The Relationship Between The Half-shadow Wave And The Shadow Oscillation And A Fast EUV Wave With CME Burst

Observation of the main sunspot of AR11692 were carried out with the 1m New Vacuum Solar Telescope(NVST) located on the Fuxian Solar Observatory(FSO) with the Ha on 2013 march 13. The high cadence(up to 12s) Hα intensity images permit us to elaborate the relationship between the 5-min oscillation and 3-min oscillation. It is found that there are running waves that periodically appear at the wave sources, and propagate outward while forming partial arcs. Due to their expansion, the running waves become more diffused, and eventually disappear at the edge of penumbra. But there are obvious difference when we measured the period of running waves in different region of sunspot. The period is 156 s when the running waves is in umbral region, which is a typical 3-min oscillation, the period is 312 s when the running waves propagate in the penumbral district, which is a typical 5-min oscillation. On the base of timeslice image, we conclude that the waves are form in the umbral region with the 5-min oscillation period, which can cause the brightness periodicity change in the umbra region with the period 3-min(in fact is the half of 5-min oscillation) and 5-min in the penumbra.Taking advantage of the high temporal and spatial resolution of the Solar Dynamics Observatory(SDO) observations, we present a solar corona Extreme UltraViolet(EUV) wave associated with a Coronal Mass Ejection(CME) on 2014 January 7. We aim at understanding the driving mechanism of this EUV wave, by comparing the onset time and the initial location of the CME and the EUV wave, we propose that the EUV wave should be driven by the associated CME. Through analysing the time-slice plots, we found that the wave had a speed of about 1200 km s-1. Our observations can be interpreted by the hybrid model proposed by Chen et al. 2002, and the observed fast EUV wave corresponds to the fast component in Chen’s model, i.e., the Coronal Moreton wave.