On the radio frequency dependence of the pulse delay phenomenon in PSR B0943+10

• Published in: Monthly notices of the Royal Astronomical Society Vol. 502; no. 4; pp. 6094 - 6100
• Main Authors: Suleymanova, S A, Kazantsev, A N, Rankin, J M, Logvinenko, S V
• Format: Journal Article
• Language: English
• Published: Oxford University Press 01.04.2021
• Subjects: pulsars: individual: B0943+10; pulsars: individual: J0946+0951; pulsars: general; stars: neutron
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stab472

ABSTRACT We report the result of measurements of a gradual shift of the integrated pulses towards later spin phase of the anomalous pulsar B0943+10 at high radio frequencies. We have used observations from the Arecibo Observatory and the GMRT at 327 and 325 MHz correspondingly. For the measurements, we have proposed a special method for calculating the correct positions of the partially merged two components of the pulse profile shape with significant temporal changes in their amplitude ratio. The exponential change in the pulse phase with an amplitude of 4 ms and characteristic time of about 1 h has been found. Comparison of our measurements at 325 and 327 MHz with those at the lower frequencies of 25–80, 62 and 112 MHz have shown that the character of the process does not depend on frequency across a wide frequency range. The result is very important for constraining the nature of the delay. It supports the assumption that the process results from changes in the vacuum gap near the surface of the pulsar. The further correlation between changes in the pulse phase and its intensity is discussed.