Pulsar wind nebulae in supernova remnants Spherically symmetric hydrodynamical simulations

By E. Swaluw, A. Achterberg, Y. Gallant, G. T'oth. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Axially symmetric relativistic MHD simulations of Pulsar Wind Nebulae in Supernova Remnants. On the origin of torus and jet-like features (2004, methodology): “For similar settings see van der Swaluw et al. (2001), Blondin et al. (2001), Bucciantini et al. (2003, 2004).”
The population of TeV pulsar wind nebulae in the H.E.S.S. Galactic Plane Survey (2017, background): “73 for t < τ0 in van der Swaluw et al. (2001) and R ∼ t0.”
The evolution and structure of pulsar wind nebulae (2006, background): “In the presence of a young pulsar, the inward moving SNR reverse shock collides with the outward moving PWN forward shock after a time tcoll < tSedov, typically a few thousand years (van der Swaluw et al. 2001, Blondin et al. 2001).”
Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae (2011, background): “…compresses the PWN, and the system may reverberate for a couple of cycles before establishing a new equilibrium (Blondin et al. 2001; van der Swaluw et al. 2001; Gelfand et al. 2009) The compression of the PWN raises the internal magnetic field, resulting in substantial synchrotron burnoff…”
Dust formation and survival in supernova ejecta (2007, methodology): “D hydrodynamical models of SN blast waves of van der Swaluw et al. (2001) and with simulations kindly provided by L. Del Zanna (based on the code described in Del Zanna et al. 2003).”
Chandra Imaging of the X-Ray Nebula Powered by Pulsar B1509–58 (2001, background): “Since the PWN itself has a sound speedc/ √ 3, this condition can only be met if the reverse shock from the surrounding SNR has collided with the PWN, bringing thermal material to the center of the system (Chevalier 1998; van der Swaluw et al. 2001; Blondin, Chevalier, & Frierson 2001).”
Three-dimensional magnetohydrodynamic simulations of the Crab nebula (2013, methodology): “We can hence utilise the hydrodynamic results obtained by means of the thin shell approximation for the forward PWN shock (e.g. van der Swaluw et al. 2001) and use the resulting index αr = 6/5 as our reference value.”
Young Core-Collapse Supernova Remnants and Their Supernovae (2004, background): “=3 fluid (Ostriker & Gunn 1971; Reynolds & Chevalier 1984; Chevalier & Fransson 1992; van der Swaluw et al. 2001).”