Solar wind proton temperature anisotropy: Linear theory and WIND/SWE observations

By P. Hellinger, P. Trávnícek, Justin C. Kasper, A. Lazarus. 2006

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Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/8c06027aa841b2861af4e9f828e2977dbc6d91c2

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Citations in the corpus

Radial evolution of nonthermal electron populations in the low‐latitude solar wind: Helios, Cluster, and Ulysses Observations (2009, neutral): “Similar evidence for wave-particle interactions resulting from plasma instabilities has also been reported for the solar wind protons [Kasper et al., 2003; Hellinger et al., 2006; Marsch et al., 2006].”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “…in a rather precise 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…”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “…T⊥/T‖) versus the parallel plasma beta parameter (β‖, parallel gas pressure divided by magnetic pressure), the resulting distribution of data points (see Hellinger et al. 2006; Maruca et al. 2012) provides additional constraints on the nature of wave-particle interactions that energize the protons.”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “Still, it has been shown that for some regions in the solar wind, the velocity distributions are kept from deforming too far away from isotropy by plasma instabilities (e.g., Kasper et al. 2002; Hellinger et al. 2006).”
PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, background): “…anisotropy is measuredin situ at r > 0.3 AU for protons in fast-solar-wind streams withβ ≪ 1, despite the fact that (double) adiabatic expansion acts to decreaseT⊥/T‖ (Marsch et al. 1982, 2004; Hellinger et al. 2006), whereβ = 8πp/B2 is the ratio of the plasma pressure to the magnetic pressure.”
Solar Wind Turbulence and the Role of Ion Instabilities (2013, background): “One continuing puzzle here is the following: the instability thresholds, with the rate γ 10−32πfci , calculated by Hellinger et al. (2006) suggest that the ion cyclotron instability should be unstable at values of T⊥/T|| lower than the mirror instability (at low β‖), however there is no clear…”
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.”
Evolution of the solar wind proton temperature anisotropy from 0.3 to 2.5 AU (2007, methodology): “observations are not compatible with the proton-cyclotron threshold based on an electron-proton plasma [Marsch et al., 2004; Hellinger et al., 2006].”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “Cyclotron Instability versus Mirror Instability Hellinger et al. (2006) showed that nearr = 1 AU, the proton temperature anisotropy ratioT⊥p/T‖p is limited from above by the threshold of the mirror instability.”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “The inherently anisotropic nature of magnetized turbulence lends itself to description by an approximation called gyrokinetics [Rutherford and Frieman ,1 968;Taylor and Hastie, 1968; Catto ,1 978; Antonsen and Lane, 1980; Catto et al., 1981; Frieman and Chen, 1982; Dubin et al., 1983; Hahm et al., ”