Synchrotron nebulae created by anisotropic magnetized pulsar winds

By Serguei Komissarov, Y. Lyubarsky. 2004

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Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/974d798d3fa0c1c3d99978ded15fad38e4e1dbeb

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ECHO: a Eulerian conservative high-order scheme for general relativistic magnetohydrodynamics and magnetodynamics (2007, background): “…2006), the acceleration of magnetized pulsar winds (Bucciantini et al. 2006) and the dynamics and emission properties of their related nebulae (Komissarov & Lyubarsky 2004; Del Zanna et al. 2004; Bucciantini et al. 2005; Del Zanna et al. 2006), the morphology and the dynamics of axisymmetric…”
ACCELERATION OF PARTICLES AT THE TERMINATION SHOCK OF A RELATIVISTIC STRIPED WIND (2011, background): “From the equatorial plane, radio-emitting electrons will quickly fill the whole nebula, transported by the strong fluid motions observed in MHD models of PWNe downstream from the termination shock (e.g., Komissarov & Lyubarsky 2004; Del Zanna et al. 2004; Camus et al. 2009).”
Simulations of the axisymmetric magnetospheres of neutron stars (2006, methodology): “This approach has already been successfully applied in recent MHD simulations of Pulsar Wind Nebulae (Komissarov & Lyubarsky 2004b).”
Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae (2011, background): “…observations have provided a rich suite of information, but we now need relativistic magnetohydrodynamic simulations to fully understand the flow conditions and instabilities that produce these effects (Komissarov & Lyubarsky 2004; Del Zanna et al. 2004; Bucciantini et al. 2005; Bucciantini 2010).”
Magnetized relativistic jets and long-duration GRBs from magnetar spin-down during core-collapse supernovae (2009, methodology): “By analogy with PWNe (Del Zanna, Amato & Bucciantini 2004; Komissarov & Lyubarsky 2004), we focused on the low-magnetization regime in which most (but not all) of the magnetic energy of the wind (associated with the toroidal component of the magnetic field) is assumed to be converted into bulk…”
The Crab Nebula as a standard candle in very high-energy astrophysics (2010, methodology): “A straightforward extension of the spherical KC84 model would be to incorporate an asymmetric flow with a modulated magnetization (see e.g. Komissarov & Lyubarsky 2004; Del Zanna et al. 2004; Del Zanna et al. 2006; Volpi et al. 2008).”
EFFICIENCY OF MAGNETIC TO KINETIC ENERGY CONVERSION IN A MONOPOLE MAGNETOSPHERE (2009, background): “…& Eichler 2001) is an alternative model to the more recent view that the observed jet is caused by a post-shock polar backflow withσ & 0.01 that is guided by hoop stresses and forced to converge toward (and rise up along) the rotation axis (Komissarov & Lyubarsky 2004; Del Zanna et al. 2004).”
Three-dimensional magnetohydrodynamic simulations of the Crab nebula (2013, methodology): “In order to check these ideas and study the 2D models in details, a number of groups carried out axisymmetric relativistic MHD simulations of pulsar wind nebulae (Komissarov & Lyubarsky 2003, 2004; Del Zanna, Amato & Bucciantini 2004; Bogovalov et al. 2005).”
The evolution and structure of pulsar wind nebulae (2006, background): “Moreover, modeling of the flow conditions across the shock shows that magnetic collimation produces jet-like flows along the rotation axis (Bogovalov et al. 2005, Komissarov & Lyubarsky 2004).”
Magnetic acceleration of ultrarelativistic jets in gamma-ray burst sources (2008, methodology): “To speed up the simulations, we implement a sectioning of the computational grid as described in Komissarov & Lyubarsky (2004).”
THE MAXIMUM ENERGY OF ACCELERATED PARTICLES IN RELATIVISTIC COLLISIONLESS SHOCKS (2013, background): “In this regard, we argue that the wind termination shock might form in a macroscopically turbulent medium, with the outer scale of the turbulence driven by the large-scale shear flows in the nebula (Komissarov & Lyubarsky 2004; Del Zanna et al. 2004; Camus et al. 2009).”
Magnetic acceleration of relativistic AGN jets (2007, methodology): “To speed up the simulations, we implemented a sectioning of the computational grid as described in Komissarov & Lyubarsky (2004).”
PARTICLE ACCELERATION IN RELATIVISTIC MAGNETIZED COLLISIONLESS PAIR SHOCKS: DEPENDENCE OF SHOCK ACCELERATION ON MAGNETIC OBLIQUITY (2009, background): “Recent relativistic MHD simulations of PWNe (Komissarov & Lyubarsky 2003, 2004; Del Zanna et al. 2004) have shown that polar jets with the observed velocities can develop provided that the magnetization of the relativistic (γ0 & 106) electron-positron pulsar wind is large enough (σ & 0.01) to…”