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Rate of losing energy in Quantum Redshift
The paper uses the distance and temperature of 47,111 hottest nearby space objects including stars, quasars, white dwarf, and carbon stars. We have used SIMBAD Astronomical Database and obtained this information from 930,000 records. The range of temperature of the hottest objects is between 6158 and 99,575 K. Also, the distance of the objects is between 231.7375 and 1 (mas). We report the correlation between the distance and temperature of these hot objects at the temperature upper than 6632 K is equal to 0.135063 and will be increased to 0.32001 at temperatures upper than 9860 K. Also, the correlation between the temperature and distance of objects hotter than 12,000 K is equal to 0.270218.
Cosmic Microwave Background (CMB) is radiation that we receive from all directions of space. Most scientists believe that it is a radiant of the early universe. Its spectrum is equal to the spectrum of the blackbody in 2.725 K. We show that Quantum Redshift can describe CMB spectrum without the big bang and inflation theories. In the Quantum Redshift, at the emitting time, periods of the electromagnetic waves are not fully filled, and they are interested in absorbing quanta energies from younger periods. In this mechanism electromagnetic waves lose some periods while their quanta energies share with the remaining periods. Hence, their frequency will be decreased, and their spectrum will be converted to a lower equivalent temperature until their spectrum reaches the CMB spectrum. We anticipate our assay to be a starting point for a more sophisticated modeling universe. Predicting the age and size of the universe in a no expansion space is another usage of the Quantum CMB.
The Redshift of the electromagnetic waves is a powerful tool for calculating the distance of the objects in space and studying their behavior. However, physicists' misinterpretation of why Redshift occurs has led us to a misunderstanding of the most cosmological phenomena. The paper introduces Quantum Redshift (QR) by using the quantum structure of the electromagnetic waves (QSEW) In the Quantum Redshift, although the Planck constant is the smallest unit of three-dimensional energy, it is consisting of smaller units of one-dimensional energy. The maximum energy of each period of the electromagnetic waves is equal to the Planck constant hence, the capacity of each period is carrying 89875518173474223 one-dimensional quanta energy. However, in the QR, at the emitting time of the electromagnetic waves, their periods are not fully filled. On the other hand, they are interested in sharing quanta energies with each other to have fully filled periods. Sharing the quanta energies ofا some periods between other periods is the reason for destroying some periods and decreasing the frequency of the electromagnetic waves. Our other studies show Quantum Redshift can well explain the whole phenomenon of the universe, and real data support our theory. The quantum redshift rejects the big bang theory, expansion of space and dark energy. It predicts dark matters and describes CMB. The paper obtains the basic equation of the QR for use in future papers.
In this paper, we consider a holographic dark energy model driven by the gravitationally induced adiabatic matter creation with constant creation rate. It is assumed that the present accelerating stage is a consequence of the negative pressure describing the irreversible process of gravitational matter creation. Exact solutions are obtained to discuss the evolution of the universe. We obtain the best-fit values of the model parameters through MCMC method by the use of EMCEE python package on latest observational data. With the best-fit values, it is found that the universe shows transition from decelerated phase to accelerated phase. We carry out the diagnostic analysis to distinguish our model with other standard dark energy models. We also discuss the cosmography analysis of our model. We analyse the model by applying Akaike information criterion (AIC) and Bayesian information criterion (BIC) based on the penalization associated to the number of parameters. The results show that the model behaves quintessence like and approaches to CDM model in late time.
