We investigate the effects of magnetic fields on proto-neutron star winds by performing numerical simulations. We assume that the atmosphere of a proto-neutron star has a homogenous magnetic field (ranging from 10 12G to 5 × 1015G) perpendicular to the radial direction and examine the dependence of the three key quantities (the dynamical time scale τdyn, electron fraction Ye, and entropy per baryon s) for the successful r-process on the magnetic field strength. Our results show that even with a magneter-class field strength, ∼ 10 15G, the features of the wind dynamics differ only little from those of non-magnetic winds and that the conditions for an effective r-process are not realized.
|Number of pages||26|
|Journal||Progress of Theoretical Physics|
|Publication status||Published - 2005 Nov|
ASJC Scopus subject areas
- Physics and Astronomy(all)