Standing fast magnetoacoustic kink waves of solar coronal loops with field-aligned flow

Details Standing fast magnetoacoustic kink waves of solar coronal loops with field-aligned flow Standing fast magnetoacoustic kink waves of solar coronal loops with field-aligned flow

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008a%26a...488..757g&link_type=abstract

Astronomy and Astrophysics, Volume 488, Issue 2, 2008, pp.757-761

Astronomy and Astrophysics

Astrophysics

6

Magnetohydrodynamics (Mhd), Sun: Corona, Sun: Oscillations

Scientific paper

Aims: We refer to the recent observational data of Hinode, which detected weakly-attenuated coronal loop oscillations in the presence of background flow (Ofman & Wang 2008, A&A, 482, L9). Vertical loop oscillations that lasted for three wave periods were reported with a wave period P = 113 ± 2 s, attenuation time τ = 560 ± 260 s, and wave amplitude A{max} = 0.67 ± 0.12 Mm. Ofman & Wang (2008) estimated the flow speed within the range of 74-123 km s-1. We consider impulsively generated standing fast magnetoacoustic kink waves of a straight solar coronal slab with field-aligned internal flow. We aim to determine the influence of such flow on the spatial and temporal signatures of these waves. Methods: The time-dependent, ideal magnetohydrodynamic equations are solved numerically. Results: The numerical results show that as a result of wave scattering on inhomogeneous flow kink waves experience stronger attenuation than for a still plasma, while P remains weakly altered by this flow. Numerically evaluated values of A{max} and P are close to the observational data. A value of τ is about two times smaller than observed.

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