4.7 Article

The low emission mode in PSR B0329+54

Journal

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 512, Issue 2, Pages 1906-1915

Publisher

OXFORD UNIV PRESS
DOI: 10.1093/mnras/stac539

Keywords

stars: neutron; pulsars: general; pulsars: individual: PSR B0329+54

Funding

  1. Operation, Maintenance and Upgrading Fund for Astronomical Telescopes and Facility Instruments
  2. National Natural Science Foundation of China [U1838109, 12041301, 11873080, U1631106]
  3. Key Laboratory of Xinjiang Uygur Autonomous Region Goverment [2020D04049]
  4. 2018 Project of Xinjiang Uygur Autonomous Region of China for Flexibly Fetching in Upscale Talents

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This study investigates the properties of the low emission mode in PSR B0329+54, and finds that it is characterized by a drop in intensity in the central component. The low mode is related to the two emission modes, and the integrated profile of the low mode is unique. The occurrence rate of low modes is higher in the normal emission mode, and the intensity drop in the central component is separated from the emission of the other two components.
We investigate properties of the low emission mode in PSR B0329+54 based on four single-pulse observations at frequency centred at 1.54 GHz using Nanshan radio telescope in Urumqi. The low emission mode is characterized by an intensity drop in the central component below that of the other two components. Referred here as the low mode, it has an average duration of 3P(0) and is observed in both abnormal and normal emission modes of the pulsar occupying 3.6 per cent of the observed pulses. We demonstrate that the properties of low modes are related to the two modes. We find that the integrated profile of low modes is unique to the two modes, and that low modes occur more frequently when the pulsar is in the normal mode. Analysis of the energy distribution for normal low modes suggests that the cause for the intensity drop in the central component is separated from the emission of the other two components. We demonstrate that the pulse emission characteristics in the normal emission mode shortly after a low-mode bears some similarities with the abnormal mode and gradually recovering to the original normal emission in about three pulsar periods. In addition, the occurrence rate for low modes in different normal modes is mostly consistent, which implies that the duration of low modes is related to a normal mode for this pulsar. Our results imply profile modes each corresponds to specific magnetospheric plama density in particular geometric configuration, and profile mode changing signifies distinct changes of both at different parts of the profile.

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