Delayed Magnetic Field Amplification in Magnetars

Details Delayed Magnetic Field Amplification in Magnetars Delayed Magnetic Field Amplification in Magnetars

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21333305l&link_type=abstract

American Astronomical Society, AAS Meeting #213, #333.05; Bulletin of the American Astronomical Society, Vol. 41, p.394

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Scientific paper

Magnetars, which consist of Anomalous X-ray Pulsars (AXPs) and Soft Gamma-ray Repeaters (SGRs), have a high birthrate, i.e, 1/5 to 1/10 the birthrate of core-collapse supernovae. This implies a high fraction of core collapse progenitors (>8; M&sun;) end up as magnetars with magnetic fields >1014 Gauss. We confirm the high birthrate of magnetars, and consider the magnetic fields of magnetars in the context of their progenitors. Evidence points to a need for a large magnification of magnetic field as many progenitors have too low magnetic fields otherwise. Based on core collapse models and observations of young supernova remnants, we conclude that the magnetic field magnification should occur many years after the supernova event. Our proposed solution is delayed magnetic field amplification in a high mass neutron star which is initiated by the transition from baryonic to quark matter and caused by color ferromagnetism in quark matter. The implication is that magnetars are quark stars.

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