arXiv subjects

A. O. Skoryk

Publications and source records attributed to A. O. Skoryk.

3 recordsLinked to original sources

arXiv2026

The UTR-2 decametre pulsar and transient survey I. Transient detection

Context. This paper presents a detailed description of the Decametre Pulsar and Transient Survey of the Northern Sky that was carried out in 2012-2017 using the world's largest radio telescope at decametre wavelengths - UTR-2 in Ukraine. This extensive survey covers the northern sky from declination -10 to +80 deg , with a temporal resolution of 8 ms, and explores dispersion measures up to 30 pc/cc. Aims. The major advantage of the decametre wavelength range is a comparatively wide band, in which the dispersive delay due to the interstellar plasma reaches hundreds of seconds, giving us the opportunity to determine the dispersion measure with a very high accuracy. This enables us to discover new transients, while avoiding data contamination from numerous weak signals of a different nature. Methods. The drift-scan survey in 5-beam mode of UTR-2 was carried out at night time. To cover the entire sky along the right ascension, the duration of the sessions was more than 12 hours at a time close to the autumn and spring equinoxes (to obtain the same conditions for the interference situation). 90 degrees along the declination were covered by five beams in 40 days (each equinox). Results. We discovered 380 individual transient signals with dispersion measures significantly differ from those of known sources. We determined the parameters of each single transient signal. We show that they cannot be explained by ionospheric scintillations. Repeated observations have shown that some detected transient signals are repetitive and are thus likely to originate from pulsars or rotating radio transients. Key words. Stars: neutron - pulsars: general - Methods: data analysis - Methods: observational - Astronomical databases: Surveys

astro-ph.GA↗

arXiv2015

Detection of the fine structure of the pulsar J0953+0755 radio emission in the decametre wave range

In this paper the anomalous intense pulse of the PSR J0953+0755 was studied in decametre wavelength range. For this pulse two scales of fine structure were discovered. The long-scale structure consists of four components, where the visible dispersion measures of even and odd components are different. The obtained time-scale of the short fine structure is 1 ms. The difference in visible dispersion measure can be caused by propagation of two normal modes of the pulsar radiation and irregularities of electron concentration in the space near the neutron star like upper layers of magnetosphere and pulsar wind.

astro-ph.HE↗

arXiv2014

Polarization Sounding of Pulsar Magnetosphere (Part I)

In a cycle of papers, starting with the present one, a fundamental possibility of the polarization sounding of a pulsar magnetosphere using pulsar self-radiation as a test signal will be considered. The main idea of such a sounding is based on the fact that in some models of pulsar magnetosphere the emission frequency depends on the height of its origin above the pulsar surface. For this purpose it is needed to study the dependence of such a parameter as the rotation measure on frequency and pulse phase. We expect that it is possible to register the rotation measure dependence on the central observing frequency and/or the pulse phase during the observations at widely spaced frequencies in the same conditions. The reliable registration of this dependence will result in resolving of the pulsar magnetosphere in depth. It is preferably to carry out the polarization researches in the observational mode of the individual pulses. In this part of the work the model of polarized pulsed radio emission and the model of weakly anisotropic propagation medium are considered. In future articles we will show how to determine the polarization parameters of pulsar radiation with the highest precision in presence of different types of recorders on the receiving side. The specifics of polarization observations at decameter wavelengths will be considered. The algorithms for solving the inverse problem for different types of receivers and the variable conductivity of the underlying surface will be developed.

astro-ph.GA↗