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Magnetic Fields in Supernovae

  • Shizuka Akiyama
  • J. Craig Wheeler
Part of the Astrophysics and Space Science Library book series (ASSL, volume 302)

Abstract

A relatively modest value of the initial rotation of the iron core, a period of ∽ 6 – 31 s, will give a very rapidly rotating protoneutron star and hence strong differential rotation with respect to the infalling matter. Under these conditions, a seed field is expected to be amplified by the magnetorotational instability (MRI) and to grow exponentially. Exponential growth of the field on the time scale Ω-1 by the MRI will dominate the linear growth process of field line “wrapping” with the same characteristic time. The shear is strongest at the boundary of the newly formed protoneutron star. Modest initial rotation velocities of the iron core result in sub-Keplerian rotation and a sub-equipartition magnetic field that nevertheless produce substantial magnetohydrodynamic (MHD) luminosity and hoop stresses: saturation fields of order 1015 — 1016 G develop ∽ — 300 msec after bounce with an associated MHD luminosity of ∽ — 1049 — 1053 erg s-1 . Bi-polar flows driven by this MHD power can affect or even cause the explosions associated with core-collapse supernovae. If the initial rotation is too slow, then there will not be enough rotational energy to power the supernova despite the high luminosities. The MRI should be active and may qualitatively alter the flow if a black hole forms directly or after a fall-back delay.

Keywords

Supernova jets MHD 

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Copyright information

© Springer Science+Business Media Dordrecht 2004

Authors and Affiliations

  • Shizuka Akiyama
    • 1
  • J. Craig Wheeler
    • 1
  1. 1.Astronomy departmentUniversity of Texas at AustinAustinUSA

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