Alfvén Waves in the Lower Solar Atmosphere

  title={Alfvén Waves in the Lower Solar Atmosphere},
  author={David B. Jess and Mihalis Mathioudakis and R{\'o}bert Erd{\'e}lyi and P. J. Crockett and Francis P. Keenan and Damian J. Christian},
  pages={1582 - 1585}
The flow of energy through the solar atmosphere and the heating of the Sun's outer regions are still not understood. Here, we report the detection of oscillatory phenomena associated with a large bright-point group that is 430,000 square kilometers in area and located near the solar disk center. Wavelet analysis reveals full-width half-maximum oscillations with periodicities ranging from 126 to 700 seconds originating above the bright point and significance levels exceeding 99%. These… 


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High-frequency torsional Alfvén waves as an energy source for coronal heating

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Torsional oscillations within a magnetic pore in the solar photosphere

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An estimate of the energy carried by the waves that are spatially resolved indicates that they are too weak to heat the solar corona; however, unresolved Alfvén waves may carry sufficient energy.

Chromospheric Alfvénic Waves Strong Enough to Power the Solar Wind

Estimates of the energy flux carried by these waves and comparisons with advanced radiative magnetohydrodynamic simulations indicate that such Alfvén waves are energetic enough to accelerate the solar wind and possibly to heat the quiet corona.

High-frequency acoustic waves are not sufficient to heat the solar chromosphere

The detection of high-frequency waves is reported, and numerical simulations are used to show that the acoustic energy flux of these waves is too low, by a factor of at least ten, to balance the radiative losses in the solar chromosphere.

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Wave and oscillatory activity of the solar corona is confidently observed with modern imaging and spectral instruments in the visible light, EUV, X-ray and radio bands, and interpreted in terms of

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