期刊
ASTRONOMY & ASTROPHYSICS
卷 491, 期 2, 页码 L9-L12出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:200810659
关键词
Sun: corona; Sun: oscillations; Sun: magnetic fields
资金
- Marie Curie Intra European Fellowship
- STFC
- EPSRC [EP/D062837/1] Funding Source: UKRI
- STFC [ST/F00205X/1] Funding Source: UKRI
- Engineering and Physical Sciences Research Council [EP/D062837/1] Funding Source: researchfish
- Science and Technology Facilities Council [ST/F00205X/1] Funding Source: researchfish
The peculiarities of the propagating transverse waves observed in the solar corona with the Coronal Multi-channel Polarimeter ( CoMP) indicate the existence of fine field structuring in the coronal density. We present results of numerical simulations studying the evolution of a localised transverse magneto-hydrodynamic wave in a uniform magnetic field. We consider two initial low plasma-beta equilibria: one with a homogeneous density, and one with a field-aligned dense structure ( such as a loop or a plume). The perpendicular localisation of the wave strongly determines the angular distribution of the energy propagation. If the perpendicular scale of the wave is significantly smaller than the parallel scale ( e. g. wavelength), as established by CoMP, the wave develops as an oblique fast magneto-acoustic wave. In an unstructured medium, the energy of such a wave is transferred mainly across the magnetic field. However, it is possible to channel the energy of the transverse wave along the magnetic field in the presence of a field-aligned density enhancement. We conclude that the CoMP results provide an independent seismological proof that the corona is structured in density in the perpendicular direction.
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