Three general cases of dynamical interacting dark energy models (-class) are investigated in the context of Brans-Dicke cosmology. Some of important cosmological quantities are calculated for every cases as a function of redshift parameter. The most important part of this paper deals with fitting models with two different expansion history: (\mbox{SNIa}+ \mbox{BAO}_{A}+\mathit{Omh}^{2} and \mbox{SNIa}+ \mbox{BAO}_{A}+H(z)) and with two different sets of data for Hubble parameter. This provides a remarkable feature to could analytically see the effects of each analyses and each data sets on final results. The best fitted values of parameters according to these analyses and data points, , AIC and BIC are reported. By these diagnostic tools we found that some of these models have no chance against CDM, even without need to study the structure formation, and could be ruled out. While some (e.g. and ) render the best fit quality, i.e. the value of AIC and BIC and figures shows that they fit perfectly with overall data and reveals a strong evidence in favor of these two models against CDM.
In this article, the model of an expanding universe, which is more than a century old and evolved into the Λ-CDM, is found to violate causality. This is shown by constructing the lightcone, which is relevant for any point in space, and by calculating the curvature for that point. From these calculations it is concluded that for any homogeneous and isotropic energy density in space, the geodesic of a test mass in it is always straight. With that, it follows that space is flat for any energy density. Furthermore an alternative theory is proposed as a demonstration that, with different explanations of the astronomical observations, a theory can be constructed that isn't in contradiction with General Relativity.
We make a direct comparison of the derived dark matter (DM) distributions between hydrodynamical simulations of dwarf galaxies assuming a ΛCDM cosmology and the observed dwarf galaxies sample from the THINGS survey in terms of (1) the rotation curve shape and (2) the logarithmic inner density slope α of mass density profiles. The simulations, which include the effect of baryonic feedback processes, such as gas cooling, star formation, cosmic UV background heating, and most importantly, physically motivated gas outflows driven by supernovae, form bulgeless galaxies with DM cores. We show that the stellar and baryonic mass is similar to that inferred from photometric and kinematic methods for galaxies of similar circular velocity. Analyzing the simulations in exactly the same way as the observational sample allows us to address directly the so-called cusp/core problem in the ΛCDM model. We show that the rotation curves of the simulated dwarf galaxies rise less steeply than cold dark matter rotation curves and are consistent with those of the THINGS dwarf galaxies. The mean value of the logarithmic inner density slopes α of the simulated galaxies' DM density profiles is ~–0.4 ± 0.1, which shows good agreement with α = –0.29 ± 0.07 of the THINGS dwarf galaxies. The effect of non-circular motions is not significant enough to affect the results. This confirms that the baryonic feedback processes included in the simulations are efficiently able to make the initial cusps with α ~–1.0 to –1.5 predicted by DM-only simulations shallower and induce DM halos with a central mass distribution similar to that observed in nearby dwarf galaxies.
We present spectral and photometric observations of 10 Type Ia supernovae (SNe Ia) in the redshift range 0.16 ≤ z ≤ 0.62. The luminosity distances of these objects are determined by methods that employ relations between SN Ia luminosity and light curve shape. Combined with previous data from our High-z Supernova Search Team and recent results by Riess et al., this expanded set of 16 high-redshift supernovae and a set of 34 nearby supernovae are used to place constraints on the following cosmological parameters: the Hubble constant (H0), the mass density (ΩM), the cosmological constant (i.e., the vacuum energy density, ΩΛ), the deceleration parameter (q0), and the dynamical age of the universe (t0). The distances of the high-redshift SNe Ia are, on average, 10%–15% farther than expected in a low mass density (ΩM = 0.2) universe without a cosmological constant. Different light curve fitting methods, SN Ia subsamples, and prior constraints unanimously favor eternally expanding models with positive cosmological constant (i.e., ΩΛ > 0) and a current acceleration of the expansion (i.e., q0 < 0). With no prior constraint on mass density other than ΩM ≥ 0, the spectroscopically confirmed SNe Ia are statistically consistent with q0 < 0 at the 2.8 σ and 3.9 σ confidence levels, and with ΩΛ > 0 at the 3.0 σ and 4.0 σ confidence levels, for two different fitting methods, respectively. Fixing a "minimal" mass density, ΩM = 0.2, results in the weakest detection, ΩΛ > 0 at the 3.0 σ confidence level from one of the two methods. For a flat universe prior (ΩM + ΩΛ = 1), the spectroscopically confirmed SNe Ia require ΩΛ > 0 at 7 σ and 9 σ formal statistical significance for the two different fitting methods. A universe closed by ordinary matter (i.e., ΩM = 1) is formally ruled out at the 7 σ to 8 σ confidence level for the two different fitting methods. We estimate the dynamical age of the universe to be 14.2 ± 1.7 Gyr including systematic uncertainties in the current Cepheid distance scale. We estimate the likely effect of several sources of systematic error, including progenitor and metallicity evolution, extinction, sample selection bias, local perturbations in the expansion rate, gravitational lensing, and sample contamination. Presently, none of these effects appear to reconcile the data with ΩΛ = 0 and q0 ≥ 0.
