Chromospheric Alfvénic Waves Strong Enough to Power the Solar Wind

@article{DePontieu2007ChromosphericAW,
  title={Chromospheric Alfvénic Waves Strong Enough to Power the Solar Wind},
  author={Bart De Pontieu and Scott W. McIntosh and Mats Carlsson and Viggo H. Hansteen and Theodore D. Tarbell and Carolus J. Schrijver and Alan M. Title and Richard A. Shine and Saku Tsuneta and Yukio Katsukawa and Kiyoshi Ichimoto and Yoshinori Suematsu and T. Taro Shimizu and S. Nagata},
  journal={Science},
  year={2007},
  volume={318},
  pages={1574 - 1577}
}
Alfvén waves have been invoked as a possible mechanism for the heating of the Sun's outer atmosphere, or corona, to millions of degrees and for the acceleration of the solar wind to hundreds of kilometers per second. However, Alfvén waves of sufficient strength have not been unambiguously observed in the solar atmosphere. We used images of high temporal and spatial resolution obtained with the Solar Optical Telescope onboard the Japanese Hinode satellite to reveal that the chromosphere, the… 

Alfvénic waves with sufficient energy to power the quiet solar corona and fast solar wind

Observations of the transition region of the chromosphere and the corona are reported that reveal how Alfvénic motions permeate the dynamic and finely structured outer solar atmosphere.

Alfvén waves as a solar-interplanetary driver of the thermospheric disturbances

The observed ability of Alfvén waves to excite large-scale gravity waves, together with their proved ubiquity in the solar atmosphere and solar wind, suggests that Alfven waves could be an important solar-interplanetary driver of the global thermospheric disturbances.

Alfvén wave dissipation in the solar chromosphere

Magnetohydrodynamic Alfvén waves1 have been a focus of laboratory plasma physics2 and astrophysics3 for over half a century. Their unique nature makes them ideal energy transporters, and while the

HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE

A three-dimensional magnetohydrodynamic (MHD) model for the propagation and dissipation of Alfvén waves in a coronal loop is developed. The model includes the lower atmospheres at the two ends of the

PROPAGATION OF ALFVÉNIC WAVES FROM CORONA TO CHROMOSPHERE AND CONSEQUENCES FOR SOLAR FLARES

How do magnetohydrodynamic waves travel from the fully ionized corona, into and through the underlying partially ionized chromosphere, and what are the consequences for solar flares? To address these

Multiwavelength Studies of MHD Waves in the Solar Chromosphere

The chromosphere is a thin layer of the solar atmosphere that bridges the relatively cool photosphere and the intensely heated transition region and corona. Compressible and incompressible waves

Coronal Heating by MHD Waves

The heating of the solar chromosphere and corona to the observed high temperatures, imply the presence of ongoing heating that balances the strong radiative and thermal conduction losses expected in

Magnetic tornadoes as energy channels into the solar corona

The imprints of these chromospheric swirls in the transition region and low corona are identified as observational signatures of rapidly rotating magnetic structures, which resemble super-tornadoes under solar conditions and provide an alternative mechanism for channelling energy from the lower into the upper solar atmosphere.

Solar wind and kinetic heliophysics

Abstract. This paper reviews recent aspects of solar wind physics and elucidates the role Alfvén waves play in solar wind acceleration and turbulence, which prevail in the low corona and inner

Spectroscopic Detection of Alfvénic Waves in the Chromosphere of Sunspot Regions

Transverse magnetohydrodynamic waves often called Alfvénic (or kink) waves have been often theoretically put forward to solve the outstanding problems of the solar corona like coronal heating, solar
...

References

SHOWING 1-10 OF 27 REFERENCES

Alfvén Waves in the Solar Corona

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.

Alfvén Waves and Turbulence in the Solar Atmosphere and Solar Wind

We solve the problem of propagation and dissipation of Alfvénic turbulence in a model solar atmosphere consisting of a static photosphere and chromosphere, transition region, and open corona and

Acceleration of the High Speed Solar Wind in Coronal Holes

We outline a theory for the origin and acceleration of the fast solar wind as a consequence of network microflares releasing a spectrum of high frequency Alfvén waves which heat (by cyclotron

Alfvén waves in the solar atmosphere

The nonlinear propagation of Alfvén waves on open solar magnetic flux tubes is considered. The flux tubes are taken to be vertical and axisymmetric, and they are initially untwisted. The Alfvén waves

Alfvén Wave Model of Spicules and Coronal Heating

Magnetohydrodynamic simulations are performed for torsional Alfvén waves propagating along an open magnetic flux tube in the solar atmosphere. It is shown that, if the root mean square of the

Alfvén waves in the solar atmosphere

We examine the propagation of Alfvén waves in the solar atmosphere. The principal theoretical virtues of this work are: (i) The full wave equation is solved without recourse to the small-wavelength

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

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

On cyclotron wave heating and acceleration of solar wind ions in the outer corona

The preferential heating and acceleration of O+5 ions, as observed by Ultraviolet Coronagraph Spectrometer (UVCS) on Solar and Heliospheric Observatory (SOHO) [Kohl et al., 1998] in the solar coronal

Solar winds driven by nonlinear low‐frequency Alfvén waves from the photosphere: Parametric study for fast/slow winds and disappearance of solar winds

[1] We investigate how properties of the corona and solar wind in open coronal holes depend on properties of magnetic fields and their footpoint motions at the surface. We perform one-dimensional

Coronal heating, densities, and temperatures and solar wind acceleration

The outflow of coronal plasma into interplanetary space is a consequence of the coronal heating process. Therefore the formation of the corona and the acceleration of the solar wind should be treated