How do magnetars acquire fields of 1e14 to 1e15 G? · revision history

Revision 2

Accepted · core change · record

Changes against revision 1:

Title
How do magnetars acquire fields of $1\mathrm{e}14\ \text{to}\ 1\mathrm{e}15\,\mathrm{G}$?
Plain
The field could be inherited from a strongly magnetic parent star or amplified by a dynamo (stirring motions that regenerate magnetic field) during the collapse.
Precise · changed · core
Revision 1: Determine whether magnetar dipole fields $B \sim 1e14\ \text{to}\ 1e15\ \mathrm{G}$ arise from flux conservation of fossil fields in magnetic massive stars (possibly stellar-merger products), from convective or magnetorotational dynamos in a proto-neutron star spinning at $P$ of a few ms, or from a fall-back-driven Tayler-Spruit dynamo. Answer: the channel or channels consistent with the magnetar birth fraction (estimates ~10 to 40 percent of neutron stars), ordinary supernova remnant energies and kick distributions.
Revision 2: Determine whether magnetar dipole fields $B \sim 10^{14}\ \text{to}\ 10^{15}\ \mathrm{G}$ arise from flux conservation of fossil fields in magnetic massive stars (possibly stellar-merger products), from convective or magnetorotational dynamos in a proto-neutron star spinning at $P$ of a few ms, or from a fall-back-driven Tayler-Spruit dynamo. Answer: the channel or channels consistent with the magnetar birth fraction (estimates ~10 to 40 percent of neutron stars), ordinary supernova remnant energies and kick distributions.
Settled by
Proto-neutron star dynamo simulations predicting field strengths and topology, compared with magnetar population statistics and remnant energetics.
Kind
phenomenon
Answer type
identification
References
(empty)
Literature status
contested
Status note
(empty)
Posed since
1992

Decisions