The Hubble constant, which measures the expansion rate, together with the total energy density of the Universe, sets the size of the observable Universe, its age, and its radius of curvature. Excellent progress has been made recently toward the measurement of the Hubble constant: a number of different methods for measuring distances have been developed and refined, and a primary project of the Hubble Space Telescope has been the accurate calibration of this difficult-to-measure parameter. The recent progress in these measurements is summarized, and areas where further work is needed are discussed. Currently, for a wide range of possible cosmological models, the Universe appears to have a kinematic age less than about 14±2 billion years. Combined with current estimates of stellar ages, the results favor a low-matter-density universe. They are consistent with either an open universe, or a flat universe with a non-zero value of the cosmological constant.
A milestone of modern cosmology was the prediction and serendipitous discovery of the Cosmic Microwave Background (CMB), the radiation left over after decoupling from matter in the early evolutionary stages of the Universe. A prediction of the standard hot Big-Bang model is the linear increase with redshift of the black-body temperature of the CMB (TCMB). This radiation excites the rotational levels of some interstellar molecules, including carbon monoxide (CO), which can serve as cosmic thermometers. Using three new and two previously reported CO absorption-line systems detected in quasar spectra during a systematic survey carried out using VLT/UVES, we constrain the evolution of TCMB to z~3. Combining our precise measurements with previous constraints, we obtain TCMB(z)=(2.725+/-0.002)x(1+z)^(1-beta) K with beta=-0.007+/-0.027, a more than two-fold improvement in precision. The measurements are consistent with the standard (i.e. adiabatic, beta=0) Big-Bang model and provide a strong constraint on the effective equation of state of decaying dark energy (i.e. w_eff=-0.996+/-0.025). Comment: accepted for publication in A&A Letters
Arising from: H. Muller, A. Peters & S. Chu Nature 463, 926-929 (2010); Muller & Chu reply
In ref. 1 the authors present a re-interpretation of atom interferometry experiments published a decade ago. They now consider the atom interferometry experiments as a measurement of the gravitational redshift on the quantum clock operating at the Compton frequency [ohgr]C = mc2/nature09340-m1jpg422914 [ap] 2[pgr] [times] 3.0 [times] 1025 Hz, where m is the caesium (Cs) atom rest mass. They then argue that this redshift measurement compares favourably with existing as well as projected clock tests. Here we show that this interpretation is incorrect.
The FIRAS data are independently recalibrated using the WMAP data to obtain a CMB temperature of 2.7260 +/- 0.0013. Measurements of the temperature of the cosmic microwave background are reviewed. The determination from the measurements from the literature is cosmic microwave background temperature of 2.72548 +/- 0.00057 K. Comment: 6 Pages 3 figures
Much like ordinary matter, dark matter might consist of elementary particles, and weakly interacting massive particles are one of the prime suspects. During the past decade, the sensitivity of experiments trying to directly detect them has improved by three to four orders of magnitude, but solid evidence for their existence is yet to come. We overview the recent progress in direct dark matter detection experiments and discuss future directions.
