Wind/SWE observations of firehose constraint on solar wind proton temperature anisotropy

By Justin C. Kasper, A. Lazarus, S. Gary. 2002

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View Paper: https://www.semanticscholar.org/paper/bc7b56522bde62d3ef7407094099c94d691d3094

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In Astronomy and Astrophysics

Citations in the corpus

INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “Spacecraft measurements show that the values ofR found in the solar wind are bounded from below by the instability threshold of the oblique firehose mode and from above by the instability threshold of the mirror mode (Kasper et al. 2002; Hellinger et al. 2006; Bale et al. 2009).”
The Solar Probe Cup on the Parker Solar Probe (2019, background): “…is considerably more difficult than with instruments such as Wind/SWE (Ogilvie et al. 1995), where the spinning spacecraft provides the ability to regularly make measurements of the velocity distribution function at different angles with respect to the magnetic field (Kasper et al. 2002).”
Electron Heating in Hot Accretion Flows (2007, background): “This does not appear to be true in the solar wind, where large pressure anisotropies are measured (e.g., Cranmer et al. 1999) andwhere there is in situ experimental evidence for pressure isotropization via the firehose instability (Kasper et al. 2002).”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “…parameter plane (T0⊥/T0‖,βi) circumscribed 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…”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, methodology): “…or velocityspace instabilities that transfer energy from the parallel to the perpendicular direction [Scarf et al., 1967; Eviatar and Schulz , 1970; Kasper et al., 2002; Marsch, 2006]—we may employ our model to determine under what conditions the gyrokinetic cascade reaches the ion cyclotron…”
Shearing Box Simulations of the MRI in a Collisionless Plasma (2005, unknown): “It is also interesting to note that satellites have observed that the pressure anisotropy in the solar wind near1 AU is approximately marginally stable to the firehose instability (Kasper et al. 2002), consistent with our assumption that microinstabilities dominate the isotropization of the plasma.”
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, background): “[2] Direct observations of the solar wind plasma have suggested that at 1 AU the proton velocity distribution functions are constrained by the wave-particle interaction deriving from plasma instabilities [it Kasper et al., 2002; Hellinger et al., 2006].”
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).”