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Cranmer SR, Asgari-Targhi M, Miralles MP, et al. The role of turbulence in coronal heating and solar wind expansion. Philos Trans A Math Phys Eng Sci. 2015;373(2041)doi: 10.1098/rsta.2014.0148.
Cranmer, S. R., Asgari-Targhi, M., Miralles, M. P., Raymond, J. C., Strachan, L., Tian, H., & Woolsey, L. N. (2015). The role of turbulence in coronal heating and solar wind expansion. Philosophical transactions. Series A, Mathematical, physical, and engineering sciences, 373(2041), . https://doi.org/10.1098/rsta.2014.0148
Cranmer, Steven R, et al. "The role of turbulence in coronal heating and solar wind expansion." Philosophical transactions. Series A, Mathematical, physical, and engineering sciences vol. 373,2041 (2015). doi: https://doi.org/10.1098/rsta.2014.0148
Cranmer SR, Asgari-Targhi M, Miralles MP, Raymond JC, Strachan L, Tian H, Woolsey LN. The role of turbulence in coronal heating and solar wind expansion. Philos Trans A Math Phys Eng Sci. 2015 May 13;373(2041). doi: 10.1098/rsta.2014.0148. PMID: 25848083; PMCID: PMC4394680.
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Philos Trans A Math Phys Eng Sci. 2015 May 13;373(2041). doi: 10.1098/rsta.2014.0148.

The role of turbulence in coronal heating and solar wind expansion.

Philosophical transactions. Series A, Mathematical, physical, and engineering sciences

Steven R Cranmer, Mahboubeh Asgari-Targhi, Mari Paz Miralles, John C Raymond, Leonard Strachan, Hui Tian, Lauren N Woolsey

Affiliations

  1. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA Laboratory for Atmospheric and Space Physics, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 8030, USA [email protected].
  2. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA.

PMID: 25848083 PMCID: PMC4394680 DOI: 10.1098/rsta.2014.0148

Abstract

Plasma in the Sun's hot corona expands into the heliosphere as a supersonic and highly magnetized solar wind. This paper provides an overview of our current understanding of how the corona is heated and how the solar wind is accelerated. Recent models of magnetohydrodynamic turbulence have progressed to the point of successfully predicting many observed properties of this complex, multi-scale system. However, it is not clear whether the heating in open-field regions comes mainly from the dissipation of turbulent fluctuations that are launched from the solar surface, or whether the chaotic 'magnetic carpet' in the low corona energizes the system via magnetic reconnection. To help pin down the physics, we also review some key observational results from ultraviolet spectroscopy of the collisionless outer corona.

© 2015 The Author(s) Published by the Royal Society. All rights reserved.

Keywords: heliosphere; plasma physics; solar atmosphere; solar corona; solar wind; turbulence

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