Speaker
Rosalba Perna
(Stony Brook University)
Description
The magnetic field strength at birth is arguably one of the most
important properties to determine the evolutionary path of a neutron
star. Objects with very high fields, collectively known as magnetars,
are characterized by high X-ray quiescent luminosities, outbursts,
and, for some of them, sporadic giant flares. While the magnetic field
strength is believed to drive their collective behaviour, however, the
diversity of their properties, and, especially, the observation of
magnetar-like bursts from 'low-field' pulsars, has been a theoretical
puzzle. In this talk, I will discuss results of long-term MHD
simulations which, by following the evolution of magnetic stresses
within the neutron star crust, have allowed to relate the observed
magnetar phenomenology to the physical properties of the neutron
stars, and in particular to their age and magnetic field strength and
topology. The dichotomy of 'high-B' field pulsars versus magnetars is
naturally explained, and occasional outbursts from old, low B-field
neutron stars are predicted. I will conclude speculating on the fate
of old magnetars.
Primary author
Rosalba Perna
(Stony Brook University)
Co-authors
Mr
Daniele Vigano'
(U. of Barcelona)
Prof.
Jose Pons
(U. of Alicante)
Prof.
Nanda Rea
(U. of Amsterdam)
