Physics
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...6e...3t&link_type=abstract
Neutron Stars and Black Holes in Star Clusters, 26th meeting of the IAU, Joint Discussion 6, 17-18 August 2006, Prague, Czech Re
Physics
Scientific paper
We use axisymmmetric magnetohydrodynamic simulations to investigate the spinning-down of magnetars rotating in the propeller regime and moving supersonically through the interstellar medium. The star loses its angular momentum due to direct interaction of the rotating magnetosphere with the non-rotating interstellar medium. The simulations indicate that magnetars spin-down rapidly due to this interaction, much faster than for the case of a non-moving star. A magnetar with a surface magnetic field of 1013 - 1015 G is found to spin-down to a period P > 10^5-10^6 s in 10^4 - 10^5 yr. This may explain, why a number of soft gamma-repeaters is so small: because only a tiny fraction of all magnetars rotate sufficiently fast to be identified with the neutron stars. From many simulation runs we have derived an approximate scaling law for the angular momentum loss rate, dot{L} ∝ - ρ0.8μ0.6Ω_*1.5/v0.4, where ρ is the density of the interstellar medium, μ is the star's magnetic moment, Ω_* is its angular velocity, and v is velocity of motion.
Lovelace Richard V. E.
Romanova Marina M.
Toropina Olga D.
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