The detection of radio emission from the gamma-ray pulsar J1836+5925 is reported. Rare events of radio emission from this object have been recorded with the LPA radio telescope at the Pushchino Radio Astronomy Observatory. A two- or three-component integrated profile and very narrow individual pulses are a peculiarity of the radio emission from the pulsar J1836+5925. The presence of an interpulse is also possible. We have measured the dispersion measure, DM=23± 1 pc cm ^-3 , and estimated the distance to the pulsar, 1.5 kpc. The flux density and the lower limit on the spectral index have been estimated.

The drift periods P2 and P3 were searched for using the summed power spectra of 41 pulsars observed at declinations from -9o to +42o. The power spectra of pulses with a given period, pulse width and drift behavior have been simulated, the applicability of such a method for estimating drift parameters is shown. For most pulsars, the distribution of harmonic amplitudes in the power spectra corresponds to the expected distribution for these pulsars without drift. At the same time, it was found that for a number of sources, the summed power spectra accumulated over a long period of time give the same drift parameters as those determined by other methods. For 11 pulsars we have defined or redefined the drift period P2. For 8 sources the drift period P3 has been determined or redefined. The drift direction of subpulses was redefined for them.

In this article the title was incorrectly given as ‘‘The Method of Periodic Principal Components for the Dynamic Spectrum of Radio Pulsars and Faraday Rotation of Nine Pulse Components of PSR B0329#’’ but it should have been ‘‘The Method of Periodic Principal Components for the Dynamic Spectrum of Radio Pulsars and Faraday Rotation of Nine Pulse Components of PSR B0329+54’’.

The effect of an absorbing element being displaced relative to a regular lattice node on the neutron balance in a reactor is considered. A way of accounting for a displacement based on the use of the dipole component of the neutron flux in a reactor calculation by the heterogeneous method is described. The proposed method is shown to be effective in calculations performed for fuel assemblies with displaced absorbing elements. Calculations based on the UNK and MCNP5 codes are compared with one another.

Results of long time observations of the pulsar B0950+08 are given. These observations were carried out at the LPA radio telescope at the frequency of 111 MHz from January of 2016 to May of 2019(450 days). A strong variability in emission of this pulsar has been detected with changes in signal to noise ratios hundreds of times. Part of the long-time flux density variability can be explained by refractive scintillations in the interstellar medium. The existence of radiation between the interpulse(IP) and main pulse(MP) was confirmed. It was more powerful than at high frequencies. We detected the unusual IP and precursor(Pr) radiation on 2017 August 1. On the basis of 65 strong IPs we found the correlations between energies of IP and Pr and between the phase of IP and the distance Pr–IP. It is shown that the observed peculiarities of this pulsar can be explained in the frame of the aligned rotator model. We estimated distances of radiation levels from the center of the neutron star. The calculated value of the initial period of 0.2 s means that not all pulsars are born with millisecond periods. The large age of the pulsar(6.8 million years) and the small angle between its magnetic moment and the rotation axis(less than 20°) confirm the suggestion related to pulsar evolution with respect to alignment.

The analysis of radio emission of three new pulsars discovered at the Pushchino Radio Astronomy Observatory is presented. The detailed observations were carried out at a frequency of 111 MHz using the large phase array and the standard digital receiver with a total bandwidth of 2.245 MHz and a time resolution of 2.46 or 5.12 ms. All pulsars exhibit features of their radiation, the subpulse drift is observed in J0220+3622, the flare activity is exhibited in J0303+2248, and the nulling phenomenon has been detected in J0810+3725.

In observations of 2020 performed at the Large Phased Array radio telescope of the Lebedev Physical Institute, two new rotating transients were detected. Dispersion measures of the detected transients are DM = 21 and 35 pc/cm3, pulse half-widths are We = 18 and 35 ms for J1550+09 and J2047+13, respectively. The RRAT J2047+13 period was upper estimated as Р = 2.925. The study shows the existence occurrence of rotating transients whose pulses appear more rarely than one pulse per 10 hours of observations.

We describe the 10-day radio observations of the gamma-ray pulsar J1836+5925. Observations were carried out in the Pushchino Radio Astronomical Observatory at the frequency of 111 MHz using the Large Phased Array of the Lebedev Physical Institute.

