Coronal Heating by Magnetohydrodynamic Turbulence Driven by Reflected Low-Frequency Waves | Zendy

W. H. Matthaeus | Zendy; G. P. Zank | Zendy; S. Oughton | Zendy; D. J. Mullan | Zendy; P. Dmitruk | Zendy

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Coronal Heating by Magnetohydrodynamic Turbulence Driven by Reflected Low-Frequency Waves

Author(s) -

W. H. Matthaeus,

G. P. Zank,

S. Oughton,

D. J. Mullan,

P. Dmitruk

Publication year - 1999

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/312259

Subject(s) - physics , magnetohydrodynamics , magnetohydrodynamic turbulence , photosphere , magnetohydrodynamic drive , turbulence , chromosphere , coronal radiative losses , corona (planetary geology) , nanoflares , astrophysics , cascade , coronal loop , alfvén wave , computational physics , wavelength , field line , magnetic field , transverse plane , solar wind , mechanics , astronomy , coronal mass ejection , optics , spectral line , chemistry , structural engineering , engineering , chromatography , quantum mechanics , astrobiology , venus

A candidate mechanism for the heating of the solar corona in open field line regions is described. The interaction of Alfvén waves, generated in the photosphere or chromosphere, with their reflections and the subsequent driving of quasi-two-dimensional MHD turbulence is considered. A nonlinear cascade drives fluctuations toward short wavelengths which are transverse to the mean field, thereby heating at rates insensitive to restrictive Alfvén timescales. A phenomenology is presented, providing estimates of achievable heating efficiency that are most favorable

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