Is SGR0418+5729 indeed a waning magnetar?

R. Turolla, S. Zane, J. A. Pons, P. Esposito, N. Rea

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    57 Citations (Scopus)

    Abstract

    SGR0418+5729 is a transient soft gamma-ray repeater which underwent amajor outburst in 2009 June, during which the emission of short bursts was observed. Its properties appeared quite typical of other sources of the same class until long-term X-raymonitoring failed to detect any period derivative. The present upper limit on Ṗ implies that the surface dipole field is Bp ≤ 7.5×1012 G, well below those measured in other soft gamma-ray repeaters (SGRs) and in the Anomalous X-ray Pulsars (AXPs), a group of similar sources. Both SGRs and AXPs are currently believed to be powered by ultra-magnetized neutron stars (magnetars, Bp ≈ 10 141015 G). SGR 0418+5729 hardly seems to fit in such a picture. We show that the magneto-rotational properties of SGR 0418+5729 can be reproduced if this is an aged magnetar, ≈1 Myr old, which experienced substantial field decay. The large initial toroidal component of the internal field required to match the observed properties of SGR 0418+5729 ensures that crustal fractures, and hence bursting activity, can still occur at the present time. The thermal spectrum observed during the outburst decay is compatible with the predictions of a resonant Compton scattering model (as in other SGRs/AXPs) if the field is low and the magnetospheric twist is moderate. © 2011. The American Astronomical Society. All rights reserved.
    Original languageEnglish
    Article number105
    JournalAstrophysical Journal
    Volume740
    Issue number2
    DOIs
    Publication statusPublished - 20 Oct 2011

    Keywords

    • stars: magnetic field
    • stars: neutron

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