A wide range of information on the characteristics of various landforms on different planetary bodies has been obtained from exploration missions conducted over the last few decades. Indictors of tectonic, volcanic, glacial, fluvial, and lacustrine activities were found on several solid surface bodies. Under the Planetary Science course at Eötvös Loránd University of Sciences (ELTE), a collaboration on educational methodologies between the Astronomy and Earth Science departments has been developed. The presentation modes were shaped to make BSc and MSc students familiar with the research methods and approaches used to address specific questions in this domain. A comparative evaluation of the surface landforms, along with their background characteristics (like gravity, temperature range, atmospheres, solid surface material composition), was also performed.

The whole curriculum was built based on groups of processes and surface conditions and not on planetary bodies to compare the same process under different environments. The main messages encouraged the students to integrate current knowledge with concepts from other classical university courses like physics, chemistry, geography, petrology, etc., while also pointing to existing knowledge gaps to be discovered in the future. As an additional optional part of the curriculum, students could suggest specific test types or even missions to clarify these unknown aspects (related physics and Earth science subjects are indicated in brackets). Details of the curriculum will be presented at the meeting.

Liquid water availability is an important aspect of Mars habitability studies; however, current conditions allow only transient, localized liquid formation. Perchlorate salts have been identified across Martian latitudes and might deliquesce under ideal conditions. Deliquescence occurs when temperature and relative humidity exceed salt-specific thresholds. Atmospheric dust shapes near-surface microclimates where brine formation is possible and understanding how dust conditions influence deliquescence is essential for identifying when and where brines may form on Mars.

I used the Mars Climate Database v6.1 to model near-surface conditions in three climate scenarios. “Climatology” scenario represents a standard Martian year; “Warm” scenario sets dust opacity to the observed maximum (excluding global dust storms); “Cold” scenario corresponds to a clear atmosphere with dust opacity set to the minimum observed over Mars years 24-35. The model ran on a 3.75° x 5.625° latitude-longitude grid for one year. I selected the region where the overall deliquescence chance was the highest, between 73.125° W - 5.625° W and 33.75° N – 71.25° N. To compare the possibility of deliquescence between scenarios, I calculated the percentage of ideal days per year.

In the climatology scenario, deliquescence probability was the highest at 10 PM =–12 AM, with lower chances at 2 AM and 6 AM, and a secondary peak at 4 AM. In the warm scenario, the maximum probability occurred at 2 AM–4 AM, followed by a sharp decline. Between 6 PM–12 AM, the probability increased gradually. In the cold scenario, the probability increased after 8 PM, peaking at 12 AM, with lower values at 2 AM and 6 AM, and a small peak at 4 AM. Overall, the warm scenario shifted the peak to later in the night. Cold and climatology scenarios behaved similarly, with climatology yielding more ideal days except for 12 AM.

A combined rock magnetic study and scanning electron microscopy (SEM) were conducted on the NWA11469 carbonaceous chondrite. The studied meteorite was purchased in 2016 in Mauritania, and no detailed analysis of its magnetic mineralogy has yet been published. This study aims to identify the magnetic minerals in NWA 11469 by integrating SEM observations with mineral information inferred from rock magnetic experiments, providing a foundation for future magnetic investigations. Rock magnetic measurements, including hysteresis, IRM acquisition, and thermomagnetic analyses, were performed using an MMVFTB at the University of Burgos. Complementary mineralogical observations were conducted with a JEOL JSM-6480LAII SEM–EDS at Kobe University. Hysteresis measurements of NWA 11469 show a “pot-bellied” shape consistent with mixture grains and dominant MD grains, supported by Day-plot Mrs/Ms = 0.04–0.1; Hcr/Hc = 4.5–5). IRM data showed that 70–80% of the magnetic contributors saturate below 300 mT, indicating low-coercivity phases (magnetite/Fe–Ni), while 20–30% reflect high-coercivity components likely related to, e.g., goethite. Thermomagnetic curves exhibit inflection points near 580 °C and 800 °C, attributed to major Fe phases, and show irreversible behavior, suggesting oxidation-related mineral (e.g., magnetite) formation. SEM-EDS observations confirm kamacite, taenite, pyrrhotite, goethite, and ferrihydrite, but no magnetite was detected. Some discrepancies emerged between the magnetic and SEM–EDS datasets. Goethite and pyrrhotite, although clearly recognized by SEM/EDS, were not observed during the thermomagnetic experiments, likely because their weak magnetization was masked by the strongly magnetic Fe–Ni alloys. Conversely, magnetite was not verified by SEM, likely because its nanometric SD-sized grains fell below the SEM resolution limit. These discrepancies emphasize the complementary strengths of the two approaches: magnetic methods can detect nanoscale contributors that are hidden from SEM, whereas SEM–EDS provides direct mineral identification. Integrating both datasets, therefore, yields a more comprehensive understanding of the mixed magnetic mineral assemblages in NWA 11469.

