A new model of a magnetar |
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Authors: | I F Malov G Z Machabeli V M Malofeev |
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Institution: | (1) Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Leninskii pr. 53, Moscow, 117924, Russia;(2) Abastumani Astrophysical Observatory, Academy of Sciences of Georgia, Gora Kanobili, Abastumani, 383762, Georgia |
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Abstract: | A new model is put forward to explain the observed features of anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs). It is shown that drift waves can be excited in the magnetosphere of a neutron star with a rotational period of P~0.1 s, surface magnetic field Bs~1012 G, and angle between the rotational axis and magnetic moment β<10°. These waves lead to the formation of radiation pulses with a period of Pdr~10 s. The rate of loss of rotational energy by such a star (~1037 erg/s) is sufficient to produce the observed increase in the period \((\dot P \sim 10^{ - 10} )\), the X-ray luminosities of AXPs and SGRs (~1034–1036 erg/s), and an injection of relativistic particles into the surrounding supernova remnant. A modulation of the constant component of the radiation with a period of P~0.1 s is predicted. In order for SGRs to produce gamma-ray bursts, an additional source of energy must be invoked. Radio pulsars with periods of Pobs>5 s can be described by the proposed model; in this case, their rotational periods are considerably less than Pobs and the observed pulses are due to the drift waves. |
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