Vol 33, No 2 (2017)

The method for the multicomponent photoionization modeling of the H II region radiation surrounding the starburst knot is presented. The internal structure of the H II region has been determined using the evolutionary model of the superwind bubble from the starburst center. Models of Chevalier and Clegg (1985) and Weaver et al. (1977) have been used to determine the radial distribution of the gas density, the velocity of gas layers, and the temperature in the region of the superwind free expansion and in the cavity, respectively. The chemical content of the internal components of the bubble has been set by the results of the modeling of the evolutionary population synthesis. External components of our models describe a high-density, thin layer of gas formed by the shock wave of stellar superwind from the surrounding gas and a typical H II region, respectively. Input model parameters have been taken from the precalculated evolutionary starburst models based on three types of evolutionary tracks. Evolutionary grids of multicomponent low-metallicity models are calculated. A comparative analysis of the results of their calculation with the observational data has been carried out.

The algorithm of the determination of abundances in atmospheres of stars of spectral classes F, G, and K using fits to the observed spectral lines or selected parts of the blended lines is discussed. The technique allows to determine the parameters of the atmosphere, i.e., gravity, microturbulent velocity, rotational velocity of the star, and abundance of elements, for a given effective temperature of the star. At each stage of the iterative process the model atmosphere is recalculated for a new set of input data. The results of applying the procedure for the analysis of the spectra of the Sun (G2 V) and HD 101348 (G3 V) are discussed.

The propagation of galactic cosmic rays in heliospheric magnetic fields is studied. An approximate solution to the cosmic ray transport equation has been derived on the basis of a method that takes into account the small value of anisotropy of particle angular distribution. The spatial and energy distributions of the cosmic ray intensity and anisotropy have been investigated, and estimates of cosmic ray energy flux have been carried out.

When analyzing the pressure dependences of the aerosol volume scattering coefficient calculated from the measurement data on the geometric albedo of Jupiter obtained in 1993 in the methane absorption bands at 619, 727, and 842 nm, the signs of probable changes in the parameters of aerosol particles in the deep atmospheric layers were detected and the first estimates of the magnitude of these changes were obtained. It has been found that, in the pressure interval from 4 to 14 bar, the effective radius of particles may increase twofold and more (larger than 0.73 μm) and the real part of the refractive index may grow by 10% (from 1.44 and higher) relative to the values of these parameters in the upper atmosphere. If we take into account these changes, we find no signs of aerosol deep in the atmosphere of Jupiter.