Том 101, № 5 (2024)

In the framework of entropic cosmology and Prigozhin’s gravitational theory about the connection between geometry and matter, providing the production of particles in the cosmological fluid, as well as in the assumption of exchange entropy at the event horizon, a one-liquid model of the evolution of a spatially flat, homogeneous and isotropic Universe is constructed. For its construction the energy conservation equation is derived from the first law of thermodynamics taking into account gravitationally induced creation of matter and exchange energy processes on the visible horizon of the Universe. On the basis of the energy equation and the fundamental Friedman equation describing the expansion of the Universe, modified Friedman-Robertson-Walker equations have been constructed in the context of the entropic formalism, designed for modelling various dynamical aspects of the evolution of the Universe taking into account adiabatic creation of matter. Several forms of exchangeable phenomenological non-extensive entropies associated with the region of the apparent cosmological horizon were used in their derivation. The obtained evolutionary model, consistent with the standard Λ-model for cold dark matter, is intended to describe without introducing new fields the accelerated expansion of the late Universe, providing its cosmological history.

The results of a study of a star formation region are presented. S255 IR, where a young high-mass star is forming (20M_•). Observations in H₂O were carried out on RT-22 in Pushchino, and in the OH lines at the Large Radio Telescope in Nance (France). Data observations in the H₂O line at 1.35 cm were used for the period 2017–2023. Our observations in H₂O showed the existence strong flares, especially in 2023. Drift was also observed emission by radial velocity for most spectral details and predominantly in the direction of decreasing radial velocity.

In OH lines 18 cm in 2008 no emission was detected. We observed OH emission in the main lines 1665 and 1667 MHz in 2015, 2023 and 2024. Structures of spectra, degrees of circular and linear polarizations varied greatly during these epoch. However, at the same time the longitudinal magnetic field vectors had predominantly two directions:  relative to the vertical, i. e. almost perpendicular to the jet or along it. Zeeman splitting was detected only in the 1667 MHz line for one pair of features: 2.26 and 2.37 km/s. The amount of splitting 0.11 km/s corresponds to a longitudinal magnetic field value of 0.31 mGs; the field is directed towards the observer.

It is assumed that the appearance of OH maser emission in 2015 associated with an accretion flares. Significant structure changes OH spectra, their degrees of polarization and very strong flares H₂O maser in 2023 may be associated with a new possibility accretion flares in S255 IR.

This study is based on observations of the pulsar B1133+16 conducted on the BSA PRAO antenna array at a frequency of 111 MHz with continuous recording of undetected signal (voltage) in the 2.5 MHz band, providing time resolution 0.2 microseconds. From 30 observing sessions, 570 strong pulses were selected for the subsequent analysis of microstructure parameters. The analysis was performed by computing autocorrelation functions separately for the three components of the mean profile: two extreme main components I and II and for the central weak component S in the profile saddle. For the component S microstructure analysis was performed for the first time. Distributions have been constructed by the following parameters: time scales τ_µ, modulation depth m_µ, and the parameter d, which characterizes the shape of the micropulses. Noticeable differences were found in some parameters for different profile components. The discovered features were interpreted in the model of hollow cone with a central component. It was believed that the radio emission of the extreme components (I and II) is generated by ordinary mode O, and the radio emission of the central component is provided by extraordinary mode X. Under this interpretation the radio emission output heights above the polar cap, were estimated to be 45 and 280 km for the X and O modes, respectively. A noticeable deformation of the X mode emission cone relative to the central component S was mentioned. Considerations are presented that point to the spatial structure of the secondary plasma flow, elongated along the meridians of the magnetic field.

The article presents the results of determining the parameters of the Earth’s gravitational field from gradiometric measurements in the geocentric terrestrial coordinate system. The calculations were performed using the regularization method, according to which a regularization matrix multiplied by the regularization parameter is added to the matrix of normal equations. As a result of calculations for various regularization parameters, corrections to harmonic coefficients of degree and order 200 and 201 were obtained, presented in the article in the form of graphs. Based on the corrections obtained, the power-law variances presented in Tables 1 and 2 are calculated.