Expansive actions on uniform spaces and surjunctive maps

We present a uniform version of a result of M. Gromov on the surjunctivity of maps commuting with expansive group actions and discuss several applications. We prove in particular that for any group $\Gamma$ and any field \K, the space of $\Gamma$-marked groups $G$ such that the group algebra \K[G] is stably finite is compact.Comment: 21 page

Investigation of the composition of the Luna 16 lunar sample

The concentrations of aluminum, manganese, sodium, chromium, iron, cobalt, and 12 rare earth elements were determined by neutron activation analysis using slow neutrons. Oxygen and silicon were determined using a fast neutron generator. Mossbauer spectroscopy was used to investigate iron compounds in Luna 16 regolith samples from the upper part of the core

Exploring the circumstellar environment of the young eruptive star V2492 Cyg

Context. V2492 Cyg is a young eruptive star that went into outburst in 2010. The near-infrared color changes observed since the outburst peak suggest that the source belongs to a newly defined sub-class of young eruptive stars, where time-dependent accretion and variable line-of-sight extinction play a combined role in the flux changes. Aims. In order to learn about the origin of the light variations and to explore the circumstellar and interstellar environment of V2492 Cyg, we monitored the source at ten different wavelengths, between 0.55 \mu m and 2.2 \mu m from the ground and between 3.6 \mu m and 160 \mu m from space. Methods. We analyze the light curves and study the color-color diagrams via comparison with the standard reddening path. We examine the structure of the molecular cloud hosting V2492 Cyg by computing temperature and optical depth maps from the far-infrared data. Results. We find that the shapes of the light curves at different wavelengths are strictly self-similar and that the observed variability is related to a single physical process, most likely variable extinction. We suggest that the central source is episodically occulted by a dense dust cloud in the inner disk, and, based on the invariability of the far-infrared fluxes, we propose that it is a long-lived rather than a transient structure. In some respects, V2492 Cyg can be regarded as a young, embedded analog of UX Orionis-type stars. Conclusions. The example of V2492 Cyg demonstrates that the light variations of young eruptive stars are not exclusively related to changing accretion. The variability provided information on an azimuthally asymmetric structural element in the inner disk. Such an asymmetric density distribution in the terrestrial zone may also have consequences for the initial conditions of planet formation.Comment: 9 pages, 7 figures, 2 online tables, accepted for publication in A&

How Cosmic Web Environment Affects Galaxy Quenching Across Cosmic Time

We investigate how cosmic web structures affect galaxy quenching in the IllustrisTNG (TNG-100) cosmological simulations by reconstructing the cosmic web in each snapshot using the DisPerSE framework. We measure the distance from each galaxy with stellar mass log(M*/Msun)>=8 to the nearest node (dnode) and the nearest filament spine (dfil) and study the dependence of both median specific star formation rate () and median gas fraction () on these distances. We find that of galaxies is only dependent on cosmic web environment at z<2, with the dependence increasing with time. At z<=0.5, 8<=log(M*/Msun)<9 galaxies are quenched at dnode<1 Mpc, and significantly star formation-suppressed at dfil<1 Mpc, trends which are driven mostly by satellite galaxies. At z of log(M*/Msun)=10 galaxies actually experience an upturn in at dnode<0.2 Mpc (this is caused by both satellites and centrals). Much of this cosmic web-dependence of star formation activity can be explained by the evolution in . Our results suggest that in the past ~10 Gyr, low-mass satellites are quenched by rapid gas stripping in dense environments near nodes and gradual gas starvation in intermediate-density environments near filaments, while at earlier times cosmic web structures efficiently channeled cold gas into most galaxies. State-of-the-art ongoing spectroscopic surveys such as SDSS and DESI, as well as those planned with JWST and Roman are required to test our predictions against observations.Comment: 5 Figures, 15 pages, submitted to ApJ Letter

Lower leg fractures treated with an external fixator at the Department of Orthopedics and Traumatology of the Clinical Hospital Center of Kosovska Mitrovica

IIntroduction: Fractures of the lower leg are frequent fractures of long bones that are of great importance in traumatology. The role of external fixation (SF) as a type of surgical treatment is significant and widely applied. There are 3 methods of using SF to treat tibial fractures: SF as primary and definitive treatment, SF combined with internal fixation, and conversion of SF to internal fixation. Objective: To show the possibilities of SF as a definitive way of treating lower leg fractures. Methods: In our paper, we analyzed 254 lower leg fractures treated with SF according to Mitković M20, which were treated at the Department of Orthopedics and Traumatology of CHC Kosovska Mitrovica. This series included 172 men or 68% of the total number of patients, and 83 or 32% women. Results: The average age of patients treated with this method is between the third and fourth decades of life. Falling on the leg with twisting of the table or the entire lower part of the leg is the most common type and cause of injuries in 69%. A closed lower leg fracture was diagnosed in 220 patients (A AO 59.%, B AO 26% and C AO 15%). Adequate position of the bone fragments was achieved by the closed reposition method in 190 (%), the average healing time was 18.4 weeks. In 93% of patients, we achieved bone union. Conclusion: The simple placement technique, the simplicity of the instrumentation, the wide range of indications where SF can be used, have led to the fact that it is a type of surgical treatment of great importance for lower leg fractures in small areas

