DEMONSTRATIONS THAT THE SOLAR WIND IS NOT ACCELERATED BY WAVES OR TURBULENCE

Journal Article · Wed Mar 10 00:00:00 EST 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/711/2/1044· OSTI ID:21394309

Roberts, D Aaron ^[1]

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1. NASA Goddard Space Flight Center, Heliophysics Science Division, Greenbelt, MD 20771 (United States)

The present work uses observations and theoretical considerations to provide both qualitative and quantitative arguments that hydromagnetic waves, whether turbulent or not, cannot produce the acceleration of the fast solar wind and the related heating of the open solar corona. Waves do exist, and can play a role in the differential heating and acceleration of minor ions, but their amplitudes are not sufficient to power the wind, as demonstrated by extrapolation of magnetic spectra from Helios and Ulysses observations. Dissipation mechanisms invoked to circumvent this conclusion cannot be effective for a variety of reasons. In particular, turbulence does not play a strong role in the corona as shown both by observations of coronal striations and other features, and by theoretical considerations of line tying to a nonturbulent photosphere, nonlocality of interactions, and the nature of the kinetic dissipation. We consider possible 'ways out' of the arguments presented, and suggest that in the absence of wave or turbulent heating and acceleration, the chromosphere and transition region become the natural source, if yet unproven, of open coronal energization through the production of nonthermal particle distributions.

• OSTI ID: 21394309
• Journal Information: Astrophysical Journal, Vol. 711, Issue 2; Other Information: DOI: 10.1088/0004-637X/711/2/1044; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ACCELERATION
CHROMOSPHERE
EXTRAPOLATION
HYDROMAGNETIC WAVES
IONS
MAGNETIC FIELDS
PHOTOSPHERE
SOLAR CORONA
SOLAR WIND
SPECTRA
STRIATIONS
SUN
TURBULENCE
TURBULENT HEATING
ATMOSPHERES
CHARGED PARTICLES
HEATING
MAIN SEQUENCE STARS
MATHEMATICAL SOLUTIONS
NUMERICAL SOLUTION
PLASMA HEATING
SOLAR ACTIVITY
SOLAR ATMOSPHERE
STARS
STELLAR ACTIVITY
STELLAR ATMOSPHERES
STELLAR CORONAE
STELLAR WINDS