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We analyze several data sets obtained by Hinode/EIS and find various types offlows during CMEs and EUV jet eruptions. CME-induced dimming regions are foundto be characterized by significant blueshift and enhanced line width by using asingle Gaussian fit. While a red-blue (RB) asymmetry analysis and a RB-guideddouble Gaussian fit of the coronal line profiles indicate that these are likelycaused by the superposition of a strong background emission component and arelatively weak (~10%) high-speed (~100 km s-1) upflow component. This findingsuggests that the outflow velocity in the dimming region is probably of theorder of 100 km s-1, not ~20 km s-1 as reported previously. Density andtemperature diagnostics suggest that dimming is primarily an effect of densitydecrease rather than temperature change. The mass losses in dimming regions asestimated from different methods are roughly consistent with each other andthey are 20%-60% of the masses of the associated CMEs. With the guide of RBasymmetry analysis, we also find several temperature-dependent outflows (speedincreases with temperature) immediately outside the (deepest) dimming region.In an erupted CME loop and an EUV jet, profiles of emission lines formed atcoronal and transition region temperatures are found to exhibit twowell-separated components, an almost stationary component accounting for thebackground emission and a highly blueshifted (~200 km s-1) componentrepresenting emission from the erupting material. The two components can easilybe decomposed through a double Gaussian fit and we can diagnose the electrondensity, temperature and mass of the ejecta. Combining the speed of theblueshifted component and the projected speed of the erupting material derivedfrom simultaneous imaging observations, we can calculate the real speed of theejecta.

What can we learn about solar coronal mass ejections, coronal dimmings, and Extreme-Ultraviolet jets through spectroscopic observations?