Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004pasj...56..207m&link_type=abstract
Publications of the Astronomical Society of Japan, Vol.56, No.1, pp. 207-214
Astronomy and Astrophysics
Astronomy
16
Sun: Corona, Sun: Flares, Sun: Magnetic Fields, Sun: Oscillations
Scientific paper
We performed three-dimensional MHD numerical simulations for solar coronal magnetic loop oscillations and found: (1) The loop oscillation period is determined by its Alfvén time. (2) The amplitude of oscillation decreases exponentially in time. This is explained as energy transport by fast-mode MHD waves. The damping rate, ωdamp, is described as ωdamp ∝ Va/R, where Va is the Alfvén speed around loops and R is the radius of the loop. Because of computer resources limitations, the plasma β value is much larger than that of the real corona. We thus applied a scaling law derived from numerical simulation results to the real corona parameter ranges and analyzed the results.
Miyagoshi Takehiro
Shimojo Masumi
Yokoyama Takaaki
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