Investigation of the temporal variations in scattering and dispersion measure of Giant Radio Pulses in the pulsar в0531+21 in the Crab Nebula at 111 MHz frequency in 2002–2024
- Authors: Losovsky B.Y.1, Potapov V.A.1
-
Affiliations:
- Lebedev Physical Institute of Russian Academy of Sciences
- Issue: Vol 101, No 11 (2024)
- Pages: 977-985
- Section: Articles
- URL: https://journals.rcsi.science/0004-6299/article/view/276114
- DOI: https://doi.org/10.31857/S0004629924110042
- EDN: https://elibrary.ru/JLJNTC
- ID: 276114
Cite item
Abstract
We present in the article the results of our monitoring of Giant Radio Pulses (GRPs) of pulsar B0531+21 (J0534+2200) in the Crab Nebula. Observations has been carried in the PRAO ASC LPI using the BSA LPI radio telescope at 111 MHz frequency at bandwith 2.5 MHz with a 128-channel spectrum analyzer and PRAO Digital Pulsar Receiver in 2002–2024. It is shown that the dependence between the scattering time τ and the dispersion measue DM of GRPs in the period 2010–2021 differs significantly from that before 2010 and after 2021. In 2010–2021 the values of τ and DM demonstrated significant growth and instability, and the functional relationship between them changes rapidly. The data for the entire observation period forms on plot of {τ, dm } (where dm = ( DM – 56.7) × 10 3 ) three main and one transitional branches, formed by 14 different time segments. Thay may be well approximated by power functions τ ∝ dmn with values n = 0.7, 1.1 and 1.86 for the main and 2.1 for the transitional branches. This behavior of τ and DM is explained by anomalous variations in the density and turbulence of magnetically active plasma in the Crab Nebula and the interstellar medium in 2010–2021. Comparing the data at 111 and 610 MHz in the period MJD 55000–56500 (June 2009 – July 2013), we obtained an estimate β = 3.4 ± 0.2 for the dependence of observed scattering on the frequency τ ∝ ν−β. This value is close to the previously published, but significantly differs from the dependencies for both Kolmogorov (β = 4.4) and normal distribution (β = 4) of spatial inhomogeneities of the interstellar medium.
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About the authors
B. Ya. Losovsky
Lebedev Physical Institute of Russian Academy of Sciences
Author for correspondence.
Email: blos@prao.ru
Pushchino Radio Astronomy Observatory, Astro Space Center
Russian Federation, PushchinoV. A. Potapov
Lebedev Physical Institute of Russian Academy of Sciences
Email: potap@prao.ru
Pushchino Radio Astronomy Observatory, Astro Space Center
Russian Federation, PushchinoReferences
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