Spectral Exponents of Kinetic and Magnetic Energy Spectra in Solar Wind Turbulence

By J. Podesta, D. Roberts, M. Goldstein. 2007

203 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/11986685b6afc3e3ec6cf584e134b4774176eaca

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

1. C. Chen
2. E. Quataert
3. S. Bale
4. T. Horbury
5. A. Schekochihin
6. Tamas I. Gombosi
7. O. Alexandrova
8. G. T'oth

In Molecular Biology

1. C. Chen
2. B. T. MacBride
3. G. T'oth
4. Tamas I. Gombosi
5. B. Chandran
6. A. Mallet
7. Charles W. Smith
8. Igor M. Sokolov

Citations in the corpus

• The Turbulent Cascade at 1 AU: Energy Transfer and the Third-Order Scaling for MHD (2007, background): “See Podesta et al. (2007a) for a more complete discussion.”
• Solar Wind Turbulence and the Role of Ion Instabilities (2013, background): “Velocity fluctuations in the solar wind appear to have a spectrum significantly shallower than the magnetic field, with a spectral index near −3/2 (Grappin et al. 1991; Salem 2000; Mangeney et al. 2001; Podesta et al. 2007; Salem et al. 2009; Chen et al. 2011b, 2013b; Boldyrev et al. 2011; Borovsky ”
• DEPENDENCE OF SOLAR-WIND POWER SPECTRA ON THE DIRECTION OF THE LOCAL MEAN MAGNETIC FIELD (2009, background): “…analysis shows that solar-wind velocity fluctuations have typical spectral exponents around 3/2, magnetic field fluctuations have typical spectral exponents around 5/3, and the spectral exponents for the total energy (kinetic plus magnetic) lie somewhere between these two (Podesta et al. 2007).”
• INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “…AW correlation length (outer scale)L⊥, the rms amplitude of the AW velocity fluctuations at perpendicular scaleλ is ∝ λ1/4 as in observations atr = 1 AU (Podesta et al. 2007; Chen et al. 2011), direct numerical simulations of AW turbulence in the presence of a strong background magnetic field…”
• PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, background): “The valuec3 = 3/2 is motivated by a different set of theoretical and numerical studies (Boldyrev 2006; Mason et al. 2006; Perez and Boldyrev 2009), as well as recent in situ observations of the velocity power spectrum in the solar wind (Podesta et al. 2007; Podesta and Bhattacharjee 2009).”
• Anisotropy of Alfvénic turbulence in the solar wind and numerical simulations (2010, background): “…occurs only in the decaying period of our RMHD simulation, while solar wind observations show rA < 1 (e.g. Matthaeus & Goldstein 1982; Marsch & Tu 1990; Bruno et al. 2007; Podesta et al. 2007; Salem et al. 2009), suggests that solar wind turbulence may be better described by a forced model.”
• ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, result): “The above scaling is compatible with the 1 AU observations of Podesta et al. (2007).”