arXiv
Open Access
2019
The Period-Width relationship for radio pulsars revisited
Simon Johnston
Aris Karastergiou
Abstrak
In the standard picture of radio pulsars, the radio emission arises from a set of open magnetic field lines, the extent of which is primarily determined by the pulsar's spin period, P, and the emission height. We have used a database of parameters from 600 pulsars to show that the observed profile width, W, follows W proportional to P^-0.3 albeit with a large scatter, emission occurs from heights below 400 km and that the beam is underfilled. Furthermore, the prevalence in the data for long period pulsars to have relatively wide profiles can only be explained if the angle between the magnetic and rotation axis decays with time.
Topik & Kata Kunci
Penulis (2)
S
Simon Johnston
A
Aris Karastergiou
Akses Cepat
Informasi Jurnal
- Tahun Terbit
- 2019
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- en
- Sumber Database
- arXiv
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- Open Access ✓