The baryonic Tully–Fisher relation logM_bar=c+blogV_flat links the baryonic mass of spiral-galaxies with their asymptotic velocity. Flat rotation curves suggest extra-gravity at galactic scales, which is explained by dark matter. However, astrophysicists point to facts/data that contradict the DM-hypothesis (P.Kroupa). Instead, the MOND-model is advocated, which requires b=4. M_bar includes stars, atomic/molecular gas, and HI/HeI/H₂; for dwarfs, HII-component is important (intergalactic radiation ionizes, as N.Gnedin notes). Сonducting calculations is hard and requires assumptions/modeling; in [1] slope b≈3 was obtained for spirals (V_flat≈45...280km/s). Slope b=2 appears in modeling [2;App.G] (except for dwarfs); this indicates F~M_bar/R gravity;.This is possible for one 5D-variant of Teleparallelism with 4th-order gravity and expanding brane-universe [3]: Newton's law transforms to F/m=GM/(LR) when R>L (L is brane's co-moving thickness along the extra-dimension). This model, called MOGA, unlike MOND, preserves the momentum/angular momentum and stability of three-body systems (Toxvaerd S. arXiv:2512.03823; MOdifiedGravityAttraction).

For thin (SO₂-symmetry; 1/R-model) disks, the force/acceleration in the disk-plane, at radius R, depends on the mass M_R inside R: F(R)/m=GM_R/(LR); on the axis (uniform discs, radius a; 'test-mass' m): F(Z)/m=GMZ/(La²) ln(1+a²/Z²). For balls/bulges, one finds (let GMm/L=1):
F(R)=3/(8a){a/R+R/a–0.5(a/R–R/a)² ln[(R+a)/|R–a|]}=R/a²{1–(R/a)²/5–...–3(R/a)²ⁿ/[(2n–1)(2n+1)(2n+3)]–...}=1/R{1–(a/R)²/5–...}.

Logarithmic potential growth stops when "underdensities" appear, and voids should be objects with negative masses. Our MW-galaxy resides in the KBC-void (among the largest—redshift z is small!) with a shift from its center. Defocussing caused by the KBC-void provides some extra-dipoles (redshift-dependent).

1. Ponomareva A.A. etal. MNRAS.474(2018)4366(hal-02117129f).
2. Valageas P., Schaeffer R. Astron.Astrophys.345(1999)329(arXiv:astro-ph/9812213).
3. Zhogin I.L. Space,Time&Fund.Inter.#2(2025)40(stfi.ru/journal/STFI_2025_02/STFI_2025_02_Zhogin.pdf).

In this work, we investigate the role of equation of state (EOS) parameters in governing the complexity of static, self-gravitating stellar systems. Employing Herrera’s definition of complexity for static, spherically symmetric configurations within the framework of general relativity [L. Herrera, Phys. Rev. D 97, 044010 (2018)], we study three anisotropic stellar models constructed using the Vaidya–Tikekar background geometry together with different equations of state. The complexity factor provides a useful tool for probing the internal structure of self-gravitating astrophysical objects. For static, spherically symmetric fluid distributions with anisotropic pressure, complexity is fundamentally associated with energy density inhomogeneity and the anisotropic distribution of stresses. The complexity factor, defined through the orthogonal splitting of the Riemann tensor, quantifies the interplay between pressure anisotropy and density inhomogeneity within the system.