During five years of daily observations, the search for new pulsars using the BSA LPI radio telescope in 96 spatial beams covering 17 000 square degrees was conducted. Five new pulsars were identified. Candidate pulsars were selected in summed power spectra. A noise generator was used to renormalize data and total the power spectra for individual directions correctly. As a result, the sensitivity increased by a factor of 10–20 relative to that in individual observational sessions. The sensitivity for pulsars with pulses longer than 100 ms at declinations +30° < δ < +40° was 1.2 and 0.4 mJy in and out of the galaxy plane, respectively.

Pulsar J0810+37 with a period of 1.2483 s is detected at a frequency of 111 MHz during the pulsar search at the Big Scanning Antenna (BSA) radio telescope of the Lebedev Physical Institute [1]. In this paper, we present the results of the detailed study of radio emission from J0810+37 which exhibits a rare nulling effect of different durations in a very wide time interval with an average nulling fraction in “switch-on” days 〈NF〉 = 38%; considering “switch-off” days, 〈NF〉 = 74%, since radio emission from this source is interrupted on average by 2–3 days, and then it again revives on average for 1–2 days. The “switch-off” periods reach 7 days.

Nearly all fast rotating radio transients (RRAT) that are pulsars with rare pulses have previously been detected using decimeter wavelengths. We present here 34 transients detected at meter wavelengths in our daily monitoring at declinations −9° ≤ δ ≤ +42°. Twenty-five transients are new RRATs. We confirm the detection of 7 RRATs based on our early observations. One of the 34 detected transients was determined to be a new pulsar, J1326+3346. At the same time, of the 35 RRATs detected at the decimeter wavelengths in the studied area, only one was detected by us, J1848+1518. The periods of 6 RRATs were found from the arrival time of single pulses. Three quarters of all RRATs were observed more than once, and the total number of RRATs in the area we studied has doubled.

Since 2013, round-the-clock monitoring of the sky has been carried out simultaneously in 96 beams using a high-sensitivity radio telescope called the Large Phased Array (LPA) at the frequency 110.25 MHz. These observations are made under the program of interplanetary plasma investigation. The same data are used to search for pulsars by means of power spectra. To increase the sensitivity of the pulsar search, 500-600 power spectra corresponding to different days of observations are summed. In the integrated spectra of known pulsars, besides expected improvement in signal-to-noise (S/N) ratio for the frequency harmonics, some features are explored in this paper. We present the 27 strongest pulsars which are in a field with declination 21 degrees - 42 degrees. The observable details in the integrated power spectra are connected with the presence of pulsar periods of the second (P-2) and third (P-3) class, which have been identified. Empirical relations for calculating these periods are obtained. The value P-2 is estimated for 26 pulsars, and for 15 sources it is made for the first time. The value P-3 is estimated for 13 pulsars, among them these values are given for five sources for the first time.

Results of 111-MHz monitoring observations carried out on the Big Scanning Antenna of the Pushchino Radio Astronomy Observatory during September 1–28, 2015 are presented. Fifty-four pulsating sources were detected at declinations −9° < δ < 42°. Forty-seven of these are known pulsars, five are new sources, and two are previously discovered transients. Estimates of the peak flux densities and dispersion measures are presented for all these sources.

In this paper we will consider a problem of registration of radio signals from distant sources, natural pulsars or artificial SETI signals. These signals possess a number of common properties, i.e. they are weak, almost indistinguishable from the background noise, are strongly localized on celestial sphere, have spectral characteristics smeared by dispersion on interstellar medium and Doppler drift, suffer from near-Earth electromagnetic interference. In this paper we will overview existing methods for registration of such signals and discuss some alternatives. We implement selected methods as data filters connected to data processing workflow, with 3D Virtual Environment as a frontend, integrate the methods into a system for radio astronomical monitoring StarWatch and apply them for detection of pulsar signals from BSA telescope at Pushchino Radio Astronomy Observatory and narrow band signals in SETI database setilive.org.

We develop a model to explain flares observed at a frequency of 111 MHz in the radiation of pulsar J0643+80. We consider non-linear processes in the electron–positron plasma of the pulsar magnetosphere and show that these interactions can cause self-trapping of radio emission in narrow bands of frequencies. This mechanism can explain the origin of the observed flares without any additional sources of radio emission. The proposed scenario naturally explains why strong enhancement of the radio emission does not affect radiation in other frequency bands.