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- W72645412 abstract "Context. The recent observations of SGR 0418+5729 offer an authentic Rosetta Stone for deciphering the energy source of Soft Gamma Ray Repeaters (SGRs) and Anomalous X-ray Pulsars (AXPs). The “magnetar” model, appeals to a yet untested new energy source in astrophysical systems: bulk magnetic energy. It leads for SGR 0418+5729 to results in contradiction with observations. Aims. It is shown how a consistent model for SGRs and AXPs can be expressed in terms of canonical physics and astrophysics within massive, fast rotating, and highly magnetized white dwarfs. Methods. The pioneering work of B. Paczynski (1990) on 1E 2259+586 is extended and further developed to describe the observed properties of all known SGRS and AXPs by assuming spin-down powered massive, fast rotating, and highly magnetized white dwarfs. Results. Within this model, we obtain the theoretical prediction for the lower limit of the first time derivative of the rotational period of SGR 0418+5729, Ṗ ≥ LXP/(4πI) = 1.18 × 10−16 s/s being LX and P the observed X-ray luminosity and rotational period of the source, and I the moment of inertia of the white dwarf. Besides the case of SGR 0418+5729, we also show that the energetics of all SGRs and AXPs, including their outburst activities can be well explained through the change of rotational energy of the white dwarf, associated to the observed sudden changes of the rotational period. For all sources, we find a surface dipole magnetic field 7.5 × 108G . B . 2.1 × 1011G, well below the critical field Bc = mec 3/(e~) = 4.42 × 1013 G. Conclusions." @default.
- W72645412 created "2016-06-24" @default.
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- W72645412 date "2011-02-03" @default.
- W72645412 modified "2023-09-25" @default.
- W72645412 title "SGRs and AXPs: Massive Rotating White Dwarfs versus Magnetars" @default.
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