The Vaidya–Tikekar metric is an important exact solution of Einstein’s field equations that is widely used in relativistic astrophysics to model compact stellar objects such as neutron stars and strange stars. In this model, the interior spacetime of a static, spherically symmetric star is assumed to be pseudo-spheroidal rather than perfectly spherical. The Vaidya–Tikekar metric, previously shown to effectively describe compact and dense stellar objects, is adopted as the underlying spacetime geometry.

In this model, we perform a systematic analysis of the impact of EOS parameters on the complexity factor and its individual contributions. Our results demonstrate a strong dependence of the complexity factor on the EOS parameters. In particular, we observe that the complexity of anisotropic stellar configurations increases monotonically with increasing EOS parameters for all equations of state considered. Using current observational data of the pulsar 4U-1608, we show the impact of the EOS parameter in our model, supported by graphical depictions. These findings underscore the crucial influence of the equation of state on the structural complexity and internal organization of relativistic compact stars.

We investigate the physical relationship between the open clusters Berkeley 6 (Be 6) and S1 using astrometric and photometric data from Gaia Data Release 3 (DR3). Previous studies have suggested that S1 may be a physical companion or substructure associated with Berkeley 6, motivating a detailed kinematic and photometric comparison. We analyze stellar proper motions, parallaxes, and Gaia G, BP, and RP photometry within a spatial region encompassing both clusters.

Probable cluster members are identified using Vector Point Diagrams (VPDs) combined with the HDBSCAN density-based clustering algorithm applied in proper-motion space, allowing probabilistic membership determination while minimizing field-star contamination. High-confidence members are subsequently examined through color–magnitude diagrams (CMDs) constructed from Gaia photometry. The CMDs of both groups reveal a well-defined and nearly identical main sequence, with no statistically significant differences in turn-off features or sequence dispersion.

Further constraints are obtained via manual isochrone fitting using PARSEC stellar evolution models. Although the fit is not exact—owing to observational scatter and residual field contamination—a single isochrone provides a reasonable and consistent representation of the combined stellar population. The derived parameters suggest an age of approximately 200 Myr, sub-solar metallicity (Z ≈ 0.008), and a heliocentric distance of about 2.9 kpc.

The strong agreement in proper-motion distributions, CMD morphology, and broadly consistent physical parameters indicates that Berkeley 6 and S1 are unlikely to be independent clusters, instead representing different regions or substructures of a single, extended open cluster. This study demonstrates that the combined use of Gaia DR3 astrometry and HDBSCAN-based membership selection is an effective approach for investigating the physical association and internal structure of nearby open clusters within the Galactic disk.

The microvariability in AGNs was firstly announced and received with skepticism at the beginning of the 1960s, when a few sources were studied with a single-channel photoelectric photometer and the biggest Palomar telescopes. The availability and utilization of CCD cameras breathed new life into small telescopes. For many decades, the variability time-scales from minutes to years have been studied for many blazars using CCD cameras and small telescopes. In the last 30 years, we have been conducting a systematic study of over seventy blazars at the Abastumani Observatory on Mt. Kanobili using CCD cameras and two dedicated medium-sized 125 cm RCh and 70 cm meniscus telescopes. The observations were also conducted using the Calar-Alto 123 cm telescope.

From the middle of the 1990, over 4500 observing nights, we collected in BVRI bands about 600000 images. Among the studied blazars are thirty Northern Sky TeV sources such as Mrk421, Mrk 501, 1ES 0229+200, 1ES 0502+675, 1ES 0647+250, 1ES 0806+52.4, PG 1553+113, 1ES 1959+650, 1ES 2344+51.4, etc., and well-known classical sources such as BL Lacertae, 3C 454.4, 3C 279, S5 0716+714, CTA 102, AO 0235+164, 3C 66A, OJ 287, S4 0954+658, ON 231, 3C 273, PKS 1510-089, and 3C 345.

All images were reduced in MIDAS using DaoPhot II. The typical differential photometric accuracy for an R=15.0 star-like source in a 180 sec exposure is around one percent. A maximum variation for TeV sources up to 1.5 magnitude in the R band was detected, while a few other classical sources showed variations over five magnitudes. Pronounced microvariability at the level of 5% was detected in the case of BL Lacertae and S5 0716+714.

