Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21530007h&link_type=abstract
American Astronomical Society, AAS Meeting #215, #300.07; Bulletin of the American Astronomical Society, Vol. 42, p.296
Astronomy and Astrophysics
Astronomy
Scientific paper
We model the core collapse dynamics of massive progenitor stars with high surface magnetic fields in the theoretical framework of a self-similar general polytropic magnetofluid under self-gravity with a quasi-spherical symmetry. With the specification of physical parameters such as mass density, temperature, magnetic field and wind mass-loss rate on the progenitor stellar surface and the consideration of a rebound shock breaking through the stellar interior and envelope, we find a remnant compact object left behind at the centre with a radius of 106 cm and a mass range of 1 3 solar masses. We also find that surface magnetic fields of such a type of compact objects can be 1014-1015 G, providing that the surface magnetic fields of the progenitor are 103 G. The magnetic field enhancement factor critically depends on the self-similar scaling index n, which also determines the initial density distribution of the massive progenitor. Our research favors the 'fossil-field' scenario of forming magnetars from the strongly magnetized core collapse inside massive progenitor stars. The resulting magnetic field strength on the surface of the remnant proto-neutron star is proportional to the surface magnetic field strength of the progenitor and to the neutron star mass itself, while it anti-correlates with the progenitor stellar mass.
Hu Renyu
Lou Yifei
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