Propagating slow magnetoacoustic waves in coronal loops observed by Hinode/EIS

Details Propagating slow magnetoacoustic waves in coronal loops observed by Hinode/EIS Propagating slow magnetoacoustic waves in coronal loops observed by Hinode/EIS

2009-02-25

arxiv.org/abs/0902.4480v1

Astrophys.J.696:1448-1460,2009

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

13 pages, 11 color figures, 4 tables, Astrophys.J, May 2009 - v696 issue, (in press)

Scientific paper

10.1088/0004-637X/696/2/1448

We present the first Hinode/EIS observations of 5 min quasi-periodic oscillations detected in a transition-region line (He II) and five coronal lines (Fe X, Fe XII, Fe XIII, Fe XIV, and Fe XV) at the footpoint of a coronal loop. The oscillations exist throughout the whole observation, characterized by a series of wave packets with nearly constant period, typically persisting for 4-6 cycles with a lifetime of 20-30 min. There is an approximate in-phase relation between Doppler shift and intensity oscillations. This provides evidence for slow magnetoacoustic waves propagating upwards from the transition region into the corona. We find that the oscillations detected in the five coronal lines are highly correlated, and the amplitude decreases with increasing temperature. The amplitude of Doppler shift oscillations decrease by a factor of about 3, while that of relative intensity decreases by a factor of about 4 from Fe X to Fe XV. These oscillations may be caused by the leakage of the photospheric p-modes through the chromosphere and transition region into the corona, which has been suggested as the source for intensity oscillations previously observed by TRACE. The temperature dependence of the oscillation amplitudes can be explained by damping of the waves traveling along the loop with multithread structure near the footpoint. Thus, this property may have potential value for coronal seismology in diagnostic of temperature structure in a coronal loop.

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