The Origin Magnetars: the role of anisotropic neutron superfluid of neutron stars
| dc.creator | Peng, Qiu-he | |
| dc.date | 2006-07-11 | |
| dc.date.accessioned | 2026-07-07T07:15:39Z | |
| dc.date.available | 2026-07-07T07:15:39Z | |
| dc.description | We estimate the strength of the induced magnetic field due to the total induced magnetic moment of the anisotropic ($^3PF^2$) neutron superfluid interior of neutron stars. The induced magnetic field of the neutron stars is found as follows. $B^{(in)} = \fracη{T_7 - η}B^{(0)} ,\begin{array}{*{20}c}{} & {η=} \ \end{array}\frac{m(^3 P_2 )}{0.1m_{Sun}}R_{NS,6}^{- 3} $ ($T_7$ denotes the interior temperature of the neutron star in unit of 10$^7$ K). The induced magnetic field will gradually increase with the temperature of the neutron star decreasing in their late evolutionary stage. A magnetar may appear in a condition when $T_7 \to η$. The upper limit of the induced magnetic field of $^3P^2$ superfluid is $3.35 \time 10^{14} η$. | |
| dc.description | 6 page, no figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0607215 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0607215 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/113291 | |
| dc.subject | Astrophysics | |
| dc.title | The Origin Magnetars: the role of anisotropic neutron superfluid of neutron stars | |
| dc.type | text |