Joint IRIS and SDO/AIA Observations of Coronal EUV Waves

Coronal EUV waves on various spatio-temporal scales have recently been observed in unprecedented detail by SDO/AIA and are being used as seismological tools to infer the physical conditions in the corona. The newly launched Interface Region Imaging Spectrograph (IRIS) can extend our observational domain from the corona to the previously under-explored transition region and chromosphere. It can shed critical light on the nature of such waves, on their influence on the lower solar atmosphere, and on their role in transporting energy through different atmospheric layers. We present here early results of joint IRIS and SDO/AIA observations of two types of coronal EUV waves. For global EUV waves or the so-called EIT waves, we use the measured Doppler velocity to infer the potential compression to the deep atmosphere due to the wave passage. For quasi-periodic, fast-mode magnetosonic wave trains (e.g., Liu et al. 2011, ApJL), we focus on their flaring source region in an effort to identify their long-sought physical driver. In particular, we will test the hypothesis that the commonly detected 1-3 minute periodicity of such waves may have a chromospheric origin such as p-mode leakage. SDO/AIA images of quasi-periodic fast-mode magnetosonic wave trains observed on 2010/08/01 (from Liu et al. 2011, ApJL).