Gas flows are an important aspect of feedback and the regulation of star formation in galaxies. Nearby starburst galaxies and luminous infrared galaxies (LIRGs) provide extreme environments, where feedback and the changes due to it can be studied in great detail. Understanding the gas flows in these galaxies will help us to understand galaxy evolution better. I will present the results from my recently completed PhD thesis. We studied the resolved gas flows in a sample of 12 nearby (0.0073 ≤ z ≤ 0.0374) starburst galaxies and luminous infrared galaxies in the SUperNovae and starBurst in the InfraReD (SUNBIRD) survey with long-slit spectra from the Southern African Large Telescope. We found evidence of ionized and neutral non-circular gas flows (which includes outflows, inflows and extraplanar gas) in all 12 galaxies at varying velocities. No previous measurements of gas flows had been made for five galaxies (ESO 428-G023, ESO 550-IG025, IRAS 18293-3413, NGC 1819 and NGC 3508). The non-circular gas flow velocities of the 12 galaxies range between 35-182 km/s for the ionized gas and 61-403 km/s for the neutral gas and originate from the nucleus for most of the galaxies. Our results also showed that none of the gas flows are strong enough to leave the galaxies and could possibly cool down to form more stars. This suggests that for these starburst galaxies and LIRGs, even though their star-formation rate is enhanced and gas is flowing outwards, star formation is not necessarily quenched by this, and could continue in the future via the galactic fountain model.

The formation and evolution of the ultra-diffuse galaxies (UDGs) continue to remain a puzzle. Similarities and differences in the morphological and the kinematical properties of the UDGs with their possible precursors, namely low-surface brightness (LSB), L*-type high-surface brightness (HSB) and dwarf galaxies, may provide crucial constraints on their origin and evolution. To investigate the possible formation scenario of the UDGs, we selected samples of UDGs, LSBs, HSBs and dwarfs from the TNG50-1 sub-box of the IllustrisTNG simulation. We studied individual galaxy cutouts to evaluate the intrinsic shapes of their dark-matter (DM) and stellar components, orbital and kinematical properties related to their stellar velocity dispersion. Further, we constructed mock integral-field spectroscopic data using the SimSpin code to extract the stellar kinematic moment maps. We find that the isolated UDGs are prolate rotators similar to the dwarf population, while the tidally bound UDGs can exhibit both prolate- and oblate-rotating shapes. The DM and stellar velocity anisotropy properties of the UDGs suggest that they reside in a cored, dwarf-like halo and may be classified by early-type galaxies. Finally, the stellar kinematic properties suggest that both the UDGs and the dwarfs are slow-rotators having low to nearly no-rotations in contrast to the late-type, disc-dominated, fast-rotating LSBs and HSBs. Therefore, we may conclude that the UDGs and the dwarfs possibly have a common dynamical lineage.

Isolated stellar-mass black holes traversing dense regions of the interstellar medium, such as molecular clouds, are expected to accrete ambient gas. This accretion process can ionize surrounding gas, carving out a low-density ionized cavity within the cloud. The accreting black holes may also possess accretion discs and jets, producing cosmic rays and triggering hadronic and leptonic interactions. In this work, we show that the number of black holes residing in molecular clouds is proportional to the size of the cloud and we estimate the specific black-hole number density to be $\sim 1.2 \times 10 ^{-5}$ per solar mass of cloud, i.e., at least 10 black holes in massive molecular clouds with mass $8.4 \times 10^5$ solar mass. We then estimate the accretion process by Bondi–Hoyle–Lyttleton accretion and the effects brought about on the cloud structures, such as the formation of ionization cavities, and on the production of energetic particles. We show that the accretion rate log($\dot{M}$) [g/s] can reach up to 18 and the ionization cavity can reach up to 1 pc, occupying a substantial region of smaller molecular clouds. We discuss the consequences of the presence of ionization cavities in molecular clouds of different sizes, hence the implications for (i) cloud fragmentation and star formation and (ii) the inhomogeneity in the cloud environment for cosmic-ray transport in molecular clouds.