Recent measurements of the cosmic microwave background (CMB) anisotropies by
Planck provide a sensitive probe of dark matter annihilation during the cosmic
dark ages, and specifically constrain the annihilation parameter
. Using new results (Paper II)
for the ionization produced by particles injected at arbitrary energies, we
calculate and provide values for photons and pairs
injected at keV-TeV energies; the value for any dark matter
model can be obtained straightforwardly by weighting these results by the
spectrum of annihilation products. This result allows the sensitive and robust
constraints on dark matter annihilation presented by the Planck Collaboration
to be applied to arbitrary dark matter models with s-wave annihilation. We
demonstrate the validity of this approach using principal component analysis.
As an example, we integrate over the spectrum of annihilation products for a
range of Standard Model final states to determine the CMB bounds on these
models as a function of dark matter mass, and demonstrate that the new limits
generically exclude models proposed to explain the observed high-energy rise in
the cosmic ray positron fraction. We make our results publicly available at
http://nebel.rc.fas.harvard.edu/epsilon.
The theoretical framework of cosmology is mainly defined by gravity, of which general relativity is the current model. Recent tests of general relativity within the Lambda Cold Dark Matter (ΛCDM) model have found a concordance between predictions and the observations of the growth rate and clustering of the cosmic web. General relativity has not hitherto been tested on cosmological scales independently of the assumptions of the ΛCDM model. Here we report an observation of the gravitational redshift of light coming from galaxies in clusters at the 99 per cent confidence level, based on archival data. Our measurement agrees with the predictions of general relativity and its modification created to explain cosmic acceleration without the need for dark energy (the f(R) theory), but is inconsistent with alternative models designed to avoid the presence of dark matter.
We compute in detail the rate at which energy injected by dark matter annihilation heats and ionizes the photon-baryon plasma at z ~ 1000, and provide accurate fitting functions over the relevant redshift range for a broad array of annihilation channels and DM masses. The resulting perturbations to the ionization history can be constrained by measurements of the CMB temperature and polarization angular power spectra. We show that models which fit recently measured excesses in 10-1000 GeV electron and positron cosmic rays are already close to the 95% confidence limits from WMAP. The recently launched Planck satellite will be capable of ruling out a wide range of DM explanations for these excesses. In models of dark matter with Sommerfeld-enhanced annihilation, where sigma v rises with decreasing WIMP velocity until some saturation point, the WMAP5 constraints imply that the enhancement must be close to saturation in the neighborhood of the Earth. Comment: 17 pages, 6 figures, v2 extends discussion of constraints on Sommerfeld-enhanced models
We propose a method for cosmographic measurements by combining gravitational lensing of the cosmic microwave background (CMB) with cosmic shear surveys. We cross-correlate the galaxy counts in the lens plane with two different source planes: the CMB at and galaxies at an intermediate redshift. The ratio of the galaxy count/CMB lensing cross-correlation to the galaxy count/galaxy lensing cross correlation is shown to be a purely geometric quantity, depending only on the distribution function of the source galaxies. By combining Planck, ADEPT and LSST the ratio can be measured to accuracy, whereas a future polarization based experiment like CMBPOL can make a more precise () measurement. For cosmological models where the curvature and the equation of state parameter are allowed to vary, the direction of degeneracy defined by the measurement of this ratio is different from that traced out by Baryon Acoustic Oscillation (BAO) measurements. Combining this method with the stacked cluster mass reconstruction cosmography technique as proposed by Hu, Holz and Vale (2007), the uncertainty in the ratio can be further reduced, improving the constraints on cosmological parameters. We also study the implications of the lensing-ratio measurement for early dark energy models, in context of the parameterization proposed by Doran and Robbers (2006). For models which are degenerate with respect to the CMB, we find both BAO and lensing-ratio measurements to be insensitive to the early component of the dark energy density. Comment: 8 pages; 7 figures
Dark energy and the accelerating universe
- Joshua A Frieman