Supernova remnant energetics and magnetars: no evidence in favour of millisecond proto-neutron stars

By J. Vink, Lucien Kuiper Utrecht University, The Netherlands, Sron Netherlands Institute for Space Research, Utrecht. 2006

144 citations recorded by the source corpus.

It is generally accepted that anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are magnetars, i.e. neutron stars with extremely high surface magnetic fields (B > 1014 G). The origin of these high magnetic fields is uncertain, but a popular hypothesis is that magnetars are born with an initial spin period not much exceeding the convective overturn time (∼3 ms), which results in a powerful dynamo action, amplifying the seed magnetic field to ≳1015 G. Part of this rotation energy is then expected to power the supernova through rapid magnetic braking. It is therefore possible that magnetar creation is accompanied by supernovae that are an order of magnitude more energetic than normal supernovae, provided their initial spin period is ∼1 ms. However, we list here evidence that the explosion energies of these supernova remnants associated with AXPs and SGRs – Kes 73 (AXP 1E 1841−045), CTB 109 (AXP 1E2259+586) and N49 (SGR 0526−66) – are close to the canonical supernova explosion energy of 1051 erg, suggesting an initial spin period of P0≳ 5 ms.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d2c735455382a9a06142dba4b1fb2de7bd818222

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Citations in the corpus

• The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “Furthermore, the SN remnants of Galactic magnetars do not show evidence for hyper-energetic SN explosions (e.g. Vink & Kuiper 2006; see, however, Horvath & Allen 2010).”
• SUPERNOVA LIGHT CURVES POWERED BY YOUNG MAGNETARS (2009, background): “Such rapidly rotating magnetars must be rare, as Vink & Kuiper (2006) found that the galactic supernovae remnants of known magnetars were explained with typical explosion energies of 1051 ergs.”
• 1E 1547.0–5408: A Radio-emitting Magnetar with a Rotation Period of 2 Seconds (2007, background): “This is 1 small for the free-expansion stage of an SNR. Assuming instead that the SNR is already in the adiabatic (Sedov) phase, and following Vink & Kuiper (2006) who argued that the explosion energies of AXP remnants are no larger than those of ordinary pulsars, we find, for an explosion energy…”
• A Flaring Magnetar in FRB 121102? (2017, background): “By contrast, local magnetars have supernova shells with energies 1051~ erg (Vink & Kuiper 2006).”
• BRIGHT SUPERNOVAE FROM MAGNETAR BIRTH (2009, background): “This will affect the light curve, perhaps making it rise at an earlier time, and the morphology of the supernova remnant, perhaps leading to a “hole” in the remnant (Vink & Kuiper 2006; Kriss et al. 1985).”
• GIANT SPARKS AT COSMOLOGICAL DISTANCES? (2014, background): “There is little evidence that the inferred energy release in any Galactic supernova remnant, including those associated with magnetars, exceeds 1051 erg (Vink & Kuiper 2006).”
• A unified picture of Galactic and cosmological fast radio bursts (2020, background): “In contrast, Galactic magnetars were likely born with a more moderate initial spin, as evidenced by the limited energy in their surrounding supernova remnants (e.g., Vink & Kuiper 2006).”