In this work, the light curve of the Seyfert galaxy Mrk 6 constructed from photometric observations in the B, V, and Rc filters over the period from 5 April 2016 to 1 February 2026 is presented and analyzed. Over the entire monitoring interval (2016–2026), the variability amplitude of the light curve reaches ΔB=1.9 mag, ΔV=1.5 mag, and ΔRc=1.4 mag. During 2024–2026, the galaxy exhibits synchronous photometric variability in the B, V, and Rc filters with an amplitude of ∼0.3 mag. The study also uses spectroscopic observations obtained on 15 and 22 November 2025 and 16 February 2026 at the Shamakhy Astrophysical Observatory (Azerbaijan), as well as on 9 January 2026 at the Fesenkov Astrophysical Institute (Kazakhstan). The fluxes of the Hβ emission line were calibrated using the [O III] λ5007 Å line, ensuring consistent relative calibration of the spectral data. The radius of the broad-line region RBLR was taken to be equal to the average time delays (lags), amounting to ≈20 light-days for the Hβ line and ≈28 light-days for the Hα line.

This paper presents the results of new B, V, and Rc photometric observations of the Seyfert 1.5 galaxy NGC 7469, conducted from October 2025 to January 2026 at the Tian Shan Astronomical Observatory. The primary goal of the study was to monitor the state of the active galactic nucleus (AGN) following a significant optical outburst recorded in late 2024. Observations were performed using a 1-meter Carl Zeiss telescope and processed with differential CCD photometry techniques using a 7″ aperture. The results show that during the study period, the galaxy remained in a state of relative photometric stability with a mean V-band magnitude of approximately 13.2–13.3. The recorded variability amplitude was ~ 0.12 mag, which significantly exceeds the photometric errors (σV ≈ 0.007). Comparison with historical data indicates that while the rapid brightness increase of 2024 has ceased, the object has stabilized at a luminosity level notably higher than the minimum observed in 2021. This stability at an elevated state confirms the persistence of a new active phase of the nucleus. The findings provide critical data for understanding the duty cycle of accretion processes and the interaction between the AGN and the surrounding starburst ring in LIRG systems.

We propose a method to measure the energy dependence of the neutron optical potential dVopt/dE in the slow neutron energy regime. Our method makes essential use of a special property of the phase shift for a nonrelativistic neutron in moving matter, known as the neutron Fizeau effect. If a neutron traverses a medium which moves along the surfaces of its own parallel boundaries, the neutron only experiences a phase shift if the neutron optical potential of matter depends on the incident neutron energy. This feature of the neutron Fizeau effect can be combined with newly-developed forms of neutron interferometry to conduct sensitive measurements of dVopt/dE. We describe some examples of scientific applications of this idea in the fields of neutron optics, subthreshold neutron-nucleus resonances, parity violation in low-energy p-wave neutron-nucleus resonances, and neutron scattering amplitudes of the nuclei of rare earth elements.

В данной работе исследуется влияние ядерных реакций, протекающих в условиях вырожденной материи, на установление термодинамического равновесия в недрах нейтронных звёзд. Особое внимание уделено условиям, при которых эти реакции становятся термодинамически возможными, а также их влиянию на химический состав и энергетический баланс вырожденной материи. Рассматриваются как реакции β-распада и электронного захвата, так и термоядерные процессы, протекающие в слоях аккрецирующей материи. Показано, что электронный захват становится возможным при достижении плотности порядка , когда химический потенциал электронов повышает порог реакции. При плотностях выше этого значения скорость реакции возрастает экспоненциально, и β-равновесие устанавливается за характерное время менее нескольких секунд. Также дается оценка временам релаксации и их зависимости от плотности и температуры. Показано, что ядерные процессы оказывают значительное влияние на состав вещества и тепловую эволюцию звезды, участвуя в перераспределении энергии и частиц. Работа основана на аналитических оценках и обзорной интеграции современных результатов численного моделирования. Представленные оценки химического потенциала, времени релаксации и условий равновесия, подтверждают ключевую роль электронного захвата в физике внутренней корки компактных звёзд. Ключевые слова: реакции электронного захвата, компактные звезды, химический потенциал, термодинамическое равновесие, ядерные процессы.

This paper investigates the role of phonon dynamics in the solid crust of neutron stars and their connection to large-scale structural instabilities. Electron capture reactions in the dense outer layers of compact stars generate excited nuclei, which may transfer their energy to the lattice in the form of phonons. These vibrational modes affect the elastic response of the crust, modifying its stress–strain behavior under extreme astrophysical conditions. Using fundamental parameters such as Young’s modulus, density, and sound velocity, we estimate phonon frequencies, wave numbers, and lifetimes across different crustal layers. Numerical analysis indicates that phonon excitations are capable of storing elastic energy and may act as precursors of sudden stress release events. A special focus is given to pulsar glitches, with the Vela pulsar serving as a representative example. The comparison between calculated phonon energies and observed glitch energetics suggests that collective phonon processes could contribute to the mechanism of these abrupt rotational irregularities. By emphasizing the importance of lattice dynamics in neutron star models, this work provides the first quantitative estimates linking microscopic phonon excitations with macroscopic glitch energetics, thus contributing to a deeper understanding of how nuclear-scale transitions manifest as observable astrophysical signals. These findings can contribute to future models of neutron star crust dynamics and related astrophysical observations.