The Solar Wind as a Turbulence Laboratory

By R. Bruno, V. Carbone. 2005

1,263 citations recorded by the source corpus.

In this review we will focus on a topic of fundamental importance for both astrophysics and plasma physics, namely the occurrence of large-amplitude low-frequency fluctuations of the fields that describe the plasma state. This subject will be treated within the context of the expanding solar wind and the most meaningful advances in this research field will be reported emphasizing the results obtained in the past decade or so. As a matter of fact, Helios inner heliosphere and Ulysses’ high latitude observations, recent multi-spacecrafts measurements in the solar wind (Cluster four satellites) and new numerical approaches to the problem, based on the dynamics of complex systems, brought new important insights which helped to better understand how turbulent fluctuations behave in the solar wind. In particular, numerical simulations within the realm of magnetohydrodynamic (MHD) turbulence theory unraveled what kind of physical mechanisms are at the basis of turbulence generation and energy transfer across the spectral domain of the fluctuations. In other words, the advances reached in these past years in the investigation of solar wind turbulence now offer a rather complete picture of the phenomenological aspect of the problem to be tentatively presented in a rather organic way.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0d4fdf8c240ddd46724863095ca2e1b7475fa562

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Citations in the corpus

The magnetic field in the solar atmosphere (2014, background): “wind (Marsch 2006; Ofman 2010; Bruno and Carbone 2013), space weather (Schwenn 2006), and the heliospheric magnetic field (Owens and Forsyth 2013).”
Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, background): “Solar wind turbulence (see Bruno and Carbone 2013, for a recent review) should also have an important role in driving ULF waves, e.g. by the pressure fluctuations associated with them.”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “…magnetic field is typically steeper (∼ k−5/3) than the velocity power spectrum in spacecraft measurements (Matthaeus & Goldstein 1982; Goldstein et al. 1995; Bruno & Carbone 2005; Podesta et al. 2007; Chen et al. 2011) and direct numerical simulations (Müller & Grappin 2005; Boldyrev et al. 2011).”
Kinetic Physics of the Solar Corona and Solar Wind (2006, background): “Recently in this journal, two modern and comprehensive reviews have become available, by Bruno and Carbone (2005) on the solar wind as a turbulence laboratory, an article which partly covers kinetic issues as well, and by Nakariakov and Verwichte (2005) on the novel subject of coronal waves and…”
Magnetic Turbulence in the Geospace Environment (2010, result): “As a matter of fact, the obtained experimental results do not allow to firmly distinguish between Kolmogorov (α = 5/3) and Kraichnan (α = 3/2) spectra (Bruno and Carbone 2005), that is, between hydrodynamic and MHD scalings, respectively.”
Cascades and transitions in turbulent flows (2018, background): “It is met in a variety of systems such as in the stellar interiors [345], the solar wind [346, 347], accretion disks [348] and the galaxies [349, 350] but also in industrial applications [92, 351].”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, methodology): “…Alfvénic fluxes are measured in the fast solar wind, where the influence of initial conditions in the solar atmosphere is more pronounced, while the slow-wind turbulence is approximately balanced (Marsch & Tu 1990a; see also reviews by Tu & Marsch 1995; Bruno & Carbone 2005 and references therein).”
Turbulence transport throughout the heliosphere (2007, background): “[2] It is now well established that the radial evolution of interplanetary hydromagnetic turbulence in the heliosphere is not fully accounted for by theories based on noninteracting waves, such as WKB theory [e.g., Bavassano et al., 1982a, 1982b; Roberts et al., 1987a, 1987b; Matthaeus et al., 1990;”
The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “Thus, turbulence in fast solar wind streams and also in slower streams that are far from the plasma and current sheets are dominated by Alfvénic fluctuations (Bruno and Carbone 2005, 2013; Telloni et al. 2015).”
PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, background): “The valuec3 = 5/3 is suggested by in situ measurements of magnetic-field fluctuations in the solar wind (Matthaeus and Goldstein 1982; Bruno and Carbone 2005), as well as some theoretical and numerical studies of MHD turbulence (Goldreich and Sridhar 1995; Cho and Vishniac 2000).”
Slow Solar Wind: Observations and Modeling (2016, positive): “The magnetic fluctuations spectra in the solar wind as observed in situ by the various spacecraft often exhibit power law scaling with turbulent spectrum in the inertia range that agrees with Kolmogorov turbulence scaling of −5/3, and steeper slope in the high frequency (above the proton gyroresonat”
In-situ Switchback Formation in the Expanding Solar Wind (2020, positive): “Figure 2c also shows that |B| remains fairly constant despite large fluctuations in B, as ubiquitously observed in solar-wind data (Belcher & Davis 1971; Barnes 1981; Bruno & Carbone 2013).2 Time traces in the lower panels illustrate several other relevant simulations.”
Anisotropy of Alfvénic turbulence in the solar wind and numerical simulations (2010, background): “1 IN T RO D U C T I O N The solar wind is a turbulent plasma (see reviews by Goldstein, Roberts & Matthaeus 1995; Bruno & Carbone 2005; Horbury, Forman & Oughton 2005) with a power spectrum extending over many orders of magnitude (e.g. Coleman 1968).”