arXiv subjects

A. E. Rodin

Publications and source records attributed to A. E. Rodin.

5 recordsLinked to original sources

arXiv2025

Revisiting the energy distribution and formation rate of CHIME fast radio bursts

Based on the first CHIME/FRB catalogue, three volume-limited samples of fast radio bursts (FRBs) are built, with samples 1, 2, and 3 corresponding to a fluence cut of 5, 3, and 1, respectively. The Lynden-Bell's c$^-$ method was applied to study their energy function and event rate evolution with redshift ($z$). Using the non-parametric Kendall's $τ$ statistics, it is found that the FRB energy ($E$) strongly evolves with redshift as $E(z)\varpropto(1+z)^{1.24}$ for sample 1, $E(z)\varpropto(1+z)^{0.98}$ for sample 2, and $E(z)\varpropto(1+z)^{1.99}$ for sample 3. After removing the redshift dependence, the local energy distributions of the three samples can be well described by a broken power-law form with a broken energy of $\sim10^{40} \rm erg$. Meanwhile, the redshift distributions of samples 1 and 2 are identical but different from that of sample 3. Interestingly, we find that the event rates of samples 1 and 2 are independent of redshift, and sample 3 decreases as a single power-law form with an index of -2.41. The local event rates of the three samples of CHIME FRBs are found to be consistently close to $\sim 10^4\rm{\,Gpc^{-3}yr^{-1}}$, which is comparable with some previous estimates. In addition, we notice that the event rate of sample 3 FRBs with lower energies not only exceeds the star formation rate at the lower redshifts but also always declines with the increase in redshift. We suggest that the excess of FRB rates compared with the star formation rate at low redshift mainly results from the low-energy FRBs that could originate in the older stellar populations.

astro-ph.HE↗

arXiv2021

Comparative Analysis of the Observational Properties of Fast Radio Bursts at the Frequencies of 111 and 1400 MHz

A comparative analysis of the observational characteristics of fast radio bursts at the frequencies 111 and 1400 MHz is carried out. The distributions of radio bursts by the dispersion measure are constructed. At both frequencies, they are described by a lognormal distribution with the parameters $μ=6.2$ $σ= 0.7$. The dependence $τ_{sc}(DM)$ of the scattering value on the dispersion measure at 111 MHz and 1400 MHz is also constructed. This dependence is fundamentally different from the dependence for pulsars. A comparative analysis of the relationship between the scattering of pulses and the dispersion measure at 1400 MHz and 111 MHz showed that for both frequencies it has the form $τ_{sc}(DM)\sim DM^k$, where $k = 0.49 \pm 0.18$ and $k = 0.43 \pm 0.15$ for the frequencies 111 and 1400 MHz, respectively. The obtained dependence is explained within the framework of the assumption of the extragalactic occurrence of fast radio bursts and an almost uniform distribution of matter in intergalactic space. From the dependence $τ_{sc}(DM)$ a total estimate of the contribution to the matter of the halo of our and the host galaxy to $DM$ is obtained $DM_{halo} + \frac{DM_{host}}{1+z}\approx 60\;{\rm pc/cm}^3$. Based on the LogN - LogS dependence, the average spectral index of radio bursts is derived $α= - 0.63 \pm 0.20$ provided that the statistical properties of these samples at 111 and 1400 MHz are the same.

astro-ph.IM↗

arXiv2019

Search for Fast Radio Bursts in the Direction of the Galaxies M31 and M33

The results of a search for individual fast radio bursts with the Large Phased Array of the Lebedev Physical Institute at 111 MHz during July 2012 through August 2018 are presented. The signals were distinguished by convolving the data with a template with a fixed form, followed by convolution with test dispersion measures. Areas of sky containing the galaxies M31 and M33 were chosen for the search. Three radio bursts were detected in the vicinity of M33, five in the vicinity of M31, and one in a region offset from the center of M31 by an hour in right ascension. The dispersion measures of the detected bursts range from 203 to 1262 $ pc \cdot cm^{-3}$.

astro-ph.IM↗

arXiv2017

On The Existence of Planets Around the Pulsar PSR B0329+54

Results of timing measurements of the pulsar PSR B0329+54 obtained in 1968--2012 using the Big Scanning Antenna of the Pushchino Radio Astronomy Observatory (at 102 and 111 MHz), the DSS 13 and DSS 14 telescopes of the Jet Propulsion Laboratory (2388 MHz), and the 64 m telescope of the Kalyazin Radio Astronomy Observatory (610 MHz) are presented. The astrometric and rotational parameters of the pulsar are derived at a new epoch. Periodic variations in the barycentric timing residuals have been found, which can be explained by the presence of a planet orbiting the pulsar, with an orbital period $P_{1}$ = 27.8 yr, mass \textit{$m_{c}$}sin\textit{i} = 2$M_{\oplus}$, and orbital semi-major axis $a$ = 10.26 AU. The results of this study do not confirm existence of a proposed second planet with orbital period $P_{2}$ = 3 yr.

astro-ph.IM↗

arXiv2011

Optimal Filtration and a Pulsar Time Scale

An algorithm is proposed for constructing a group (ensemble) pulsar time based on the application of optimal Wiener filters. This algorithm makes it possible to separate the contributions of variations of the atomic time scale and of the pulsar rotation to barycentric residual deviations of the pulse arrival times. The method is applied to observations of the pulsars PSR B1855+09 and PSR B1937+21, and is used to obtain corrections to UTC relative to the group pulsar time PT$_{\rm ens}$. Direct comparison of the terrestrial time TT(BIPM06) and the group pulsar time PT$_{\rm ens}$ shows that they disagree by no more than $0.4\pm 0.17\; μ$s. Based on the fractional instability of the time difference TT(BIPM06) -- PT$_{\rm ens}$, a new limit for the energy density of the gravitational-wave background is established at the level $Ω_g {h}^2\sim 10^{-9}$.

astro-ph.IM↗