A comparative analysis of the dynamics of the orbital motion (regular or chaotic) of 45 globular clusters in the central region of the Galaxy with a radius of 3.5 kpc is carried out. The static and evolving (based on the semi-analytical cosmological model of Gomez et al. (2010) and Hagi et al. (2015)) potentials of the Galaxy are considered both in the form of an axisymmetric and non-axisymmetric potential of the Galaxy with a rotating elongated bar with the following parameters at the present time: mass 10^10 M_⊙, length of the major semi-axis 5 kpc, rotation angle of the bar axis 25^o, angular velocity of rotation 40 km s^-1 kpc^-1 . To form the 6D-phase space required for integrating the orbits, the most accurate astrometric data to date from the Gaia satellite (Vasiliev & Baumgardt, 2021), as well as new refined average distances (Baumgardt & Vasiliev, 2021) were used. We used a frequency method for analysis of the chaotic/regular orbital motion of all 45 GCs. The results are summarized in the table, which provides an overview of each GC in our sample, the degree of chaotization in both the static and evolving potentials, and the influence of the central rotating bar on the degree of orbital chaotization in both cases. It is shown that the orbital dynamics have undergone minor changes during the transition from the static to the evolving potential. This confirms our previously obtained result that changes in the masses and sizes of the gravitational potential components act on orbital parameters in opposite ways, and at small galactocentric distances this influence is maximally compensated, while the orbits of distant objects and objects with large apocentric distances experience the greatest influence.
We present the first comprehensive photometric and orbital analysis of the detached eclipsing binary 2MASS 22425392+5439498,utilizing multi-survey data from Lapukhin, ASAS-SN, and TESS. The study combines light curves spanning over a decade to determine the orbital period, eccentricity, and evidence for apsidal motion in this previously uncharacterized system. When modeling this system based on photometric data using the JKTEBOP program, we accounted for third-light contamination from a line-of-sight star, limb darkening, and the system’s orbital geometry parameters. The secondary minimum occurs at phase ϕ= 0.4940, indicating a small but significant eccentricity. Based on the modeling results, we estimate the apsidal motion of the system to be very slow (i.e., the apsidal period is very large), and therefore, this motion does not significantly affect the depth of the eclipses.
The data from a three-year monitoring of the gravitationally lensed quasar (GLQ) B1422+231 are analyzed. The results of photometric analysis are presented: light curves that indicate significant microlensing in the lensed components of the source, as well as the probable values of time delays between the three pairs of components: ∆tAB=−52.4±3 days, ∆ tAC= 14.2±2 days and ∆ tCB= 48.4±2 days.
This study shows the correlation of 705 interplanetary (IP) type II radio bursts detected during the solar cycle (SC) 23, 24, and ascending phase of SC 25 with sunspot number (SSN) and number of flares by class. The results show that 675 (96%) of these bursts were associated with coronal mass ejections (CMEs), while the remaining 30 (4%) were not associated with CMEs. The total number of IP type II bursts was caused by B-class (5), C-class (138), M-class (275), and X-class (124) solar flares, and among them, M- class (51%) flares dominated. We examined the relationship between IP type II bursts and SSN during the ascending phase of all three SCs and found a high correlation between them (correlation coefficients 0.91, 0.98, 0.99, respectively). We found the correlation of the number of IP type II bursts with the number of C, M, and X solar flares, and found that M-class flares showed a strong correlation with IP type II bursts (correlation coefficients 0.76, 0.93, and 0.72, respectively).
A generalized expression for potential energy in three-dimensional space is investigated, which allows the existence of a local integral of motion in rotating systems. A form of potential energy is introduced that includes contributions from the gradient of a scalar field, an external potential, and rotational effects. This approach enables the description of effective potentials in galactic dynamics, including contributions from both ordinary and dark matter, as well as rotational effects. Examples of applications are discussed, ranging from analytical models of dark matter halos to hypothetical objects such as self-gravitating Bose–Einstein condensates of dark matter. It is shown that the proposed form of the potential is analogous to expressions found in the Lagrangians and energy functionals of Fuzzy Dark Matter (FDM) and Scalar Field Dark Matter (SFDM) models. This allows for the interpretation of observed galaxy properties, such as flat rotation curves, through the contributions of dark matter and kinetic-gravitational interactions in scalar fields.
Many disk galaxies exhibit a lopsided nature, with their nuclei clearly displaced from their geometric centers. This phenomenon is associated with gravitational instability during the early stages of the evolution of these objects. Based on this, the present work investigates the gravitational instability of lopsided perturbation modes in the context of a non-stationary disk model with an anisotropic velocity diagram. Corresponding non-stationary analogues of the dispersion equations for these perturbation modes have been derived. The results of the study are presented as critical dependencies of the initial virial ratio on the disk rotation parameter for different values of the superposition parameter. Based on the analysis of the obtained results, it is established that, within the framework of a non-stationary disk model, lopsided perturbation modes exhibit various types of instability depending on the values of the parameters of the non- stationary model of disk-shaped self-gravitating systems.
