Abstract
We review observations of several classes of neutron-star-powered outflows: pulsar-wind nebulae (PWNe) inside shell supernova remnants (SNRs), PWNe interacting directly with interstellar medium (ISM), and magnetar-powered outflows. We describe radio, X-ray, and gamma-ray observations of PWNe, focusing first on integrated spectral-energy distributions (SEDs) and global spectral properties. High-resolution X-ray imaging of PWNe shows a bewildering array of morphologies, with jets, trails, and other structures. Several of the 23 so far identified magnetars show evidence for continuous or sporadic emission of material, sometimes associated with giant flares, and a few “magnetar-wind nebula” have been recently identified.












































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Notes
In this Section the subscript of \(d\) means the scaling distance in kpc.
Note that \(\gamma_{\mathrm{max}}m_{e}c^{2}\sim e\varPhi \sigma /(\sigma +1)\), where \(\varPhi =B_{\mathrm{LC}}R_{\mathrm{LC}}\sim B_{\mathrm{NS}}R_{\mathrm{NS}}^{3} \varOmega^{2}/c ^{2}\) is the potential drop across the pulsar’s polar cap, \(R_{\mathrm{LC}}=c/ \varOmega \) is the light cylinder radius, \(\varOmega =2\pi /P\), \(B_{\mathrm{LC}}\) and \(B_{\mathrm{NS}}\) are the magnetic field values at the light cylinder and the neutron star surface. The maximum electron energies in other acceleration models (e.g., Romanova et al. 2005) are also fractions of \(e\varPhi \).
It can differ from the pulsar’s proper motion if the pulsar moves in a non-uniform ambient medium, but we will neglect this difference here.
We should note, however, that such estimates assume that the magnetic field strength is about the same throughout the emitting volume, which may be far from reality.
One should bear in mind, however, that much smaller spatial scales can be probed in the nearby Geminga PWN than in the Mouse.
Chatterjee and Cordes (2002) estimated \(\theta_{0}=0\stackrel {''}{.}06\pm 0\stackrel {''}{.}02\) from modeling an H\(\alpha \) image obtained with the Hubble Space Telecope.
In what follows, the angular resolutions are provided as the 68% containment radii. The Fermi-LAT sensitivity is given at \(\mbox{TS} = 25\) in 10 y, for a source at \((\ell , b) = (0^{ \circ} , 30^{\circ })\) with Pass 8 data (https://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm). The H.E.S.S. sensitivity is provided at 5 \(\sigma \) in 25 h, for a source near zenith (https://www.mpi-hd.mpg.de/hfm/HESS/pages/home/proposals/). See also the dashed lines in Fig. 38.
From Abramowski et al. (H.E.S.S. Collaboration) 2016, in prep. See also https://www.mpi-hd.mpg.de/hfm/HESS/pages/home/som/2016/01/.
The possibility that a hadronic component could carry a significant fraction of the energy content in PWNe has been investigated in several works (see Di Palma et al. 2016 and references therein), but the observational evidence of the presence of accelerated ions in PWNe, through e.g. pion production in hadronic interactions and the subsequent emission of \(\gamma \)-rays and neutrinos, has been so far elusive.
The modeling presented in Vorster et al. (2013) assumes that the particle spectrum has a discontinuity at the transition between the low- and high-energy components.
The luminous blue variable star LBV 1806-20 (Figer et al. 2004).
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Acknowledgements
SPR thanks the NuSTAR team for their outstanding work and permission to present their PWN results. GGP, OK, and NK are grateful to Andrei Bykov and Maxim Lyutikov for helpful discussions, and to Blagoy Rangelov and Bettina Posselt for their help in data analysis. Support for their work was provided by the National Aeronautics and Space Administration through Chandra Awards G03-14082 and G03-14057 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. The work was also partly supported by NASA grant NNX08AD71G. MR is grateful to Jamie Cohen and Marco Ajello for providing the Fermi-LAT 2FHL image towards HESS J1356-645 and to Marie-Hélène Grondin for the Fermi-LAT images of Vela X.
All of us warmly thank the organizers for the invitation to participate in this very stimulating ISSI workshop on Jets and Winds in Pulsar Wind Nebulae, Gamma-ray Bursts and Blazars: Physics of Extreme Energy Release, and the International Space Science Institute (ISSI) for support.
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Reynolds, S.P., Pavlov, G.G., Kargaltsev, O. et al. Pulsar-Wind Nebulae and Magnetar Outflows: Observations at Radio, X-Ray, and Gamma-Ray Wavelengths. Space Sci Rev 207, 175–234 (2017). https://doi.org/10.1007/s11214-017-0356-6
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DOI: https://doi.org/10.1007/s11214-017-0356-6