Evolution of the solar wind proton temperature anisotropy from 0.3 to 2.5 AU
By L. Matteini, S. Landi, P. Hellinger, F. Pantellini, M. Maksimović, M. Velli, B. Goldstein, Eckart Marsch. 2007
159 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/2014294d3581396d6504d81fef4944a0f53a2b47
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In Astronomy and Astrophysics
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Citations in the corpus
- SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES (2012, background): “However, for most of the solar wind observations, the plasma is stable (Matteini et al. 2007, 2011; Bale et al. 2009).”
- Power and spectral index anisotropy of the entire inertial range of turbulence in the fast solar wind (2010, background): “Ulysses high speed wind particle distributions are often close to the firehose instability threshold (Matteini et al. 2007, see also simulations by Hellinger & Travnicek 2008).”
- The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “These VDFs are constrained by wave-particle interactions via plasma instabilities (Kasper et al. 2002, 2013; Hellinger et al. 2006; Matteini et al. 2007, 2012, 2013; Bale et al. 2009, see Fig.”
- The Solar Orbiter magnetometer (2020, background): “Non-Maxwellian plasma populations and temperature anisotropies (e.g. Matteini et al. 2007; Chen et al. 2016) can drive instabilities which heat the plasma and drive waves and other fluctuations.”
- ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “…way by the marginal stability boundaries for the mirror and firehose (Gary et al. 2001; Kasper et al. 2002; Marsch et al. 2004; Hellinger et al. 2006; Matteini et al. 2007).41 If we want to study turbulence in data sets that do not lie too close to these stability boundaries, assuming an…”
- Solar Wind Turbulence and the Role of Ion Instabilities (2013, background): “2013) or ion anisotropy instabilities (Gary et al. 2001; Matteini et al. 2007, 2011; Bale et al. 2009) may be responsible for the spectral variability within the transition range.”
- EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “Observationally, these departures are not significantly large over most of the distances considered here (see Marsch et al. 1982; Pilipp et al. 1990; Matteini et al. 2007).”