Turbulence transport throughout the heliosphere

By Ben Breech, William H. Matthaeus, J. Minnie, J. Bieber, S. Oughton, Charles W. Smith, P. Isenberg. 2007

168 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d549acf3dea3596f2ef853c885d9d365093e6c70

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. S. Cranmer
2. William H. Matthaeus
3. Ben Breech
4. S. Bale
5. S. Oughton
6. Tamas I. Gombosi
7. Gary Zank
8. G. T'oth

Citations in the corpus

• ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, background): “For example, the transverse correlation length could be obtained from a time evolution equation (Breech et al. 2008) instead of the simple scaling with the magnetic field strength.”
• The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “Slow-fast wind shears, fine-scale structures, and gradients are all candidate mechanisms (Tu and Marsch 1990; Breech et al. 2008).”
• Solar Orbiter (2012, background): “Slow-fast wind shears, fine-scale structures, and gradients are all candidate mechanisms (Tu and Marsch, 1990; Breech et al., 2008).”
• Theory and Transport of Nearly Incompressible Magnetohydrodynamic Turbulence (2017, background): “For example, Matthaeus et al. (1999a, 1999b) used α= 1, Smith et al. (2006), Breech et al. (2008), and Usmanov et al. (2012) used α= 0.8, and Usmanov et al. (2018) used α= 0.128.”
• EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “Geophys., 4, 17 Cho, J., & Vishniac, E. T. 2000, ApJ, 539, 273 Coleman, P. J., Jr. 1968, ApJ, 153, 371 Cranmer, S. R. 2002, Space Sci. Rev., 101, 229 Cranmer, S. R., Field, G. B., & Kohl, J. L. 1999, ApJ, 518, 937 Cranmer, S. R., & van Ballegooijen, A. A. 2003, ApJ, 594, 573 Cranmer, S. R., & van Ba”
• Electron and proton heating by solar wind turbulence (2009, methodology): “Note that this dissipation model is rather robust and has been successfully applied to very different regimes, such as the super Alfvénic solar wind [e.g., Breech et al., 2008] and the corona [e.g., Dmitruk et al., 2001; Verdini and Velli , 2007].”
• The Solar Orbiter mission (2020, background): “Mechanisms for the evolution of solar wind turbulence include slow-fast wind shears, the presence of fine-scale structures, and gradients (Tu & Marsch 1990; Breech et al. 2008; Pucci et al. 2018; Borovsky et al. 2019).”