Testing the distance-duality relation with the baryon acoustic oscillations data and type Ia supernovae data

In this letter, the cosmic distance-duality relation has been constrained with a model-independent method by combining the baryon acoustic oscillation(BAO) data and the type Ia supernova(SNe Ia) data. The results show that this relation is consistent with the observational data in the 68.27% error range, except for the instance of Union 2.1 plus BAO with the statistic errors only,where the relation is consistent with the observations in the 95.45% error range. To study the result of the uncertainty of the Hubble constant on the investigation of this relation,we treat the dimensionless Hubble constant h as a free parameter and get that the observational data favors the relation in the 68.27% error range. And then h has been marginalized and the results support that this relation is favored by the observations in the 68.27% error range too.     

The tight-coupling approximation for baryon acoustic oscillations

The tight-coupling approximation (TCA) used to describe the early dynamics of the baryons–photons system is systematically built to higher orders in the inverse of the interaction rate. This expansion can be either used to grasp the physical effects by deriving simple analytic solutions or to obtain a form of the system which is stable numerically at early times. In linear cosmological perturbations, we estimate numerically its precision, and we discuss the implications for the baryons acoustic oscillations. The TCA can be extended to the second order cosmological perturbations, and in particular we recover that vorticity is not generated at lowest order of this expansion.     

Cosmological implications of different baryon acoustic oscillation data

In this work, we explore the cosmological implications of different baryon acoustic oscillation(BAO) data, including the BAO data extracted by using the spherically averaged one-dimensional galaxy clustering(GC) statistics(hereafter BAO1) and the BAO data obtained by using the anisotropic two-dimensional GC statistics(hereafter BAO2). To make a comparison, we also take into account the case without BAO data(hereafter NO BAO). Firstly, making use of these BAO data, as well as the SNLS3 type Ia supernovae sample and the Planck distance priors data, we give the cosmological constraints of the ΛCDM, the w CDM, and the Chevallier-Polarski-Linder(CPL) model. Then, we discuss the impacts of different BAO data on cosmological consquences, including its effects on parameter space, equation of state(Eo S), figure of merit(Fo M), deceleration-acceleration transition redshift,Hubble parameter H(z), deceleration parameter q(z), statefinder hierarchy S_3(1)(z), S_4(1)(z) and cosmic age t(z). We find that:(1)NO BAO data always give a smallest fractional matter density ?_(m0), a largest fractional curvature density ?k0and a largest Hubble constant h; in contrast, BAO1 data always give a largest ?_(m0), a smallest ?_(k0) and a smallest h.(2) For the w CDM and the CPL model, NO BAO data always give a largest Eo S w; in contrast, BAO2 data always give a smallest w.(3) Compared with the case of BAO1, BAO2 data always give a slightly larger Fo M, and thus can give a cosmological constraint with a slightly better accuracy.(4) The impacts of different BAO data on the cosmic evolution and the comic age are very small, and cannot be distinguished by using various dark energy diagnoses and the cosmic age data.     

Cosmological constraints from radial baryon acoustic oscillation measurements and observational Hubble data

We use the Radial Baryon Acoustic Oscillation (RBAO) measurements, distant type Ia supernovae (SNe Ia), the observational H(z)$H(z)$ data (OHD) and the Cosmic Microwave Background (CMB) shift parameter data to constrain cosmological parameters of ΛCDM$\mathrm{\Lambda }\text{CDM}$ and XCDM cosmologies and further examine the role of OHD and SNe Ia data in cosmological constraints. We marginalize the likelihood function over h   by integrating the probability density P∝e−χ²/2$P\propto e^{-{\chi }^2/2}$ to obtain the best fitting results and the confidence regions in the Ωm–ΩΛ${\Omega }_m\text{–}{\Omega }_{\Lambda }$ plane. With the combination analysis for both of the ΛCDM$\mathrm{\Lambda }\text{CDM}$ and XCDM models, we find that the confidence regions of 68.3%, 95.4% and 99.7% levels using OHD+RBAO+CMB$\text{OHD}+\text{RBAO}+\text{CMB}$ data are in good agreement with that of SNe Ia+RBAO+CMB$\text{Ia}+\text{RBAO}+\text{CMB}$ data which is consistent with the result of Lin et al.'s (2009) [24] work. With more data of OHD, we can probably constrain the cosmological parameters using OHD data instead of SNe Ia data in the future.     

