bahcall & Soneira void center. Such analysis, in the hypothesis of local homogeneity and isotropy, gives a particular Hubble ratio dipole structure to the expansion equation, whose solution has been studied at different precision orders and successfully tested on a few historic data sets, by de Vaucouleurs (1965), by Sandage & Tammann (1975), and by Aaronson et al. (1982-86). The fittings of both the separate AA1 and AA2 samples show a good solution convergence as the analysis order increases, giving even coinciding solutions when applied to 308 nearby individual galaxies (308AA1) and to 10 clusters (148AA2), respectively.

astro-ph↗