Relativistic Cosmology and the Pioneers Anomaly

NASA spacecrafts has suffered from three anomalies. The Pioneers spacecrafts were decelerated, and their spin when not disturbed, was declining. On the other hand, fly-bys for gravity assists, appeared with extra speeds, relative to infinity. The Pioneers and fly-by anomalies are given now exact general relativistic full general solutions, in a rotating expanding Universe. We cite new evidence on the rotation of the Universe. Our solution seems to be the only one that solves the three anomalies.

Classical Cosmology II. The Einstein Ring

The Einstein ring is usually explained in the framework of the gravitational lens. Conversely here we apply the framework of the expansion of a superbubble (SB) in order to explain the spherical appearance of the ring. Two classical equations of motion for SBs are derived in the presence of a linear and a trigonometric decrease for density. A relativistic equation of motion with an inverse square dependence for the density is derived. The angular distance, adopting the minimax approximation, is derived for three relativistic cosmologies: the standard, the flat and the wCDM. We derive the relation between redshift and Euclidean distance, which allows fixing the radius of the Einstein ring. The details of the ring are explained by a simple version of the theory of images.

THE RELATIVISTIC COSMOLOGY UNDER THE HARMONIC CONDITION(Ⅰ)

The harmonic condition is applied to the motion of galaxies in relativistic cosmology. For the material universe we consider that the average distribution of matter on the large scale in the universe is homogenous and isotropic, but within each small region individual galaxies can have large or small masses. Each galaxy moves according to the laws of motion determined by the field equations of gravitation for the average distribution of matter in the whole universe. Transformations between the isotropic, the co-moving, theRobertson-Walker and the standard system of coordinates can be derived by using the harmonic condition.

A critique of supernova data analysis in cosmology

Observational astronomy has shown significant growth over the last decade and has made important contributions to cosmology. A major paradigm shift in cosmology was brought about by observations of Type Ia supernovae. The notion that the universe is accelerating has led to several theoretical challenges. Unfortunately, although high-quality supernovae data-sets are being produced, their statistical anal- ysis leaves much to be desired. Instead of using the data to directly test the model, several studies seem to concentrate on assuming the model to be correct and limiting themselves to estimating model parameters and internal errors. As shown here, the important purpose of testing a cosmological theory is thereby vitiated.

The Ring Produced by an Extra-Galactic Superbubble in Flat Cosmology

A superbubble which advances in a symmetric Navarro-Frenk-White density profile or in an auto-gravitating density profile generates a thick shell with a radius that can reach 10 kpc. The application of the symmetric and asymmetric image theory to this thick 3D shell produces a ring in the 2D map of intensity and a characteristic “U” shape in the case of 1D cut of the intensity. A comparison of such a ring originating from a superbubble is made with the Einstein’s ring. A Taylor approximation of order 10 for the angular diameter distance is derived in order to deal with high values of the redshift.

An Analytical Solution in the Complex Plane for the Luminosity Distance in Flat Cosmology

We present an analytical solution for the luminosity distance in spatially flat cosmology with pressureless matter and the cosmological constant. The complex analytical solution is made of a real part and a negligible imaginary part. The real part of the luminosity distance allows finding the two parameters H0 and ΩM . A simple expression for the distance modulus for SNs of type Ia is reported in the framework of the mini-max approximation.

Cosmology using long gamma-ray bursts: statistical analysis of errors in calibrated data

We investigate direction dependence and non-Gaussian features in high-z cosmological data using ?_(χ~2) and ?_χ statistics and the Kolmogorov-Smirnov test. These techniques are applied on a set of calibrated long gamma-ray bursts(GRBs) and its combination with recent Type Ia supernovae data(Union2). Our statistical analysis shows a weak but consistent direction dependence in both the data sets.The analysis also indicates a non-Gaussian nature of errors in both data sets.

