The evolution and structure of pulsar wind nebulae

By B. Gaensler, P. Slane. 2006

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AbstractPulsars steadily dissipate their rotational energy via relativistic winds. Confinement of these outflows generates luminous pulsar wind nebulae, seen across the electromagnetic spectrum in ...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9cd51f8a22625e8225d019af896b4659725e39f7

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Citations in the corpus

Supernova remnants: the X-ray perspective (2011, background): “These particles advect and diffuse away from the shock creating a nebula of relativistic electron/positrons which emit synchrotron radiation from the radio to the soft γ-ray bands, and inverse Compton scattering from soft γ-ray to the TeV band (Gaensler and Slane, 2006, for a review).”
Teraelectronvolt Astronomy (2010, background): “Many of the fundamental concepts concerning PWNe are summarized in the seminal papers by Rees & Gunn (1974) and Kennel & Coroniti (1984); for a recent summaries see Gaensler & Slane (2006).”
Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes (2010, background): “This is supported by observations since pulsar wind nebulae (PWNe) are sometimes found inside or close to the shells of SNRs (see e.g. Gaensler & Slane 2006; Bucciantini 2008, for recent reviews on PWNe), though many pulsars remain non-associated5.”
Gamma-ray binaries and related systems (2013, background): “The non-thermal emission is thought to be due to high energy particles that are scattered and accelerated at the shock, as in pulsar wind nebulae (PWN, see e.g. Gaensler & Slane 2006, for a review).”
Pulsars versus dark matter interpretation of ATIC/PAMELA (2009, background): “20 kyr; [24]) is much smaller than the typical propagation time t & 100 kyr [Eq.”
Pulsar Wind Nebulae as Cosmic Pevatrons: A Current Sheet’s Tale (2012, background): “Pulsar Wind Nebulae (PWNe) demonstrate that pulsars lose rest mass at a rate large compared to the fiducial electrodynamic particle loss rate cΦmag/e (for a review of PWNe phenomenology, see Gaensler and Slane 2006).”
THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION (2013, background): “High-resolution Chandra and XMM-Newton observations of the Crab Nebula and other young PWNe typically show a “jet-torus” structure on arcminute or smaller scales (see Gaensler & Slane 2006 for a review).”
The population of TeV pulsar wind nebulae in the H.E.S.S. Galactic Plane Survey (2017, background): “The present spin-down luminosity can be calculated from the period P and its time derivative Ṗ (Gaensler & Slane 2006, Eq.”
Sensitivity of the high altitude water Cherenkov detector to sources of multi-TeV gamma rays (2013, background): “Pulsar Wind Nebulae (PWN) are the most common Galactic source of TeV gamma rays [26,27].”
A CATALOG OF X-RAY POINT SOURCES FROM TWO MEGASECONDS OF CHANDRA OBSERVATIONS OF THE GALACTIC CENTER (2008, background): “…still have latent heat from what was once the stellar core (Walter et al. 1996), if they accelerate particles in rotating, moderate-strength (B ∼ 1012 G) fields (Gaensler & Slane 2006), or if they have extremely strong fields (B ∼ 1014 G) that decay and accelerate particles (Woods & Thompson 2006).”
Millisecond Magnetar Birth Connects FRB 121102 to Superluminous Supernovae and Long-duration Gamma-Ray Bursts (2017, background): “Magnetar Wind Nebula As in other young pulsar wind nebulae (Gaensler & Slane 2006), the rotationally powered wind from the magnetar inflates a nearly spherical bubble of relativistic electron/positron pairs behind the SN ejecta (Metzger et al. 2014; Murase et al. 2016).”
45 years of rotation of the Crab pulsar (2014, background): “The Crab pulsar, along with other young pulsars, generates a powerful particle stream whose effect is observed as a wind nebula (e.g. Gaensler & Slane (2006)).”
MILAGRO OBSERVATIONS OF MULTI-TeV EMISSION FROM GALACTIC SOURCES IN THE FERMI BRIGHT SOURCE LIST (2009, background): “One possible explanation for the pulsar variation is that the pulsed emission is expected to be beamed (and thus viewing-angle dependent) and the unpulsed multi-TeV emission is likely unbeamed (Gaensler & Slane 2006).”
DUST PRODUCTION AND PARTICLE ACCELERATION IN SUPERNOVA 1987A REVEALED WITH ALMA (2013, background): “If the neutron star energizes a pulsar wind nebula (PWN), its emission would most likely have a spectrum with power-law spectral index of − 0.3 to 0 (Gaensler & Slane 2006), ﬂatter than synchrotron emission from the shock, perhaps detectable at millimeter wavelengths or even contributing to the…”
A Flaring Magnetar in FRB 121102? (2017, background): “The same calculation of freeze-out N should apply to ordinary PWN with V 108~ cm s−1 and 1031m ~ G cm3, which gives a large N.”
The Crab Nebula: An Astrophysical Chimera (2008, background): “The general problem of pulsar winds and PWN has been discussed recently in a number of reviews including those of Arons (2008) and Gaensler & Slane (2006), so further discussion here will focus on the specific properties of the PWN in the Crab.”