СНТ ФФ

Reactive oxygen species (ROS) are omnipresent inside living cells, and their concentration can decide whether a cell survives or dies, shaping the fate of entire organisms. Therefore, there is a strong need to measure the level of ROS in living cells, and to be able to rise or decrease this level accordingly. In this lecture, I will show how luminescent nanocrystals can serve as sensitive ROS sensors in aqueous solutions and biological environments. We will also look at the underlying physics that makes this technology possible, revealing how nanoparticles can be used to probe and influence complex biological processes.

Borromean states are the bound states of a system of N>2 particles in which any lower number of particles is unbound. These states include, but are not limited to, Efimov physics. In this talk, we will present several examples of the low-dimensional Borromean states.

Additive technologies (3D printing) are currently developing extremely rapidly, driven by their practical applications. Despite significant progress, they still require further improvement. This report will provide an overview of the main methods of 3D printing of metal materials and approaches to overcoming existing limitations.

In this talk, I will briefly review what gravitational waves are, how they are generated in various astrophysical environments, how scientists searched for them and ultimately detected them in 2015, thereby opening a new window on the cosmos.

We study spins coupled to an external electromagnetic field with a fixed frequency, a single polarization mode, and a well-defined propagation direction. Under these conditions, the field mediates an effectiveIsing-type interaction between the spins. At the same time, coupling to the field induces decoherence. This model reduces to the standard dephasing model described in J. Luczka, Physica A 167, 919 (1990).

H II regions are large clouds of low-density ionized hydrogen (with densities ranging from a few to thousands of particles per cm³) with star-forming regions inside. Short-lived (a few million years), bright O–B class stars formed in these regions continuously emit ultraviolet radiation, which keeps the surrounding gas in an ionized state. The H II regions themselves, whose sizes can range from a few to hundreds of parsecs, are usually parts of giant molecular clouds.

These regions have a wide variety of shapes because the distribution of stars and gas within them is uneven. They often appear composed of clumps and filaments, and sometimes form bizarre shapes. Over a period of several million years, thousands of stars are born within H II regions; afterward, powerful stellar winds from these stars, and later supernova explosions from the most massive among them, blow the gas out of the H II region, forming bubbles with a young star cluster inside.