Filaments of The Slime Mold Cosmic Web And How They Affect Galaxy Evolution

We present a novel method for identifying cosmic web filaments using the IllustrisTNG (TNG100) cosmological simulations and investigate the impact of filaments on galaxies. We compare the use of cosmic density field estimates from the Delaunay Tessellation Field Estimator (DTFE) and the Monte Carlo Physarum Machine (MCPM), which is inspired by the slime mold organism, in the DisPerSE structure identification framework. The MCPM-based reconstruction identifies filaments with higher fidelity, finding more low-prominence/diffuse filaments and better tracing the true underlying matter distribution than the DTFE-based reconstruction. Using our new filament catalogs, we find that most galaxies are located within 1.5-2.5 Mpc of a filamentary spine, with little change in the median specific star formation rate and the median galactic gas fraction with distance to the nearest filament. Instead, we introduce the filament line density, {\Sigma}fil(MCPM), as the total MCPM overdensity per unit length of a local filament segment, and find that this parameter is a superior predictor of galactic gas supply and quenching. Our results indicate that most galaxies are quenched and gas-poor near high-line density filaments at z10.5 galaxies is mainly driven by mass, while lower-mass galaxies are significantly affected by the filament line density. In high-line density filaments, satellites are strongly quenched, whereas centrals have reduced star formation, but not gas fraction, at z<=0.5. We discuss the prospect of applying our new filament identification method to galaxy surveys with SDSS, DESI, Subaru PFS, etc. to elucidate the effect of large-scale structure on galaxy formation.Comment: Submitted to ApJ, comments welcome. Data available at https://github.com/farhantasy/CosmicWeb-Galaxies

An Efficient Partitioning Oracle for Bounded-Treewidth Graphs

Partitioning oracles were introduced by Hassidim et al. (FOCS 2009) as a generic tool for constant-time algorithms. For any epsilon > 0, a partitioning oracle provides query access to a fixed partition of the input bounded-degree minor-free graph, in which every component has size poly(1/epsilon), and the number of edges removed is at most epsilon*n, where n is the number of vertices in the graph. However, the oracle of Hassidimet al. makes an exponential number of queries to the input graph to answer every query about the partition. In this paper, we construct an efficient partitioning oracle for graphs with constant treewidth. The oracle makes only O(poly(1/epsilon)) queries to the input graph to answer each query about the partition. Examples of bounded-treewidth graph classes include k-outerplanar graphs for fixed k, series-parallel graphs, cactus graphs, and pseudoforests. Our oracle yields poly(1/epsilon)-time property testing algorithms for membership in these classes of graphs. Another application of the oracle is a poly(1/epsilon)-time algorithm that approximates the maximum matching size, the minimum vertex cover size, and the minimum dominating set size up to an additive epsilon*n in graphs with bounded treewidth. Finally, the oracle can be used to test in poly(1/epsilon) time whether the input bounded-treewidth graph is k-colorable or perfect.Comment: Full version of a paper to appear in RANDOM 201

On Quasi-biennial oscillations in chromospheric macrospicules and their potential relation to global solar magnetic field

This study aims to provide further evidence for the potential influence of the global solar magnetic field on localised chromospheric jets, the macrospicules (MS). To find a connection between the long-term variation of properties of MS and other solar activity proxies, including e.g. the temporal variation of the frequency shift of solar global oscillations, sunspot area, etc., a database overarching seven years of observations was built up. This database contains 362 MS, based on observations at the 30.4 nm of the Atmospheric Imaging Assembly (AIA) on-board the Solar Dynamics Observatory (SDO). Three of the five investigated physical properties of MS show a clear long-term temporal variation after smoothing the raw data. Wavelet analysis of the temporal variation of maximum length, maximum area and average velocity is carried out. The results reveal a strong pattern of periodicities at around 2-year (also referred to as Quasi-Biennial Oscillations -- QBOs). Comparison to solar activity proxies, that also possess the properties of QBOs, provides some interesting features: the minima and maxima of QBOs of MS properties occur at around the same epoch as the minima and maxima of these activity proxies. For most of the time span investigated, the oscillations are out-of-phase. This out-of-phase behaviour was also corroborated by a cross-correlation analysis. These results suggest that the physical processes, that generate and drive the long-term evolution of the global solar activity proxies, may be coupled to the short-term local physical processes driving the macrospicules, and, therefore modulate the properties of local dynamics