Sparse Formulae for the Distance Modulus in Cosmology

We review the distance modulus in twelve different cosmologies: the ΛCDM model, the wCDM model, the Cardassian model, the flat case, the øCDM cosmology, the Einstein—De Sitter model, the modified Einstein—De Sitter model, the simple GR model, the flat expanding model, the Milne model, the plasma model and the modified tired light model. The above distance moduli are processed for three different compilations of supernovae and a supernovae + GRBs compilation: Union 2.1, JLA, the Pantheon and Union 2.1 + 59 GRBs. For each of the 48 analysed cases we report the relative cosmological parameters, the chi-square, the reduced chi-square, the AIC and the Q parameter. The angular distance as function of the redshift for five cosmologies is reported in the framework of the minimax approximation.

Four new observational H(z) data from luminous red galaxies in the Sloan Digital Sky Survey data release seven

By adopting the differential age method, we select 17 832 luminous red galaxies from the Sloan Digital Sky Survey Data Release Seven covering redshift 0 〈 z 〈 0.4 to measure the Hubble parameter. Using the full spectrum fitting package UZySS, these spectra are reduced with single stellar population models and optimal age information from our selected sample is derived. With the decreasing age-redshift relation, four new observational H（z） data （OHD） points are obtained, which are H（z） = 69.0 ± 19.6 km s^-1 Mpc^-1 at z = 0.07, H（z） = 68.6± 26.2 km s^-1 Mpc^-1 at z = 0.12, H（z）=72.9 ± 29.6 km s^-1 Mpc^-1 at z = 0.2 and H（z）=88.8 ± 36.6 km s^-1 Mpc^-1 at z = 0.28, respectively. Combined with 21 other available OHD data points, the performance of the constraint on both flat and non-flat ACDM models is presented.

Testing the Coincidence Problem with Strong Gravitational Lens,Type Ia Supernovae and Hubble Parameter Observational Data

In this paper,we use three different kinds of observational data,including 130 strong gravitational lensing(SGL)systems,type Ia supernovae(SNeIa:Pantheon and Union2.1)and 31 Hubble parameter data points(H(z))from cosmic chronometers to constrain the phenomenological model(ρ_(x)∝ρ_(m)a^(ξ)).By combining these three kinds of data(Union2.1+SGL+H(z)),we get the parameter value at the confidence interval of 2σ,Ω_(X,0)=0.69±0.34,ω_(x)=−1.24±0.61,ξ=3.8±3.9 and H_(0)=70.22±0.86 kms^(−1) Mpc^(−1).According to our results,we find that theΛCDM model is still the model which is in best agreement with the observational data at present,and the coincidence problem is not alleviated.In addition,the Ω_(X) and Ω_(m) have the same order of magnitude in 0<z<1.26.Finally,we obtain the transition redshift z_(T)=0.645.If the transition occurs in z>0.645,it is necessary to introduce the dark energy interacting with dark matter.

Classical and Relativistic Models for Time Duration of Gamma-Ray Bursts

A classical model based on a power law assumption for the radius-time relationship in the expansion of a supernova (SN) allows to derive an analytical expression for the flow of mechanical kinetic energy and the time duration of gamma-ray burst (GRB). A random process based on the ratio of two truncated lognormal distributions for luminosity and luminosity distance allows to derive the statistical distribution for time duration of GRBs. The high velocities involved in the first phase of expansion of a SN require a relativistic treatment. The circumstellar medium is assumed to follow a density profile of Plummer type with eta = 6. A series solution for the relativistic flow of kinetic energy allows to derive in a numerical way the duration time for GRBs. Here we analyze two cosmologies: the standard cosmology and the plasma cosmology.

