Simulations of the axisymmetric magnetospheres of neutron stars

By Serguei Komissarov. 2006

154 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/cd0c526f18365bb70cfe1723d41b667e742c7a53

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Spitkovsky
2. A. Tchekhovskoy
3. A. Philippov
4. Ramesh Narayan
5. J. Arons
6. J. McKinney
7. B. Cerutti
8. Jason G. Li

In Geophysics

1. J. Arons
2. A. Spitkovsky
3. A. Tchekhovskoy
4. J. McKinney
5. Jason G. Li
6. Ramesh Narayan
7. A. Harding
8. Demosthenes Kazanas

Citations in the corpus

• Three-dimensional numerical simulations of the pulsar magnetosphere: preliminary results (2008, result): “This solution has since been confirmed, improved, and generalized by several other authors (e.g. Gruzinov 2005; Contopoulos 2005; Timokhin 2006; Komissarov 2006; McKinney 2006).”
• Coherent emission mechanisms in astrophysical plasmas (2017, methodology): “FFE is used widely to model the global electrodynamics, particularly for the region r & rL covering the transition from the inner magnetosphere to the pulsar wind (Contopoulos et al, 1999; Gruzinov, 2005; Komissarov, 2006; Li et al, 2012b).”
• EFFICIENCY OF MAGNETIC TO KINETIC ENERGY CONVERSION IN A MONOPOLE MAGNETOSPHERE (2009, background): “Bogovalov (2001); Komissarov (2006); Bucciantini et al. (2006); Komissarov et al. (2009) have numerically simulated unconfined magnetized outflows and confirmed their low efficiency at converting magnetic to kinetic energy, i.e. the outflows remained highly magnetizedσ ≫ 1 out to the simulated…”
• ECHO: a Eulerian conservative high-order scheme for general relativistic magnetohydrodynamics and magnetodynamics (2007, background): “These results appear to be comparable to those presented by Komissarov (2006a), in spite of using a much simpler Riemann solver, and to those presented by Montero et al. (2007), who however considered an isentropic evolution.”
• Time-dependent 3D magnetohydrodynamic pulsar magnetospheres: oblique rotators (2012, methodology): “The first 2D MHD simulation of the aligned pulsar magnetosphere was presented by Komissarov (2006), K06 hereafter.”
• Particle acceleration in axisymmetric pulsar current sheets (2014, methodology): “At this point, the wind Lorentz factor follows almost exactly the linear increase of Γdrift with distance, in agreement with previous works (Buckley 1977; Contopoulos & Kazanas 2002; Komissarov 2006; Bucciantini et al. 2006).”
• TOWARD A REALISTIC PULSAR MAGNETOSPHERE (2011, background): “The axisymmetric solution has since been confirmed and further studied by several others (Gruzinov 2005; Timokhin 2006; Komissarov 2006; McKinney 2006), in particular with respect to its properties near the Y-point (the intersection of the last closed field line and the LC; Uzdensky 2003).”
• RESISTIVE SOLUTIONS FOR PULSAR MAGNETOSPHERES (2011, methodology): “One way to reintroduce accelerating electric fields in 1 We note that Komissarov (2006) has also calculated the structure of the aligned rotator in the relativistic MHD limit including particle inertia. ar X iv :1 10 7.”
• Pulsar Wind Nebulae as Cosmic Pevatrons: A Current Sheet’s Tale (2012, background): “…analytically minded theorists to guess the detailed answer uniformly failed over 30 years of trying), first for the aligned rotator (Contopoulos et al. 1999; Gruzinov 2005; Komissarov 2006; Timokhin 2006), then for the full 3D oblique rotator (Spitkovsky 2006; Kalapotharakos and Contopoulos 2009).”
• MODELING OF GAMMA-RAY PULSAR LIGHT CURVES USING THE FORCE-FREE MAGNETIC FIELD (2009, background): “The structure of the FF magnetosphere differs substantially from the rotating dipole field due to the poloidal current and the returning current sheet (Contopoulos et al. 1999; Gruzinov 2005; Komissarov 2006; McKinney 2006; Timokhin 2006).”