Parametric decay of circularly polarized Alfvén waves: Multidimensional simulations in periodic and open domains

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Alfvén Waves and Turbulence in the Solar Atmosphere and Solar Wind (2007, background): “Geophys., 20, 1265 Casalbuoni, S., Del Zanna, L., Habbal, S. R., & Velli, M. 1999, J. Geophys.”
The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere (2019, background): “One possible reason for the slow mode component to increase as the solar wind travels from the Sun is continual local driving, e.g., from velocity shears (Roberts et al. 1992) or parametric decay (Del Zanna et al. 2001; Tenerani & Velli 2013; Bowen et al. 2018a).”
Coronal Holes and the High-Speed Solar Wind (2002, background): “…(e.g., Poedts et al. 1998) and the nonlinear production of “daughter” waves from an input “mother” (via, e.g., decay or modulational instabilities; see Vasquez and Hollweg 1999; Del Zanna et al. 2001; and references therein) have produced a wide variety of results applicable to the solar wind.”
Alfvén Waves in the Solar Atmosphere (2012, background): “Numerical simulations of the time evolution of large amplitude Alfvén waves have confirmed the development of this instability in the solar wind (Malara et al. 2000a; Del Zanna et al. 2001).”
Athena: A New Code for Astrophysical MHD (2008, background): “Although suchwaves are subject to a parametric instability (Del Zanna et al. 2001), for the parameters adopted by T2000 no instability should be present.”