Non-Uniqueness of Einstein’s Special Relativity, and the Inconclusiveness of High Energy (Relativistic) Physics

In this paper, we present a new form of “special relativity” (BSR), which is isomorphic to Einstein’s “special relativity” (ESR). This in turn proves the non-uniqueness of Einstein’s “special relativity” and implies the inconclusiveness of so-called “relativistic physics”. This work presents new results of principal significance for the foundations of physics and practical results for high energy physics, deep space astrophysics, and cosmology as well. The entire exposition is done within the formalism of the Lorentz SL(2C) group acting via isometries on real 3-dimensional Lobachevskian (hyperbolic) spaces L3 regarded as quotients SL(2C)/SU(2). We show via direct calculations that both ESR and BSR are parametric maps from Lobachevskian into Euclidean space, namely a gnomonic (central) map in the case of ESR, and a stereographic map in the case of BSR. Such an identification allows us to link these maps to relevant models of Lobachevskian geometry. Thus, we identify ESR as the physical realization of the Beltrami-Klein (non-conformal) model, and BSR as the physical realization of the Poincare (conformal) model of Lobachevskian geometry. Although we focus our discussion on ball models of Lobachevskian geometry, our method is quite general, and for instance, may be applied to the half-space model of Lobachevskian geometry with appropriate “Lorentz group” acting via isometries on (positive) half space, resulting yet in another “special relativity” isomorphic with ESR and BSR. By using the notion of a homotopy of maps, the identification of “special relativities” as maps from Lobachevskian into Euclidean space allows us to justify the existence of an uncountable infinity of hybrid “special relativities” and consequently an uncountable infinity of “relativistic physics” built upon them. This is another new result in physics and it states that so called “relativistic physics” is unique only up to a homotopy. Finally, we show that “paradoxes” of “special relativities” in either ESR or BSR are simply common distortions of maps between non-isometric spaces. The entire exposition is kept at elementary level accessible to majority of students in physics and/or engineering.

Dynamical Dark Energy in Light of Cosmic Distance Measurements.Ⅱ.A Study Using Current Observations

We extract key information on dark energy from current observations of BAO,OHD and H_(0),and find hints of dynamical behavior of dark energy.In particular,a dynamical dark energy model whose equation of state crosses-1 is favored by observations.We also find that the Universe has started accelerating at a lower redshift than expected.

FLRW cosmology in metric-affine F(R,Q)gravity

We investigated some Friedmann-Lemaître-Robertson-Walker(FLRW)cosmological models in the context of metric-affine F(R,Q)gravity,as proposed in[arXiv:1205.5266v6].Here,R and Q are the curvature and nonmetricity scalars using non-special connections,respectively.We obtained the modified field equations using a flat FLRW metric.We then found a connection between the Hubble constant H_(0),density parameter Ω_(m0),and other model parameters in two different situations involving scalars u and w.Next,we used new observational datasets,such as the cosmic chronometer(CC)Hubble and Pantheon SNe Ia datasets,to determine the optimal model parameter values through a Markov chain Monte Carlo(MCMC)analysis.Using these best-fit values of the model parameters,we discussed the results and behavior of the derived models.Further,we discussed the Akaike information criterion(AIC)and Bayesian information criterion(BIC)for the derived models in the context of the Lambda cold dark matter(ΛCDM).We found that the geometrical sector dark equation of state parameter ω_(de)behaves just like a dark energy candidate.We also found that both models are transit phase models.Model-Ⅰ approaches the ΛCDM model in the late-time universe,whereas Model-Ⅱ approaches quintessence scenarios.

Quantized Redshift and its Significance for Recent Observation

With the recent observational evidence in extragalactic astronomy,the interpretation of the nature of quasar redshift continues to be a research interest.Very high redshifts are being detected for extragalactic objects that are presumably very distant and young while also exhibiting properties that are characteristic of a more mature galaxy such as ours.According to Halton Arp and Geoffrey Burbidge,redshift disparities consist of an intrinsic component and are related to an evolutionary process.Karlsson observed redshift periodicity at integer multiples of0.089 in log scale and Burbidge observed redshift periodicity at integer multiples of 0.061 in linear scale.Since Singular Value Decomposition based periodicity estimation is known to be superior for noisy data sets,especially when the data contain multiple harmonics and overtones,mainly irregular in nature,we have chosen it to be our primary tool for analysis of the quasar-galaxy pair redshift data.We have observed a fundamental periodicity of0.051 with a confidence interval of 95%in linear scale with the site-available Sloan Digital Sky Survey Data Release 7(SDSS DR7)quasar-galaxy pair data set.We have independently generated quasar-galaxy pair data sets from both 2d F and SDSS and found fundamental periodicities of 0.077 and 0.089,respectively,in log scale with a confidence interval of 95%.

