Kinematics and Physics of Celestial Bodies

We study the mid-infrared photometric properties of a sample of compact star-forming galaxies from the SDSS Data Release 14. The sample includes about 30 000 galaxies. The H_β emission lines with equivalent widths EW(H_β) > 1 nm are observed in the spectra of all selected galaxies. The selected galaxies are compact objects with angular diameters less than 6 arcsec. About 10 000 galaxies were detected by the WISE space telescope at wavelengths of 3.4 and 4.6 μm. A considerable number of galaxies was also detected at wavelengths of 12 and 22 μm. Using these data and the results of observations obtained in the ultraviolet range with the GALEX space telescope, it was shown that the heating of dust in the sample of galaxies is caused by the ultraviolet radiation of massive stars in the star-forming regions. The stellar and ionized-gas emission dominates at wavelengths of 3.4 and 4.6 μm in a majority of galaxies, whereas the dust emission dominates at wavelengths of 12 and 22 μm. In some galaxies with high H_β luminosity, dust emission is observed even at the short wavelength of 3.4 μm, and it has a steep increase in the intensity toward the wavelength of 4.6 μm. This emission is characterized by “red” color (W1 – W2 > 2^m), where W1 and W2 are magnitudes at wavelengths of 3.4 and 4.6 μm, respectively. The probable cause of this emission is the presence of hot dust with a temperature of hundreds of Kelvins. A list of 39 galaxies with such an extremely high W1 – W2 color index is presented.

According to the data of complex 2D observations on the VTT telescope of the solar facula, a 3D model of the solar atmosphere in the facular region was obtained by solving the inverse radiative transfer problem in the Ba II 4554 A line. The magnetic field was estimated using the Stokes V profiles of the Fe I 15648 A line. The influence of magnetic field on photospheric convection was investigated: spatial variations in temperature and velocities at different heights were considered. It is shown that the mutual transformation of the mechanical and thermal energy of the solar plasma into magnetic energy occurs in the layers of the middle photosphere. The integral effect of a small-scale magnetic dynamo leads to lowering the temperature and slowing down the motion of the predominant downward flows in the layers of the middle photosphere in the facular regions with a strong field (greater than 1 kG), while there is an increase in temperature and acceleration of the motion of the predominant upward flows in the layers of the middle photosphere in the facular regions with a weak field (less than 1 kG). It is shown that the magnetic field of the facula stabilizes photospheric convection, and the small-scale magnetic dynamo causes a double temperature inversion in the photospheric layers of the facula.

Comprehensive modeling studies of the processes induced in all geospheres by the passage and explosion of the meteoroid near the city of Lipetsk (Russia) on June 21, 2018, have been conducted. Magnetic, electric, electromagnetic, ionospheric, and seismic effects, as well as the effects of acoustic-gravity waves have been estimated. The magnetic effect of turbulence has been shown to be insignificant. The magnetic effect of the ionospheric currents and the current in the wake of the meteoroid could be substantial (~1 nT). Under the action of an external electric field, a transient current pulse with the strength of current up to 10⁴ A could occur. The electrostatic effect could be accompanied by the accumulation of an electric charge of 1 mC producing the electric field intensity of 0.01–1 MV/m. The flow of the electric current in the wake of the meteoroid could result in the generation of an electromagnetic pulse in the 40–80 kHz band with the electric field intensity of 1–10 V/m. The electromagnetic effect of infrasound has been determined to be significant (1–10 V/m and 1–10 nT). The absorption of the shock wave at ionospheric dynamo region altitudes (100–150 km) could generate secondary atmospheric gravity waves with the 0.1–1 relative amplitude. The passage of the meteoroid acted to produce a plasma wake and noticeable disturbance not only in the lower but also in the upper atmosphere in the range of no less than 1000 km. The possibility of occurrence of the electrophonic effect, the generation of the ion and magnetic sound by infrasound, and the generation of gradient-drift and drift-dissipative instabilities are discussed. A conclusion is drawn that magnetic, electric, and electromagnetic effects dealt with in this paper significantly fill in the gaps in the theory of physical effects produced by meteoroids in the Earth–atmosphere–ionosphere–magnetosphere system. The magnitudes of magnetic, electric, electromagnetic, ionospheric, and acoustic effects were significant. The magnitude of the earthquake caused by the meteoroid explosion did not exceeded 1.7. The mean rate of the fall of celestial bodies similar to the Lipetsk meteoroid is equal to 0.68 yr^–1.

We present the results of computations of the trajectories (the asymptotic latitude and asymptotic longitude) and the magnetic cutoff rigidity of galactic cosmic ray (GCR) particles for the airport Deblin, Poland (geographical latitude 51°33′32′′ N, geographical longitude 21°50′53′′ E) based on the numerical integration of equations of motion of charged particles of cosmic rays in the Earth’s magnetic field. The set of allowed trajectories at a given site on the surface of the Earth is called the asymptotic cone of acceptance The initial distance from the center of the Earth was taken to be 20 km above the Earth’s surface. At about this altitude, most cosmic rays undergo nuclear collisions. Calculations were made for different of models of the International Geomagnetic Reference Field (IGRF) from 1965–2015. The IGRF is an internationally agreed and widely used mathematical model of the Earth’s magnetic field of internal origin. Each constituent model of the IGRF is a set of spherical harmonics of degree n and order m, representing a solution to Laplace’s equation for the magnetic potential arising from sources inside the Earth at a given epoch. In all asymptotic direction calculations, we used sixth-degree expansion of geomagnetic field model. Schmidt normalized spherical harmonic coefficients were taken for the epochs from 1965 to 2015. Knowledge of asymptotic directions and the magnetic rigidity cutoff is important from the point of view of study different classes of cosmic rays variations intensity and anisotropy.