Global InformationCoronal seismology information
Coronal seismology is a technique of studying the plasma of the Sun's corona with the use of magnetohydrodynamic (MHD) waves and oscillations. Magnetohydrodynamics studies the dynamics of electrically conducting fluids - in this case the fluid is the coronal plasma. Observed properties of the waves (e.g. period, wavelength, amplitude, temporal and spatial signatures (what is the shape of the wave perturbation?), characteristic scenarios of the wave evolution (is the wave damped?), combined with a theoretical modelling of the wave phenomena (dispersion relations, evolutionary equations, etc.), may reflect physical parameters of the corona which are not accessible in situ, such as the coronal magnetic field strength and Alfvén velocity [1] and coronal dissipative coefficients.[2] Originally, the method of MHD coronal seismology was suggested by Y. Uchida in 1970[3] for propagating waves, and B. Roberts et al. in 1984[4] for standing waves, but was not practically applied until the late 90s due to a lack of necessary observational resolution. Philosophically, coronal seismology is similar to the Earth's seismology, helioseismology, and MHD spectroscopy of laboratory plasma devices. In all these approaches, waves of various kind are used to probe a medium.
The theoretical foundation of coronal seismology is the dispersion relation of MHD modes of a plasma cylinder: a plasma structure which is nonuniform in the transverse direction and extended along the magnetic field. This model works well for the description of a number of plasma structures observed in the solar corona: e.g. coronal loops, prominence fibrils, plumes, various filaments. Such a structure acts as a waveguide of MHD waves.
This discussion is adapted from Nakariakov & Verwichte (2009).[5]
- ^ Nakariakov, V. M.; Ofman, L. (2001). "Determination of the coronal magnetic field by coronal loop oscillations" (PDF). Astronomy and Astrophysics. 372 (3): L53–L56. Bibcode:2001A&A...372L..53N. doi:10.1051/0004-6361:20010607.
- ^ Nakariakov, V. M.; Ofman, L.; Deluca, E. E.; Roberts, B.; Davila, J. M. (1999). "TRACE observation of damped coronal loop oscillations: Implications for coronal heating". Science. 285 (5429): 862–864. Bibcode:1999Sci...285..862N. doi:10.1126/science.285.5429.862. PMID 10436148.
- ^ Uchida, Y. (1970). "Diagnosis of coronal magnetic structure by flare-associated hydromagnetic disturbances". Publications of the Astronomical Society of Japan. 22: 341–364. Bibcode:1970PASJ...22..341U.
- ^ Roberts, B.; Edwin, P. M.; Benz, A. O. (1984). "On coronal oscillations". The Astrophysical Journal. 279: 857–865. Bibcode:1984ApJ...279..857R. doi:10.1086/161956.
- ^ Nakariakov, V. M.; Verwichte, E. (2005). "Coronal Waves and Oscillations". Living Reviews in Solar Physics. 2 (1): 3. Bibcode:2005LRSP....2....3N. doi:10.12942/lrsp-2005-3.