A short review of the pulsar magnetic inclination angles (II)

A short review of the pulsar magnetic inclination angles (II)
Biao-Peng Li, Wen-Qi Ma, Zhi-Fu Gao
arXiv:2404.13700v1 Announce Type: new
Abstract: The pulsar magnetic inclination angle is a key parameter for pulsar physics. It influences the observable properties of pulsars, such as the pulse beam width, braking index, polarisation, and emission geometry. In this study, we give a brief overview of the current state of knowledge and research on this parameter and its implications for the internal physics of pulsars. We use the observed pulsar data of magnetic inclination angle and braking index to constrain the star’s number of precession cycles, $xi$, which reflects the interaction between superfluid neutrons and other particles inside a neutron star,(NS). We apply the method proposed by Cheng et al. (2019) to analyse the data of PSR J2013+3845 and obtain the constraints for $xi$ ranging from $2.393times 10^{5}$ to $1.268times10^{6}$. And further analysis suggests that the internal magnetic field structure of PSR J2013+3845 is likely dominated by toroidal component. This study may help us understand the process of internal viscous dissipation and the related evolution of the inclination angles of pulsars, and may have important implications for the study of continuous gravitational wave emissions from NS.arXiv:2404.13700v1 Announce Type: new
Abstract: The pulsar magnetic inclination angle is a key parameter for pulsar physics. It influences the observable properties of pulsars, such as the pulse beam width, braking index, polarisation, and emission geometry. In this study, we give a brief overview of the current state of knowledge and research on this parameter and its implications for the internal physics of pulsars. We use the observed pulsar data of magnetic inclination angle and braking index to constrain the star’s number of precession cycles, $xi$, which reflects the interaction between superfluid neutrons and other particles inside a neutron star,(NS). We apply the method proposed by Cheng et al. (2019) to analyse the data of PSR J2013+3845 and obtain the constraints for $xi$ ranging from $2.393times 10^{5}$ to $1.268times10^{6}$. And further analysis suggests that the internal magnetic field structure of PSR J2013+3845 is likely dominated by toroidal component. This study may help us understand the process of internal viscous dissipation and the related evolution of the inclination angles of pulsars, and may have important implications for the study of continuous gravitational wave emissions from NS.