Identifying intermittency events in the solar wind

By R. Bruno, V. Carbone, P. Veltri, E. Pietropaolo, B. Bavassano. 2001

261 citations recorded by the source corpus.

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Citations in the corpus

STATISTICAL ANALYSIS OF DISCONTINUITIES IN SOLAR WIND ACE DATA AND COMPARISON WITH INTERMITTENT MHD TURBULENCE (2009, methodology): “For the solar wind case, we divided the original ACE magnetic field data into subintervals of 12 hr and normalized the variable |ΔB| and its components to the standard deviations within each subinterval (Sorriso-Valvo et al. 1999; Bruno et al. 2001).”
Flux tube texture of the solar wind: Strands of the magnetic carpet at 1 AU?: FLUX TUBE TEXTURE OF SOLAR WIND (2008, methodology): “[3] The flux tube texture of the solar wind is depicted in Figure 1 [see also Bartley et al., 1966, Figure 6; Bruno et al., 2001, Figure 4].”
Solar Orbiter (2012, background): “The origin of these structures is uncertain: are they the remnant of complex coronal structuring in the form of strands of small-scale flux tubes advected by the solar wind flow (Borovsky, 2008; Bruno et al., 2001), or are they generated locally by turbulent fluctuations? At scales around the proton”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, background): “…space may be the result of the passage of multiple uncorrelated flux tubes past the spacecraft and not intrinsic turbulence within any one flux tube (see, e.g., McCracken & Ness 1966; Jokipii & Parker 1969; Bruno et al. 2001; Giacalone & Jokipii 2004; Giacalone et al. 2006; Borovsky 2006).”
Radial evolution of solar wind intermittency in the inner heliosphere (2003, unknown): “In reality, if we consider that compressive events cause intermittency (Veltri and Mangeney, 1991, Bruno et al., 2001), we might ascribe this different behavior to the fact that fast wind becomes more and more compressive with radial distance while the compressive level of slow wind remains…”
The Heliospheric Magnetic Field (2013, background): “These signatures have been interpreted and modeled as a magnetic flux rope (Burlaga, 1988; Lepping et al., 1990).”
Solar Wind Turbulence and the Role of Ion Instabilities (2013, background): “…1991; Tu and Marsch 1995; Carbone et al. 1995; Sorriso-Valvo et al. 1999; Veltri and Mangeney 1999; Veltri 1999; Salem 2000; Mangeney et al. 2001; Bruno et al. 2001; Sorriso-Valvo et al. 2001; Hnat et al. 2003; Veltri et al. 2005; Bruno and Carbone 2005; Leubner and Voros 2005; Jankovicova et…”
Intermittent MHD structures and classical discontinuities (2008, methodology): “In this ‘‘spaghetti’’ view, the tubes may tangle up in space, but remain distinct entities [e.g., see Bruno et al., 2001], with different magnetic field, density, temperature, etc.”