Journal
PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES
Volume 373, Issue 2041, Pages -Publisher
ROYAL SOC
DOI: 10.1098/rsta.2014.0148
Keywords
heliosphere; plasma physics; solar atmosphere; solar corona; solar wind; turbulence
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Funding
- NASA [NNX-10-AC11G, NNX-14-AG99G, NX-06-AG95G, NNX-09-AH22G, NNX-10-AQ58G]
- NSF SHINE program [AGS-1259519]
- Div Atmospheric & Geospace Sciences
- Directorate For Geosciences [1540094] Funding Source: National Science Foundation
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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 fromultraviolet spectroscopy of the collisionless outer corona.
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