Abstract
We discuss the role of PIC simulations in unveiling the origin of the emitting particles in PWNe. After describing the basics of the PIC technique, we summarize its implications for the quiescent and the flaring emission of the Crab Nebula, as a prototype of PWNe. A consensus seems to be emerging that, in addition to the standard scenario of particle acceleration via the Fermi process at the termination shock of the pulsar wind, magnetic reconnection in the wind, at the termination shock and in the Nebula plays a major role in powering the multi-wavelength signatures of PWNe.
Both authors contributed equally to this chapter.
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Notes
- 1.
Other efficient methods exists as for instance the particle pusher developed by VayĀ (2008).
- 2.
The total particle charge is conserved, but not necessarily the charge deposited on the grid.
- 3.
- 4.
Typically, pushing particles and depositing currents take 90% of the computing time (without communications), this is the reason why load-balancing is so critical in PIC.
- 5.
- 6.
The parameter Īµ B denotes the magnetization of the turbulence, Īµ B ā=āĪ“B 2ā8ĻĪ³ 0 Ļ 0 c 2, where Ī“B is the fluctuating magnetic field and Ļ 0 is the mass density of the pre-shock flow. This should not be confused with the magnetization Ļ = B 0 2ā4ĻĪ³ 0 Ļ 0 c 2, which quantifies the strength of the pre-existing ordered upstream field B 0.
- 7.
This scaling is shallower than the so-called (and commonly assumed) Bohm limit Ī³ max ā t, and it naturally results from the small-scale nature of the Weibel turbulence generated in the shock layer (see Fig.ā11.6).
- 8.
The wavelength Ī» of the striped wind equals cāP, where P is the pulsar period.
- 9.
- 10.
The reconnection rate is measured to be in the range v recāc ā¼ 0.ā2 ā 0.ā5, which increases with the magnetization and saturates at around 0.5 at high magnetization limit (Lyutikov etĀ al.Ā 2016).
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LS acknowledges support from DoE DE-SC0016542 and NASA Fermi NNX16AR75G. BC acknowledges support from CNES and Labex OSUG@2020 (ANR10 LABX56).
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Sironi, L., Cerutti, B. (2017). Particle Acceleration in Pulsar Wind Nebulae: PIC Modelling. In: Torres, D. (eds) Modelling Pulsar Wind Nebulae. Astrophysics and Space Science Library, vol 446. Springer, Cham. https://doi.org/10.1007/978-3-319-63031-1_11
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