Superstrong magnetic fields and neutron stars

Details Superstrong magnetic fields and neutron stars Superstrong magnetic fields and neutron stars

May 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976aipc...29....5r&link_type=abstract

AIP Conference Proceedings, Volume 29, pp. 5-5 (1976).

Physics

Scientific paper

The observed spin down rates of pulsars (rapidly spinning isolated neutron stars) imply that their stellar surface magnetic fields exceed 1012 G. In such superstrong fields atoms shrink in each dimension by over an order of magnitude and the binding energy of atoms into molecular chains can exceed that of all the electrons in an isolated atom. The stellar surface layer forms a dense (104-105 g cm-3) tightly bound (10 kev/atom) anisotropic conductor which gives the star a sharp edge even at temperatures of 107°K.
Strong magnetospheric electric fields are insufficient to pull ions from such a surface. Instead they generate electron-positron discharges in the 1012 G field of the near magnetosphere. These particles are probably the source of current flow in the magnetosphere and of many of the observed properties of pulsar radiation.

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