Physics of radio emission in the long-period pulsars
arXiv:2112.00640 · doi:10.1093/mnrasl/slab125
Abstract
Recent multi-frequency measurements of pulse widths W50 for the long-period pulsar J0250+5854 by Agar et al provide a unique insight to the emission process owing to its small polar-cap radius. The frequency-dependence of W50 can be simply understood as a consequence of the emitting plasma remaining under acceleration during the interval of radio emission. This is possible in a plasma of ions and protons but not in one of high-multiplicity electron-positron pairs. Extension of the model to the pulse profiles of the general pulsar population is considered briefly.
4 pages
References in corpus (10)
- Physics of Strongly Magnetized Neutron Stars
- Origin of Pulsar Radio Emission
- Hubble Space Telescope non-detection of PSR J2144-3933: the coldest known neutron star
- The Thousand-Pulsar-Array programme on MeerKAT: -- VI. Pulse widths of a large and diverse sample of radio pulsars
- Old but still warm: Far-UV detection of PSR B0950+08
- The SUrvey for Pulsars and Extragalactic Radio Bursts IV: Discovery and polarimetry of a 12.1-second radio pulsar
- A broadband radio study of PSR J0250+5854: the slowest-spinning radio pulsar known
- Long-lasting accretion-powered chemical heating of millisecond pulsars
- Hubble Space Telescope observations of the old pulsar PSR J0108-1431
- Pair production in the millisecond pulsar J0030+0451