Testing the cosmic conservation of photon number with type Ia supernovae and ages of old objects

In this paper, we obtain luminosity distances by using ages of 32 old passive galaxies distributed over the redshift interval \(0.11< z < 1.84\) and test the cosmic conservation of photon number by comparing them with 580 distance moduli of type Ia supernovae (SNe Ia) from the so-called Union 2.1 compilation. Our analyses are based on the fact that the method of obtaining ages of galaxies relies on the detailed shape of galaxy spectra but not on galaxy luminosity. Possible departures from cosmic conservation of photon number is parametrized by \(\tau (z) = 2 \upvarepsilon z\) and \(\tau (z) = \upvarepsilon z/(1+z)\) (for \(\upvarepsilon =0\) the conservation of photon number is recovered). We find \(\upvarepsilon =0.016^{+0.078}_{-0.075}\) from the first parametrization and \(\upvarepsilon =-\,0.18^{+0.25}_{-0.24}\) from the second parametrization, both limits at 95% c.l. In this way, no significant departure from cosmic conservation of photon number is verified. In addition, by considering the total age as inferred from Planck (2015) analysis, we find the incubation time \(t_{inc}=1.66\pm 0.29\) Gyr and \(t_{inc}=1.23\pm 0.27\) Gyr at 68% c.l. for each parametrization, respectively.     

Resonant neutrino oscillations and the neutrino signature of supernovae

We examine the effects of resonant neutrino oscillations, proposed as a solution to the solar neutrino puzzle, on the neutrino signature of a Type II supernova. We find that, for parameters corresponding to an adiabatic conversion of most of the ⁸B neutrino flux, the supernova neutrino signal in a water-Čerenkov detector is altered in the following way: (1) The isotropic-to-directional event ratio increases; (2) The short time scale neutronization burst signal decreases by a factor 7, perhaps rendering it unobservable. Detection of these changes would allow one to distinguish between neutrino oscillations and solar model alterations as solutions to the solar neutrino problem. We also note that mixing of the higher energy ν_μ and ν_r's to ν_e's will enhance detection of the thermally produced ν-flux.     

Diffractive baryon production and the relation between reggeon and photon couplings

We illustrate how one can employ the γ-analogy hypothesis, introduced in a previous paper, which relates the couplings of the leading natural-parity reggeon exchanges, P, f and ω, to those of the isoscalar part of the photon. It enables us to predict the differential cross sections for the diffractive processes $\text{pp}\text{→}\text{pN}{}^1\text{(}\text{5}\text{2}{}^{\mathrm{+}}\text{, 1688)}$, $\text{n}{}^1\text{(}\text{3}\text{2}{}^{\mathrm{?}}\text{, 1520)}$, and $\text{N}{}^1\text{(}\text{7}\text{2}{}^{\mathrm{?}}\text{,2190)}$ starting from Regge fits to pp elastic scattering, with just a single free parameter in each case. This success stems from an intimate relation between electromagnetic and hadronic couplings demanded by duality, scaling and vector dominance. We do not expect dips due to pole-cut interference in the N¹ production differential cross sections because of their more complicated helicity structure.     

An accurate determination of the Hubble constant from baryon acoustic oscillation datasets

Even though the Hubble constant cannot be significantly determined just by the low-redshift Baryon Acoustic Oscillation(BAO)data, it can be tightly constrained once the high-redshift BAO data are combined. We combined BAO data from 6d FGS, BOSS DR11 clustering of galaxies, Wiggle Z and z = 2.34 from BOSS DR11 quasar Lyman-α forest lines to get H0= 68.17+1.55-1.56 km s-1Mpc-1. In addition, we adopted the simultaneous measurements of H(z) and DA(z) from the two-dimensional two-point correlation function from BOSS DR9 CMASS sample and two-dimensional matter power spectrum from SDSS DR7 sample to obtain H0=(68.11±1.69) km s-1Mpc-1. Finally, combining all of the BAO datasets, we conclude that H0=(68.11±0.86) km s-1Mpc-1, a1.3% determination.     

