The evolution of the magnetic fields of neutron stars
| dc.contributor.author | Bhattacharya, D | |
| dc.date.accessioned | 2005-12-29T06:01:38Z | |
| dc.date.available | 2005-12-29T06:01:38Z | |
| dc.date.issued | 1995 | |
| dc.description | Diamond jubilee symposium on pulsars,14-17 March 1994, RRI, Bangalore. | en |
| dc.description.abstract | Observational evidence, and theoretical models of the magnetic field evolution of neutron stars is discussed. Observational data indicates that the magnetic field of a neutron star decays significantly only if it has been a member of a close interacting binary. Theoretically, the magnetic field evolution has been related to the processing of a neutron star in a binary system through the spin evolution of the neutron star, and also through the accretion of matter on the neutron star surface. I describe two specific models, one in which magnetic flux is expelled from the superconducting core during spin-down, via a copuling between Abrikosov fluxoids and Onsager-Feynman vortices; and another in which the compression and heating of the stellar crust by the accreted mass drastically reduces the ohmic decay time scale of a magnetic field configuration confined entirely to the crust. General remarks about the behaviour of the crustal field under ohmic diffusion are also made. | en |
| dc.format.extent | 1403742 bytes | |
| dc.format.mimetype | application/pdf | |
| dc.identifier.citation | Journal of Astrophysics and Astronomy, 1995, Vol. 16, p217-232. | en |
| dc.identifier.issn | 0250-6335 | |
| dc.identifier.uri | http://hdl.handle.net/2289/961 | |
| dc.language.iso | en | en |
| dc.publisher | Indian Academy of Sciences, Bangalore, India. | en |
| dc.rights | Indian Academy of Sciences, Bangalore, India. | en |
| dc.subject | Neutron stars; | en |
| dc.subject | pulsars; | en |
| dc.subject | magnetic field; | en |
| dc.title | The evolution of the magnetic fields of neutron stars | en |
| dc.type | Article | en |