Astrophys. J., 707, 844-851 (2009/December-2)
The progenitor mass of the magnetar SGR1900+14.
DAVIES B., FIGER D.F., KUDRITZKI R.-P., TROMBLEY C., KOUVELIOTOU C. and WACHTER S.
Abstract (from CDS):
Magnetars are young neutron stars with extreme magnetic fields (B ≳ 1014-1015 G). How these fields relate to the properties of their progenitor stars is not yet clearly established. However, from the few objects associated with young clusters it has been possible to estimate the initial masses of the progenitors, with results indicating that a very massive progenitor star (Mprog> 40 M) is required to produce a magnetar. Here, we present adaptive-optics assisted Keck/NIRC2 imaging and Keck/NIRSPEC spectroscopy of the cluster associated with the magnetar SGR 1900+14, and report that the initial progenitor star mass of the magnetar was a factor of 2 lower than this limit, Mprog = 17±2 M. Our result presents a strong challenge to the concept that magnetars can only result from very massive progenitors. Instead, we favor a mechanism which is dependent on more than just initial stellar mass for the production of these extreme magnetic fields, such as the "fossil-field" model or a process involving close binary evolution.
open clusters and associations: individual: Cl 1900+14 - stars: evolution - stars: individual: SGR1900+14 - stars: neutron
Fig. 1: [DFK2009] NNa (Nos 1a-1d, 4a-4b, 5a-5b, 6a-6b, 7a-7d, 8a-8b, 9a-9c, 10a-10b), [DFK2009] Aa (Nos Ba-Bd, Ca-Cb). Fig. 2, Table 2: [DFK2009] NN (Nos 13, 15).
Cl 1813-13 is a misprint for Cl 1813-18 which is object [MFD2008] Stellar Cluster in SIMBAD.
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