Direct determination of the hubble parameter using type IIn supernovae

A novel approach, a Dense Shell Method, is proposed for measuring distances for cosmology. It is based on original Baade idea to relate absolute difference of photospheric radii with photospheric velocity. We demonstrate that this idea works: the new method does not rely on the Cosmic Distance Ladder and gives satisfactory results for the most luminous Type IIn Supernovae. This allows one to make them good primary distance indicators for cosmology. Fixing correction factors for illustration, we obtain with this method the median distance of ≈ 68₋₁₅⁺¹⁹(68%CL) Mpc to SN 2006gy and median Hubble parameter 79₋₁₇⁺²³(68%CL) km/(s Mpc).     

On neutrino oscillations and the time-energy uncertainty relation

We consider neutrino oscillations as a nonstationary phenomenon based on the Schrödinger evolution equation and mixed neutrino states with definite flavor. We demonstrate that for such states, invariance under translations in time does not take place. We show that the time-energy uncertainty relation plays a crucial role in neutrino oscillations. We compare neutrino oscillations with K ⁰ ? -K ⁰, B _d ⁰ ? B _d ⁰ , and other oscillations.     

Ion acoustic waves in the presence of Langmuir oscillations

The dielectric function for long-wavelength, low-frequency ion acoustic waves in the presence of short-wavelength, high-frequency electron oscillations is presented, where the ions are described by the collision-free Vlasov equation. The effect of the electron oscillations can be appropriately described by the introduction of an effective electron temperature.     

Constraints on accelerating universe using ESSENCE and Gold supernovae data combined with other cosmological probes

We use recent data: the 192 ESSENCE type Ia supernovae (SNe Ia), the 182 Gold SNe Ia, the three-year WMAP, the SDSS baryon acoustic peak, the X-ray gas mass fraction in clusters and the observational H(z) data, to constrain models of the accelerating universe. Combining the 192 ESSENCE data with the observational H(z) data to constrain the parameterized deceleration parameter, we obtain the best-fit values of the transition redshift and current deceleration parameter z _T=0.632_−0.127^+0.256 and q ₀=−0.788_−0.182^+0.182. Furthermore, using the ΛCDM model and two model-independent equations of state of the dark energy, we find that the combined constraint from the 192 ESSENCE data and four other cosmological observations gives smaller values for Ω _0m and q ₀, but a larger value for z _T than the combined constraint from the 182 Gold data with four other observations. Finally, according to the Akaike information criterion it is shown that the recently observed data equally support three dark energy models: ΛCDM, w _de(z)=w ₀ and w _de(z)=w ₀+w ₁ln (1+z).     

Stabilization of the ion acoustic instability by high frequency oscillations

The dielectric function for long wavelength, low frequency ion waves in the presence of short wavelength, high frequency electron oscillations is presented. It is shown that high frequency oscillations may stabilize a linearly unstable double-humped ion distribution function.     

Coherent acoustic phonon oscillations in semiconductor multiple quantum wells with piezoelectric fields

Large coherent acoustic phonon oscillations were demonstrated using InGaN/GaN multiple quantum wells with piezoelectric fields. With UV femtosecond pulse excitation, photogenerated carriers screened the piezoelectric field and initiated the displacive coherent phonon oscillations. The specific phonon frequency was selected by the coupling between the periodic carrier distribution and the corresponding acoustic phonon mode. The induced acoustic phonon oscillation resulted in piezoelectric field modulation and then caused absorption variation through the quantum confined Franz-Keldysh effect. The wave vector uncertainty due to the finite sample width was found to determine the observed dephasing time.