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Pulsar-Wind Nebulae

Recent Progress in Observations and Theory

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Abstract

In this review we describe recent observational and theoretical developments in our understanding of pulsar winds and pulsar-wind nebulae (PWNe). We put special emphasis on the results from observations of well-characterized PWNe of various types (e.g., torus-jet and bowshock-tail), the most recent MHD modeling efforts, and the status of the flaring Crab PWN puzzle.

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Notes

  1. Such classification is possible only for sufficiently bright and relatively nearby PWNe.

  2. A more detailed overview of the observational properties of population of relic PWNe can be found in Kargaltsev et al. (2013b).

  3. Since the PWN properties and evolution depend on the environment, one should not forget that the progenitor and SNR properties may be quite different for the Crab and Vela pulsars.

  4. See animation at http://home.gwu.edu/~kargaltsev/Crab.html.

  5. Overall, the large degree of correlation between the radio structure and optical filaments suggests than most of the radio emission is related to the SNR filaments.

  6. However, one can imagine that the jet stayed at one position (“3” in Fig. 2) for a long time and then relatively quickly moved to the other position (“1” in Fig. 2).

  7. The outer edge of the optical/NIR wisp is about \(1''\) further away from the pulsar, with the X-ray ring emission trailing behind or possibly being sandwiched between the bright wisp and the fainter wisp.

  8. Here we are following nomenclature introduced by Hester et al. (1995), see Fig. 1 (top panel).

  9. In principle, the magnetic field may deviate from the dipolar configuration more for the Vela pulsar than for the Crab pulsar. Indeed, braking indices, \(n\), of the Crab (\(n=2.5\)) and Vela (\(n=1.4\)) are very different, and the Vela pulsar is much more “glitchy” compared to Crab.

  10. The parameter that determines to what degree a PWN is affected by the pulsar motion is the ratio of the pulsar velocity to the local ambient sound speed (Mach number ℳ). The medium within the younger Crab SNR is hotter than in the Vela SNR.

  11. Here the distances are scaled as \(d_{0.3}=d/(300~\mbox{pc})\) and \(d_{2}=d/2{,}000~\mbox{pc}\).

  12. It is likely that the Mach number is somewhat larger for the Vela PWN where we see some effect of the motion (Pavlov et al. 2003).

  13. In the Radhakrishnan and Deshpande (2001) model the arcs are the traces of the particle beams from the two magnetic poles and the inner jets are the Doppler-boosted projections of the beams.

  14. Alternatively, an old SNR can break-up and dissolve.

  15. The simulations of Bucciantini et al. (2005) do not extend further than \(25r_{cd,0}\) (where \(r_{cd,0}\) is the scant-off distance at the apex of the bowshock) from the pulsar due to numerical challenges. Also, the model neglects the impact of the magnetic field on the flow dynamics. It is reasonable to expect that the pulsar tail physics may have some similarities with that of leptonic AGN jets for the case when the pulsar spin axis are parallel to its velocity vector (except that magnetic hoop stress may turn out to be larger in the case of pulsar tails). Therefore, some of the AGN jet simulations may be relevant for the pulsar tails.

  16. The simulations by Vigelius et al. (2007) only extended for a few \(r_{cd,0}\) from the pulsar, much smaller than the scales of extended tails seen in X-rays.

  17. The angle between the line of sight and the pulsar velocity vector.

  18. The X-ray flux of the Crab Nebula is also variable but to a \(\sim10~\%\) level over a year-timescale (Wilson-Hodge et al. 2011). This will not be discussed here, because this phenomenon does not appear to be directly connected to the flares.

  19. See http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/Crab_Pulsar.

  20. The flux of the inverse-Compton component above \(>100~\mbox{GeV}\) remains constant during the flares (H.E.S.S. Collaboration et al. 2014; Aliu et al. 2014).

  21. This might be challenging to achieve in relativistic shocks (Sironi and Spitkovsky 2009b).

  22. This solution is often proposed to account for the ultra-rapid gamma-ray flares in blazars.

  23. Recent studies show that reconnection produces hard particle spectra \(d\mathrm{N}/d\gamma\propto\gamma^{-1}\), \(\gamma ^{-1.5}\) for \(\sigma\gg1\) (Sironi and Spitkovsky 2014; Guo et al. 2014; Werner et al. 2014).

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Acknowledgements

We thank George Pavlov for his valuable comments and discussions. We are grateful to Blagoy Rangelov for creating the merged F550M Crab image from the archival HST data and help with the manuscript editing. We acknowledge support from NASA grants AR8-9009X, GO3-14084X, GO3-14057C, G03-14082A, NNX09AC81G, NNX09AC84G, HST-GO-13043.09, and G02-13085C. B.C. acknowledges support from the Lyman Spitzer Jr. Fellowship awarded by the Department of Astrophysical Sciences at Princeton University, and the Max-Planck/Princeton Center for Plasma Physics. Y.L. acknowledges support from Israeli Science Foundation under the grant 719/14.

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Kargaltsev, O., Cerutti, B., Lyubarsky, Y. et al. Pulsar-Wind Nebulae. Space Sci Rev 191, 391–439 (2015). https://doi.org/10.1007/s11214-015-0171-x

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  • DOI: https://doi.org/10.1007/s11214-015-0171-x

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