On the radiative and thermodynamic properties of the cosmic radiations using COBE FIRAS instrument data: I. Cosmic microwave background radiation

Abstract

Use formulas to describe the monopole and dipole spectra of the Cosmic Microwave Background (CMB) radiation, the exact expressions for the temperature dependences of the radiative and thermodynamic functions, such as the total radiation power per unit area, total energy density, number density of photons, Helmholtz free energy density, entropy density, heat capacity at constant volume, pressure, enthalpy density, and internal energy density in the finite range of frequencies v 1 ≤ v ≤ v 2 are obtained. Since the dependence of temperature upon the redshift z is known, the obtained expressions can be simply presented in z representation.Utilizing experimental data for the monopole and dipole spectra measured by the COBE FIRAS instrument in the 60 -600 GHz frequency interval at the temperature T = 2.728 K, the values of the radiative and thermodynamic functions, as well as the radiation density constant a and the Stefan-Boltzmann constant σ are calculated. In the case of the dipole spectrum, the constants a and σ, and the radiative and thermodynamic properties of the CMB radiation are obtained using the mean amplitude T amp =3.369m K. It is shown that the Doppler shift leads to a renormalization of the radiation density constant a, the Stefan-Boltzmann constant σ, and the corresponding constants for the thermodynamic functions. The radiative and thermodynamic properties of the Cosmic Microwave Background radiation for the monopole and dipole spectra at the redshift z ≈ 1089 are calculated.

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Impact of generalized polytropic equation of state on charged anisotropic polytropes

“…On varying parameters d, h and α o , masses of eight different stars were regained given in Table 1. The acceptable values for ρ 0 and P r 0 are given in Table 1 by fixing α 1 = 0.931 and = 7.5756 × 10 −16 [32]. Table 2 contains varying values of ρ, P r , m, E 2 and υ 2 from central point to boundary of stars.…”

Polylogarithmic Representation of Radiative and Thermodynamic Properties of Thermal Radiation in a Given Spectral Range: II. Real-Body Radiation

“…In conclusion of this paragraph, it is essential to note that the analytical expressions derived above in the case of black-body radiation, when 1 and 0 0   a a i , take a well-known expressions [48].…”

“…is the total energy density of blackbody radiation in the finite frequency range of the spectrum [48].…”