Том 49, № 10 (2023)

We have analyzed the results of our observations of the millisecond pulsar B0329+54 (J0332+5434), which exhibits quasi-periodic variations in the barycentric times of arrival (TOAs) of pulses
on long time scales. We have tested the hypothesis about the existence of a planet with a mass close to the mass of the terrestrial planets and an orbital period of 27.8 yr around this pulsar that was proposed previously to explain the variations in its TOAs. We show that this hypothesis is not confirmed when considering the series of TOA residuals over the entire available time interval of observations 1968–2022 and that the TOA variations for this pulsar apparently have a different physical cause.

We consider the influence of space curvature in the Schwarzschild metric on the contribution of the magnetic field outside the neutron star to the moment of inertia of a radio pulsar. Our consideration
is restricted only to the simplest configuration of the magnetic field, when it can be described by only one harmonic. We show that at a fixed magnetic field strength on the stellar surface the influence of space curvature reduces the contribution of the magnetic field outside the star to the departure of the inertia tensor from the spherical one several-fold.

In pulsating X-ray sources a magnetized neutron star is surrounded by an accretion disk whose
structure requires a study. In particular, the dipole magnetic field of the star can partially penetrate the disk
and, freezing into the matter, can give rise to an induced magnetic field in the disk. The field growth can be
limited by its turbulent diffusion. In this paper we calculate such an induced field. The problem is reduced to
solving the induction equation in the presence of diffusion. An analytical solution of the equation has been
obtained, with the radial and vertical structures of the induced field having been calculated simultaneously.
The radial structure is close to the previously predicted dependence on the difference of the angular velocities
of the disk and the magnetosphere: b ∝ Ωs − Ωk, while the vertical structure of the field is close to the linear
proportionality between the field and the height above the equator: b ∝ z. The possibility of the existence of
nonstationary quasi-periodic components of the induced magnetic field is discussed.

Gamma-ray bursts (GRBs) are the phenomena of rapid energy release of enormous power associated with the collapse ormerging of stars. As a result of internal processes, populations of nonthermal accelerated particles radiating in a wide energy range are formed in them. A number of observations have shown that photons with energies up to tens of TeV are detected from some GRBs. However, due to the great energy losses of radiating particles, the explanation of this high-energy radiation in terms of standard radiation mechanisms runs into great difficulties. In this paper, based on the model of adiabatic expansion for the GRB afterglow phase, we investigate the influence of magnetic inhomogeneities on the spectra
within the electron and proton synchrotron radiation mechanism by taking into account the Compton scattering of synchrotron photons. We show that the magnetic inhomogeneity effect can increase the
maximum energies of the synchrotron radiation from electrons and protons severalfold without affecting the maximum energies of the Compton photons being produced in the Klein–Nishina regime.