A hybrid model for pulsar's spin‐down evolution. Issue 9 (18th December 2019)

• Record Type: Journal Article
• Authors: Gao, Zhi‐Fu; Wang, Hui; Peng, Qiu‐He; Shan, Hao; Wang, Na
• Other Names: Zen Vasconcellos C.A. guestEditor.; Pérez Martínez A. guestEditor.; Pérez Rojas H. guestEditor.; Roth M. guestEditor.; Hess P. guestEditor.; Gonzalez Felipe R. guestEditor.; Boller Th. guestEditor.
• Is Part Of: Astronomische Nachrichten. Volume 340:Issue 9/10(2019)
• Page Start: 1035
• Page End: 1039
• Publication Date: 2019-12-18
• Subjects: neutron superfluid Cooper pairs -- spin‐down evolution -- hybrid model; Astronomy -- Periodicals; 520.5
• DOI: 10.1002/asna.201913712
• Languages: English
• ISSNs: 0004-6337

Abstract

Abstract: By considering the combined effects of both the standard magnetic dipole model and the composite neutron superfluid vortex model on pulsar's spin‐down, we study the evolution of pulsar's spin‐down on the P − P ˙ diagram. The evolution path of each pulsar is dictated by a particular mechanism in our hybrid model within different parameter spaces. The valley of each curve is the most possible place for a neutron star (NS) to be observed as this is the place corresponding to the minimum value of the evolution speed (i.e., the time derivative P ˙ ). In other words, pulsars would distribute around these valleys on the P − P ˙ diagram. The suppressed region in the lower‐right part of the diagram can be explained by neutrino cyclotron emission from the 1 S 0 neutron superfluid vortexes in NSs.