Surface Brightness Gradients Produced by the Ring Waves of Star Formation

We compute surface brightness profiles of galactic disks for outwardly propagating waves of star formation with a view to investigate the stellar populations in ring galaxies. We consider two mechanisms which can create outwardly propagating star forming rings in a purely gaseous disk --- a self-induced wave and a density wave. We show that the surface brightness profiles produced by both scenarios of ring formation are similar and are strongly sensitive to the velocity of the wave. The results of our computations are compared with the observational quantities sensitive to the young and old stellar populations in the ring galaxies A0035-335 (the Cartwheel galaxy) and VIIZw466. The best fit to the observed radial H_alpha surface brightness distribution in the Cartwheel galaxy is obtained for a wave velocity of about 90 km/s. The red continuum brightness of the ring can be fully explained by the evolving stars present in the trailing part of the wave. However the red continuum brightness in regions internal to the ring indicates that the wave of star formation propagates in a pre-existing stellar disk in the Cartwheel. The H_alpha and K-band surface brightness profiles in VIIZw466 match the values expected from stellar populations produced by a wave of star formation propagating in a purely gaseous disk very well. We conclude that VIIZw466 is probably experiencing the first event of star formation in the disk.Comment: Uses aas2pp4.sty and epsfig.sty, 15 pages To appear in Astrophysical Journal, March 10, 199

Chemical Abundance Gradients in the Star-Forming Ring Galaxies

Ring waves of star formation, propagating outwardly in the galactic disks, leave chemical abundance gradients in their wakes. We show that the relative [Fe/O] abundance gradients in ring galaxies can be used as a tool for determining the role of the SNIa explosions in their chemical enrichment. We consider two mechanisms which can create outwardly propagating star forming rings in a purely gaseous disk -- a self-induced wave and a density wave, and demonstrate that the radial distribution of the relative [Fe/O] abundance gradients does not depend on the particular mechanism of the wave formation or on the parameters of the star-forming process. We show that the [Fe/O] profile is determined by the velocity of the wave, initial mass function, and the initial chemical composition of the star-forming gas. If the role of SNIa explosions is negligible in the chemical enrichment, the ratio [Fe/O] remains constant throughout the galactic disk with a steep gradient at the wave front. If SNIa stars are important in the production of cosmic iron, the [Fe/O] ratio has gradient in the wake of the star-forming wave with the value depending on the frequency of SNIa explosions.Comment: Uses aas2pp4.sty and epsfig.sty, 7 pages including one figure To appear in Astrophysical Journa

Formation of Plumes in Head-on Collisions of Galaxies

Using N-body and SPH modeling we perform 3D numerical simulations of head-on collisions between gas rich disk galaxies, including collisions between counter-rotating disks and off-center collisions. Pure stellar intruders do not produce gaseous plumes similar to those seen in the Cartwheel and VII Zw466 complexes of interacting galaxies; the presence of gas in an intruder galaxy and radiative cooling are important for the formation of a gaseous plume extending from the disk of a target galaxy. A noticeable plume structure can be formed if the mass of an intruder is a few percent of the mass of the primary. The halo of the intruder is stripped in the collision, and dispersed particles form a broad stellar bridge connecting the two galaxies. The fraction of the intruder's halo dispersed in the collision depends on the total mass of the intruder, and low-mass intruders lose most of their mass.Comment: 15 pages, 14 figures in GIF. To appear ApJ. Vol. 505 #

Origin of TeV Galactic Cosmic Rays

We consider a possibility of identification of sources of cosmic rays (CR) of the energy above 1 TeV via observation of degree-scale extended gamma-ray emission which traces the locations of recent sources in the Galaxy. Such emission in the energy band above 100 GeV is produced by CR nuclei and electrons released by the sources and spreading into the interstellar medium. We use the data from the Fermi gamma-ray telescope to locate the degree-scale 100 GeV gamma-ray sources. We find that the number of such sources and their overall power match to those expected when CRs injection events happen every ~100 yr in portions of ~1e50 erg. We find that most of the sources are associated to pulsars with spin down age less than ~30 kyr and hence to the recent supernova explosions. This supports the hypothesis of supernova origin of Galactic CRs. We notice that the degree-scale extended emission does not surround shell-like supernova remnants without pulsars. Based on this observation, we argue that the presence of the pulsar is essential for the CR acceleration process. We expect that a significant fraction of the degree-scale sources should be detectable as extended sources with km3-scale neutrino detectors.Comment: 14 pages, 14 figures, accepted for publication in Phys.Rev.

