I will discuss possibility of negative radiation pressure e.g. from astronomical objects and how we could observe it, also its different potential applications like medical and computational e.g. 2WQC (two-way quantum computers). Photon sources create positive radiation pressure p=/c being toward surface, pushing it. However, generally it could be also outside surface: pulling it, for example using a process which in T-symmetry perspective (H -> -H) creates positive radiation pressure - like synchrotron radiation generated by charge travelling on a circle, which also does it in T-symmetry perspective. Similar T/CPT symmetry argument suggests that black holes might generate negative radiation pressure. I also will suggest related solution to ANITA anomaly.

TBA

TBA

Mars is a desert world with a surface covered by loose particles: sand, dust, gravel. This loose sediment is called regolith and is one of the most important elements in planetary exploration. On Mars, these small particles are transported by wind. Dust in the atmosphere is responsible for global dust storms that occur every few years on Mars. Sand and gravel form the most common and striking landforms on the planet: dunes, ripples, and streaks. Aeolian (wind) processes reveal changes in the Martian atmosphere and help to understand what happens on the surface on Mars.

The first extended radio sources were discovered in the 1970s, and Giant Radio Galaxies (GRGs) remain among the largest single structures formed by galaxies. They can grow up to Mpc scale and are extremely rare compared to normal-sized radio galaxies. The new generation of radio interferometers has significantly changed our understanding of the evolution of these extended radio sources. As of 10th November 2025, the total number of confirmed and candidate GRGs has reached around 12,682. The advent of low-frequency telescopes such as LOFAR and uGMRT has made it possible to study the spectral and dynamical ages of GRGs with better sensitivity and spatial resolution, matching those of high-frequency arrays like the VLA, ASKAP, and MeerKAT. These facilities allow the construction of broadband radio spectra from 150 MHz to 8–10 GHz with matched resolution and sensitivity. Although collecting and processing such data is time-consuming, the resulting astrophysical insights are of great significance. In this seminar, I will present an overview of ongoing GRG research and a multi-frequency study of eight GRGs, each exceeding 2 Mpc, based on dedicated LOFAR, uGMRT and VLA observations collected over the last four years as part of a long-term project. I will also highlight two rare discoveries that emerged from this project.

The general population of radio galaxies includes several classes of peculiar objects. These include giant radio galaxies (GRGs) with linear sizes greater than 0.7 Mpc and double-double radio galaxies (DDRGs) that show signs of recurrent jet-formation activity. Observations and models developed in recent decades suggest that recurrent activity, among other factors, may stimulate GRG growth. The connection between the two classes of objects is still poorly understood, however, and few of the known giant DDRGs are studied thoroughly so far. The three selected giant DDRGs are J1021+1216, J1528+0544, and J2345–0449. The collection of radio maps, obtained from archival data sets and dedicated interferometric observations, together with the basic parameters of the sources, such as independent measurements of the flux density in the inner and outer lobes, measurements of the linear sizes, and the axial ratio of the lobes facilitate an in-depth modeling of the objects. By determining the properties of these radio galaxies and their environments, a comprehensive image of the processes influencing their evolution was derived. In this seminar, I will present the results of the synchrotron age modeling performed with the Broadband Radio Astronomy ToolS software and of the DYNAGE dynamical modeling.

Recent observations of the galactic CRs indicated the presence of leptons in their content with energies up to ~ 1 TeV. Last precise measurements by the Alpha Magnetic Spectrometer (AMS-02) indicated that fluxes of CR electrons and positrons have different energy distributions, and they both deviate from the (almost) single power-law distribution typical for CR hadrons. Besides, in the high energy part of the spectrum, E > 20 GeV, spectral index for positrons is much harder than for electrons. The positron fraction also varies with energy, showing the obvious excess at higher energies. Currently, there is no generally accepted theory explaining the origin of positrons in the galactic CR flux, especially the hardness of their energy distribution. The hypotheses aimed to explain such observational data can be classified in three types: annihilation of dark matter particles; acceleration in the nearby astrophysical objects; result of CR nuclei interaction with ICM gas. Our pilot study with method of kinetic Particle-In-Cell simulations has shown, that processes of the lepton acceleration are (or may be with high probability) charge-dependent: positrons are energized much more efficiently than electrons, thah can explain the excess of high energy positrons in the flux CR leptons. Such a result is consistent with the hypothese acceleration at the nearby objects.