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The Sun is the only star that we can spatially resolve and it can be regardedas a fundamental plasma laboratory of astrophysics. The solar transition region(TR), the layer between the solar chromosphere and corona, plays an importantrole in solar wind origin and coronal heating. Recent high-resolutionobservations made by SOHO, TRACE, and Hinode indicate that the TR is highlynonuniform and magnetically structured. Through a combination of spectroscopicobservations and magnetic field extrapolations, the TR magnetic structures andplasma properties have been found to be different in coronal holes and in thequiet Sun. In active regions, the TR density and temperature structures alsodiffer in sunspots and the surrounding plage regions. Although the TR isbelieved to be a dynamic layer, quasi-steady flows lasting from several hoursto several days are often present in the quiet Sun, coronal holes, and activeregions, indicating some kind of plasma circulation/convection in the TR andcorona. The emission of hydrogen Lyman lines, which originates from the lowerTR, has also been intensively investigated in the recent past. Observationsshow clearly that the flows and dynamics in the middle and upper TR can greatlymodify the Lyman line profiles.

New views on the emission and structure of the solar transition region