The using of quality indicators of Scots pine’s seeds for bioindication of anthropogenic pollution

The quality of Scots pine’s seeds (Pinus sylvestris L.) was analyzed in conditions of industrial emissions magnesite productionПроанализировано качество семян сосны обыкновенной (Pinus sylvestris L.) в условиях промышленных выбросов магнезитового производств

Psychology features of older people in tourism

On the basis of the analysis of elderly people’s tourist activity the factors determining the organization of tourist activity have been revealed. The psychological features of elderly tourists, causing their consumer behavior, both in the process of purchasing tourist permits, and the General attitude of the consumer to tourism have been considered. It has been established that stereotypes, the environment of tourist products and the emotional sphere of the elderly tourist are the main factors, on the basis of which the decision on travel or refusal to travel is made. The model of interaction process of psychological features of elderly tourists with stages of tourist activity has been presented. The dependence between the primary experience of tourism and the subsequent recreational needs refl cts the importance of studying the psychology of elderly tourists to ensure the frequency of consumption of tourist products

Scots pine as a bioindicator of the aerotechnogenic pollution

The investigations of the conditions of the Scots pine stands in the conditions of the aerotechnogenic emissions of the magnesite industry were provided. It is shown that the weak level of pollution had an negative impact on both the vegetative and generative system of Scots pine. It is concluded that the pine species had high sensibility to the alkaline aeropollutantsПроведены исследования состояния культур сосны обыкновенной (Pinus sylvestris L.) в условиях аэротехногенных выбросов магнезитового производства. Показано, что даже слабый уровень загрязнения негативно влияет как на вегетативную, так и на генеративную системы сосны. Сделан вывод о высокой чувствительности данного вида хвойных к щелочным аэрополлютанта

Molecular genetic characteristics of Darevskia portschinskii lizard populations based on microsatellite markers analysis

The Caucasian rock lizard species Darevskia portschinskii is one of the bisexual species participating in interspecific hybridisation as the paternal ancestor with the maternal ancestors D. mixta and D. raddei resulting in the successful formation of the parthenogenetic D. dahli and D. rostombekowi, respectively. Populations of D. portschinskii have been previously divided into two subspecies, D. p. portschinskii and D. p. nigrita according to their geographical distribution and the morphological data, but they have not been characterised genetically. Here, we used ten microsatellite markers to determine the genetic structure of the D. portschinskii populations. The utility of the developed microsatellite markers for investigating the genetic variability within and among populations with a heterogeneous spatial distribution was demonstrated. Our results showed that the intra- and interspecific differentiation of the studied populations were consistent with the morphological data on the subspecies status of the D. p. portschinskii and D. p. nigrita populations. A potential applicability of the developed microsatellite markers to study genetic diversity of Darevskia species and subspecies complexes is suggested

Gravitational stability and dynamical overheating of stellar disks of galaxies

We use the marginal stability condition for galactic disks and the stellar velocity dispersion data published by different authors to place upper limits on the disk local surface density at two radial scalelengths $R=2h$. Extrapolating these estimates, we constrain the total mass of the disks and compare these estimates to those based on the photometry and color of stellar populations. The comparison reveals that the stellar disks of most of spiral galaxies in our sample cannot be substantially overheated and are therefore unlikely to have experienced a significant merging event in their history. The same conclusion applies to some, but not all of the S0 galaxies we consider. However, a substantial part of the early type galaxies do show the stellar velocity dispersion well in excess of the gravitational stability threshold suggesting a major merger event in the past. We find dynamically overheated disks among both seemingly isolated galaxies and those forming pairs. The ratio of the marginal stability disk mass estimate to the total galaxy mass within four radial scalelengths remains within a range of 0.4---0.8. We see no evidence for a noticeable running of this ratio with either the morphological type or color index.Comment: 25 pages, 5 figures, accepted to Astronomy Letter

Dynamics of Gaseous Disks in a Non-axisymmetric Dark Halo

The dynamics of a galactic disk in a non-axisymmetric (triaxial) dark halo is studied in detail using high-resolution, numerical, hydrodynamical models. A long-lived, two-armed spiral pattern is generated for a wide range of parameters. The spiral structure is global, and the number of turns can be two or three, depending on the model parameters. The morphology and kinematics of the spiral pattern are studied as functions of the halo and disk parameters. The spiral structure rotates slowly, and its angular velocity varies quasi-periodically. Models with differing relative halo masses, halo semi-axis ratios, distributions of matter in the disk, Mach numbers in the gaseous component, and angular rotational velocities of their halos are considered.Comment: 22 pages, 11 figure