The Evershed Effect with SOT/Hinode
arXiv:0903.2605 · doi:10.1007/978-3-642-02859-5_14
Abstract
The Solar Optical Telescope onboard Hinode revealed the fine-scale structure of the Evershed flow and its relation to the filamentary structures of the sunspot penumbra. The Evershed flow is confined in narrow channels with nearly horizontal magnetic fields, embedded in a deep layer of the penumbral atmosphere. It is a dynamic phenomenon with flow velocity close to the photospheric sound speed. Individual flow channels are associated with tiny upflows of hot gas (sources) at the inner end and downflows (sinks) at the outer end. SOT/Hinode also discovered ``twisting'' motions of penumbral filaments, which may be attributed to the convective nature of the Evershed flow. The Evershed effect may be understood as a natural consequence of thermal convection under a strong, inclined magnetic field. Current penumbral models are discussed in the lights of these new Hinode observations.
To appear in "Magnetic Coupling between the Interior and the Atmosphere of the Sun", eds. S.S. Hasan and R.J. Rutten, Astrophysics and Space Science Proceedings, Springer-Verlag, Heidelberg, Berlin, 2009
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Cited by in corpus (6)
- Returning magnetic flux in sunspot penumbrae
- Deep probing of the photospheric sunspot penumbra: no evidence for magnetic field-free gaps
- Evidence for convection in Sunspot penumbrae
- Multi-wavelength Study of Transition Region Penumbral Subarcsecond Bright Dots Using IRIS and NST
- Rapid Enhancement of Sheared Evershed Flow Along the Neutral Line Associated with an X6.5 Flare Observed by Hinode
- The Evershed Effect with SOT/Hinode