Spin period evolution of Vela pulsar based on the wind emission: Application to the long period radio pulsars GPM J1839‐10 (P = 21 min) and GLEAM‐X J1627 (P = 18 min)

• Published in: Astronomische Nachrichten 2024-06, Vol.345 (5), p.n/a
• Main Authors: Sun, Yi‐Hong, Wang, De‐Hua, Zhang, Cheng‐Min, Cui, Xiang‐Han, Zhang, Jian‐Wei, Yu, Jing, Zhou, Yun‐Gang, You, Zi‐Yi
• Format: Article
• Language: English
• Subjects: Age; Celestial bodies; Evolution; Magnetic dipoles; Neutron stars; PSR B0833‐45(the Vela pulsar); Pulsars; pulsars: general; pulsars: individual; Radiation; stars: neutron; Supernova remnants; supernovae: individual
• ISSN: 0004-6337; 1521-3994
• DOI: 10.1002/asna.20230176

The Vela pulsar is a young neutron star with spin period of P = 89 ms and a measured low braking index (˜1.4) that is much less than the standard value of 3 predicted by the magnetic dipole radiation (MDR) model; however, its spin period evolution has been a mystery. In this article, we assume that the spin‐down of the Vela pulsar is attributed to both MDR and wind flow (hereafter MDRW), and find that the ratio of wind flow to the magnetic dipole radiation is about 80%, which is higher than that of the Crab pulsar (25%). In other words, the spin‐down torque of the Vela pulsar is dominated by the wind flow. The spin period (P) evolution of the Vela pulsar depends on its real age, where its supernova remnant age is assumed to be an indicator of its true age, estimated from 10 to 20 kyr, and then we obtain their initial spin periods of ˜53.89 and ˜20.90 ms, respectively, which are consistent with the observed initial spin period ranges of young pulsars. Furthermore, we find that the Vela‐like pulsar by MDRW can evolve to the long spin period of a thousand of seconds in less than million years, which can conveniently help the astronomers understand the recently observed ultra‐long period radio pulsars like GPM J1839‐10 (P = 21 min), GLEAM‐X J1627 (P = 18 min), as well as PSR J0901+4046 (P = 76 s).