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

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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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Sobre autores

B. Losovsky

Lebedev Physical Institute of Russian Academy of Sciences

Autor responsável pela correspondência
Email: blos@prao.ru

Pushchino Radio Astronomy Observatory, Astro Space Center

Rússia, Pushchino

V. Potapov

Lebedev Physical Institute of Russian Academy of Sciences

Email: potap@prao.ru

Pushchino Radio Astronomy Observatory, Astro Space Center

Rússia, Pushchino

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2. Fig. 1. The Crab Nebula GR obtained at BSA and CPP on 26/07/2024, normalized to a frequency of 111.879 MHz. The figure shows the observed GR (circles) and the function inscribed in it, obtained by formula (1), simulating a pulse with τ = 17.48 ms, scattered in the frequency channel band of 2.4576 kHz (solid red line). The abscissa axis shows time in milliseconds, the ordinate axis shows the normalized flux density.

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3. Fig. 2. Changes in the scattering τ and the dispersion measure DM of the 111 MHz pulsar in the KT in the period 2002–2024. The abscissa axis shows the observation epoch in modified Julian days, the ordinate axis shows the scattering τ [ms] (left axis, triangles) and the conditional dispersion measure dm = (DM – 56.7) × 103 [0.001 pc/cm3 ] (right axis, circles). The vertical dashed lines indicate the moments of transition between different branches on the graph of the dependence of τ on DM (see below Fig. 3 and Table 1), corresponding to the transition from the quiet to the disturbed regime in the variations of the values ​​of τ and DM in MJD 55203, and the reverse transition in MJD 59375. Note also that the moments of transition are close to the local maxima of τ and, in the case of the first transition, also to the maximum of DM.

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4. Fig. 3. Statistical dependence of the scattering τ (in milliseconds) at a frequency of 111 MHz on the conditional dispersion measure dm = (DM – 56.7) × 103 [0.001 pc/cm3] of the pulsar in KT in the period September 2002–January 2024. The main branches of the dependence (see legend): lower (1), two upper (2, 3) and transition branch (4).

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