We investigate the evolutions of two prominences （P1, P2） and two bundles of coronal loops （L1, L2）, observed with SDO/AIA near the east solar limb on 2012 September 22. It is found that there were large-amplitude...We investigate the evolutions of two prominences （P1, P2） and two bundles of coronal loops （L1, L2）, observed with SDO/AIA near the east solar limb on 2012 September 22. It is found that there were large-amplitude oscillations in P1 and L1 but no detectable motions in P2 and L2. These transverse oscillations were triggered by a large-scale coronal wave, originating from a large flare in a remote active region behind the solar limb. By carefully comparing the locations and heights of these oscillating and non-oscillating structures, we conclude that the propagating height of the wave is between 50 Mm and 130 Mm. The wave energy deposited in the oscillating prominence and coronal loops is at least of the order of 10-8 erg. Furthermore, local magnetic field strength and Alfv6n speeds are derived from the oscillating periods and damping time scales, which are extracted from the time series of the oscillations. It is demon- strated that oscillations can be used in not only coronal seismology, but also to reveal the properties of the wave.展开更多
基金supported by the National Natural Science Foundation of China (Grant Nos. 41131065, 41574165, 41421063 and 41304134)MOEC (20113402110001)+2 种基金CAS Key Research Program (KZZD-EW-01-4)the fundamental research funds for the central universities (WK2080000077)the foundation for Young Talents in College of Anhui Province (2013SQRL044ZD)
文摘We investigate the evolutions of two prominences （P1, P2） and two bundles of coronal loops （L1, L2）, observed with SDO/AIA near the east solar limb on 2012 September 22. It is found that there were large-amplitude oscillations in P1 and L1 but no detectable motions in P2 and L2. These transverse oscillations were triggered by a large-scale coronal wave, originating from a large flare in a remote active region behind the solar limb. By carefully comparing the locations and heights of these oscillating and non-oscillating structures, we conclude that the propagating height of the wave is between 50 Mm and 130 Mm. The wave energy deposited in the oscillating prominence and coronal loops is at least of the order of 10-8 erg. Furthermore, local magnetic field strength and Alfv6n speeds are derived from the oscillating periods and damping time scales, which are extracted from the time series of the oscillations. It is demon- strated that oscillations can be used in not only coronal seismology, but also to reveal the properties of the wave.
