Hot and Cool Loops Composing the Corona of the Quiet Sun

We performed a raster scan observation of the quiet Sun with the EUV Imaging Spectrometer (EIS) aboard Hinode and simultaneously analyzed observed emission lines of Fe VIII to XV. From a combined analysis, radiance maps from the observed emission lines were deconvolved into plasma components at five representative temperatures between 0.40MK and 2.63MK. While the lowest temperature component shows network structures on spatial scales of between 10" and 20", the higher temperature components show thread-like patterns on larger scales. A comparison of emission measures at the different temperatures suggests that the lowest temperature component is mainly composed of bodies of small loops, rather than a collection of foot points of the higher temperature loops. The difference in morphologies is interpreted as being due to different magnetic field configurations, loops within super-granule cells and fields extending beyond the boundaries of super-granule cells, with distinct peak temperatures following a loop scaling law.