The Role of Turbulence in Coronal Heating and Solar Wind Expansion
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 prog...
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Main Authors | , , , , , , |
Format | Paper Journal Article |
Language | English |
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07.12.2014
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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. |
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AbstractList | 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. 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. |
Author | Tian, H Strachan, L Woolsey, L N Cranmer, S R Asgari-Targhi, M Miralles, M P Raymond, J C |
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BackLink | https://doi.org/10.1098/rsta.2014.0148$$DView published paper (Access to full text may be restricted) https://doi.org/10.48550/arXiv.1412.2307$$DView paper in arXiv |
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Snippet | 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... 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... |
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SubjectTerms | Activation Computational fluid dynamics Coronas Fluid flow Heating Heliosphere Magnetohydrodynamic turbulence Magnetohydrodynamics Physics - Solar and Stellar Astrophysics Plasmas (physics) Solar surface Solar wind Variation |
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Title | The Role of Turbulence in Coronal Heating and Solar Wind Expansion |
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