Observational Constraints on Varying Alpha in Λ(α)CDM Cosmology

In this work, we consider the so-called Λ(α)CDM cosmology with Λ∝α^(-6) while the fine-structure"constant" α is varying. In this scenario, the accelerated expansion of the universe is driven by the cosmological"constant" Λ(equivalently the vacuum energy), and the varying α is driven by a subdominant scalar field ? coupling with the electromagnetic field. The observational constraints on the varying α and Λ∝α^(-6) models with various couplings BF(?) between the subdominant scalar field ? and the electromagnetic field are considered.

H(z)数据对相互作用暗能量模型的观测研究

结合最新的哈勃参量H(z)观测数据、重子声学振荡(BAO)数据与普朗克卫星观测得到的宇宙微波背景辐射(CMB)数据,利用马尔柯夫链蒙特卡洛算法(MCMC)对一种相互作用暗能量模型进行了观测限制.这3种数据联合限制得到的各参数的最佳拟合值及1σ误差范围分别为:物质能量密度参数?m=0.266+0.028-0.028,相互作用因子γ=0.090+0.100-0.098,暗能量状态方程参数wX=-1.307+0.263-0.269,哈勃常数H0=74.20+4.66-4.56.相互作用耦合参数γ>0表明能量正在从暗物质转移到暗能量.然而,宇宙学常数模型中的巧合性问题在1σ误差范围内依然可以轻微缓解.为了更好地做出比较,还利用BAO+CMB组合数据及单独的H(z)数据对该模型进行了考察,得到的结果如下:(1)H(z)数据能对相互作用参数γ给出更好的限制结果;(2)ΛCDM模型仍然是与观测数据符合得最好的模型,耦合参数γ与其它模型参数(?m,H0)相互关联;(3)在考虑了暗能量与暗物质间的相互作用之后,超新星局域距离阶梯测量与普朗克观测对H0限制结果的冲突问题能够得到一定程度的缓解.

观测宇宙学的一些新进展

系统介绍了观测宇宙学和其最新进展,包括观测手段和哈勃常数和宇宙的年龄、宇宙的暗物质、暗能量、背景辐射、大尺度结构、元素丰度、活动星系核、中微子、γ暴等热点问题,并提出了观测宇宙学存在的问题和挑战.

Ia超新星与哈勃常数(英文)

蓝 Ia超新星是迄今天文学家已知的校准得最好的标准烛光 ,峰值光度弥散仅为 0 .11mag.将近处距离已知的蓝 Ia超新星匹配到远处哈勃流样本中 ,便可获得哈勃常数的估计值 .当前的数据显示哈勃常数为H0 =( 55.3± 5.3) km· s-1· Mpc-1.

活动星系核的伽玛辐射和宇宙标准烛光(英文)

编辑了一个样本,其中包括71个Gev伽玛射线噪的活动星系核(14个BL Lac天体和57个平谱射电类星体),53个FRⅠ型射电星系和63个FRⅡ型射电星系。文章采用了非线性最小二乘法来拟合这个样本。当假设Mv=-23.0时,得到一个达到最佳拟合的哈勃常数,其拟合值为H0=71.5±3.8kms-1Mpc-1。该值与通过哈勃望远镜关键计划所得到的哈勃常数值H0=71.5±8kms-1Mpc-1符合得很好。其结果表明活动星系核的Gev伽玛辐射可以被用作宇宙标准烛光。