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تسجيل مستخدم جديدExpansion of Kes 73, a Shell Supernova Remnant Containing a Magnetar
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Of the 30 or so Galactic magnetars, about 8 are in supernova remnants (SNRs). One of the most extreme magnetars, 1E 1841-045, is at the center of the SNR Kes 73 (G27.4+0.0), whose age is uncertain. We measure its expansion using three Chandra observations over 15 yr, obtaining a mean rate of 0.023% +/- 0.002% per yr. For a distance of 8.5 kpc, we obtain a shell velocity of 1100 km/s and infer a blast-wave speed of 1400 km/s. For Sedov expansion into a uniform medium, this gives an age of 1800 yr. Derived emission measures imply an ambient density of about 2 cm$^{-3}$ and an upper limit on the swept-up mass of about 70 solar masses, with lower limits of tens of solar masses, confirming that Kes 73 is in an advanced evolutionary stage. Our spectral analysis shows no evidence for enhanced abundances as would be expected from a massive progenitor. Our derived total energy is $1.9 times 10^{51}$ erg, giving a very conservative lower limit to the magnetars initial period of about 3 ms, unless its energy was lost by non-electromagnetic means. We see no evidence of a wind-blown bubble as would be produced by a massive progenitor, or any evidence that the progenitor of Kes 73/1E 1841-045 was anything but a normal red supergiant producing a Type IIP supernova, though a short-lived stripped-envelope progenitor cannot be absolutely excluded. Kes 73s magnetar thus joins SGR 1900+14 as magnetars resulting from relatively low-mass progenitors.
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Most of the proposed associations between magnetars and supernova remnant suffer from age problems. Usually, supernova remnants ages are determined from an approximation of the Sedov-Taylor phase relation between radius and age, for a fixed energy of
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