Heating of the low‐latitude solar wind by dissipation of turbulent magnetic fluctuations

By Charles W. Smith, William H. Matthaeus, Gary Zank, N. Ness, S. Oughton, J. Richardson. 2001

230 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/b4418b87d6aa42852a053248209139dcd75f406b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Molecular Biology

Citations in the corpus

Evaluation of the turbulent energy cascade rates from the upper inertial range in the solar wind at 1 AU (2007, background): “Cascade rates estimated from the energy-containing scale of turbulence at 1 AU by evaluating the triple-products of fluctuation magnetic fields and velocities and the correlation length scale of the turbulence also give values in this range [e.g., Smith et al., 2001a, 2006c; Isenberg, 2005].”
Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations (2009, background): “Other potential sources include turbulent heating [Smith et al., 2001], heating from kinetic Alfvén waves [Leamon et al., 1999] or, perhaps, through magnetic reconnection [Leamon et al., 2000], although this last scenario appears somewhat doubtful, at least in the fast wind [Gosling, 2007].”
The solar magnetic field (2006, background): “Other authors consider in their models the solar wind velocity shear and beyond ∼10 AU energetic pickup ions (see below) as an additional source for the Alfvénic turbulence [646,647].”
PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, result): “In addition, the expected rate at which the measured fluctuations dissipate (based on phenomenological turbulence theories) is comparable to the observationally inferred solar-wind heating rate (Smith et al. 2001; Breech et al. 2009; Cranmer et al. 2009).”
Turbulence transport throughout the heliosphere (2007, methodology): “[66] The rate at which this energy is added is proportional to the creation rate of new pickup protons, N/tion, where N is the local interstellar hydrogen density and tion is the neutral ionization time at 1 AU, taken to be 106 s[ Smith 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, background): “For antiparallel reconnection, vA* = vA, otherwise vA* vAsin(q/2) [Sonnerup, 1974] where q is the angle between the two axes of the two flux tubes and vA is the Alfven speed in the flux tubes.”
Turbulent Heating of the Solar Wind by Newborn Interstellar Pickup Protons (2006, methodology): “Both methods give similar results (Matthaeus et al. 1999a; Smith et al. 2001) when averaged over sufficient quantities of data; however, k1 AU has not been shown to be computed reliably from short periods of data.”
The Turbulent Cascade at 1 AU: Energy Transfer and the Third-Order Scaling for MHD (2007, background): “Smith et al. (2001, 2006) demonstrate that this model, together with the Isenberg et al. (2003) analysis of the pickup process, can account for thermal proton energies up to 75 AU, where their 1 B. T. MacBride is now a graduate student within the physics program at UC Berkeley.”
Electron and proton heating by solar wind turbulence (2009, methodology): “Previous theories [Zhou and Matthaeus, 1990; Marsch and Tu, 1993; Oughton and Matthaeus, 1995; Zank et al., 1996; Matthaeus et al., 1999; Smith et al., 2001, 2006; Matthaeus et al., 2004; Breech et al., 2005; Isenberg et al., 2003; Breech et al., 2008], have been able to account for radial…”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “Moreover, the amplitudes of these turbulent fluctuations are sufficient to explain the heating rates thathave been inferred from the proton and electron temperature profiles (Smith et al. 2001; MacBride et al. 2008; Cranmer et al. 2009; Stawarz et al. 2009).”
Alfvén Waves and Turbulence in the Solar Atmosphere and Solar Wind (2007, background): “Other models of turbulent transport have been constructed to fit the decay of turbulence with distance from the Sun in the solar wind beyond 1 AU (Smith et al. 2001; Breech et al. 2005), as well as to explain the extended heating in this region.”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, methodology): “The radial scalingλ⊥ ∝ r1/2 has been measured in the heliosphere by, e.g., Bruno & Dobrowolny (1986) and Smith et al. (2001).”