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Pulsars and Magnetars

  • Particles and Fields
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Abstract

The high-energy sources known as anomalous X-ray pulsars (AXPs) and soft γ-ray repeaters (SGRs) are well explained as magnetars: isolated neutron stars powered by their own magnetic energy. After explaining why it is generally believed that the traditional energy sources at work in other neutron stars (accretion, rotation, residual heat) cannot power the emission of AXPs/SGRs, I review the observational properties of the 20 AXPs/SGRs currently known and describe the main features of the magnetar model. In the last part of this review, I discuss the recent discovery of magnetars with low external dipole field and some of the relations between AXPs/SGRs and other classes of isolated neutron stars.

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Notes

  1. Some authors distinguish between these two designations, calling SGRs only the sources which showed episodes of many repeated and intense bursts. In this review, I will not make such a distinction and I refer to the whole group of objects as AXPs/SGRs.

  2. The moment of inertia of a NS with mass M and radius R is in the range ∼ (0.5 − 1) × 1045 (\(M/M_{\odot }\)) (\(R/10 ~km)^{2}\) g cm2 for most equations of state.

  3. Only one pulsar more energetic than the Crab is currently known: the 16-ms pulsar in the Large Magellanic Cloud PSR J0537–6960, which has Ė rot = 5 × 1038 erg s−1.

  4. Some AXPs/SGRs reach quiescent luminosity levels below their Ė rot , but during outburst they are as luminous as the persistent ones.

  5. Sco X-1 was the second observed NS, the first one being the NS in the Crab nebula, shining as a 16-magnitude object in the visible band. Both were clearly understood as NSs only after the discovery of radio pulsars in 1968.

  6. Another energy source is provided by nuclear reactions. This powers the type I bursts observed in many accreting low-mass X-binaries. The properties of SGR bursts are very different from those of type I bursts.

  7. The giant flares (Section 3.1) in which up to ∼ 1046 ergs can be released, are energetically more challenging. This limits the number of such events that a magnetar can emit in its lifetime.

  8. B d is the value on the star surface at the magnetic equator. The surface field at the pole is a factor of two larger.

  9. See [41] for a different interpretation in terms of an accretion-based model.

  10. Here and in the following, we quote luminosities for isotropic emission.

  11. \(B_{QED}\) is the magnetic field for which the energy of the first Landau level of the electron equals its rest mass. It was often regarded as the boundary between normal pulsars and magnetars, although there is no real physical reason or threshold effect to motivate this.

  12. Two isolated bursts were detected in October and November 2001 from 1E 1048.1−5937 [59], but 1E 2259 + 586 in June 2002 emitted more than 80 bursts in 4 h, associated to an increase of the persistent flux and a glitch.

  13. Unless interaction with a residual disk is invoked [3].

  14. Despite the lack of a radio detection, which could be due to an unfavorable orientation of the radio beam.

  15. Also known with the “Magnificent Seven” nickname.

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Acknowledgments

I thank Paolo Esposito and Roberto Turolla for their careful reading of this work and useful comments.

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    Sandro Mereghetti

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Mereghetti, S. Pulsars and Magnetars. Braz J Phys 43, 356–368 (2013). https://doi.org/10.1007/s13538-013-0137-y

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