Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..385..109k&link_type=abstract
Numerical Modeling of Space Plasma Flows: Astronum 2007 ASP Conference Series, Vol. 385, proceedings of the conference held 10-1
Astronomy and Astrophysics
Astronomy
Scientific paper
We describe the early evolution of a core-collapse supernova explosion following the birth of a magnetar with the dipolar magnetic field of B=10^{15} G and the rotational period of 2 ms, which was studied by means of axisymmetric general relativistic MHD simulations. The numerical models exhibit highly collimated magnetically-driven jets very early on. The power released in the jets is about 3×10^{50} erg/s which implies the spin-down time of ≃ 37 s. Given the observed propagation speed of the jets, v_{p}≃ 0.17c, they are expected to traverse the progenitor in few seconds and after this most of the released rotational energy would be carried away by these jets into the surrounding space. This could be the origin of some long duration GRBs and their afterglows. The total rotational energy of the magnetar, E≃ 10^{52} erg, is sufficient to drive a hypernova but the fraction of this energy transferred by the jets to the stellar ejecta could be rather small.
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