Solar prominences are thread-like (more exactly ribbon-shaped) partially ionized plasma clouds hanging in the solar corona. They are of one hundredth of coronal temperature and 100 times as dense as the corona. Prominences seen on the limb of the sun are really prominent against the dark sky. Seen on the solar disk, however, they are just ugly, dark threads, hence another name “filaments.” Prominences are believed to be supported against gravity and insulated from the hot coronal plasma by magnetic fields. Quite a few prominence magnetic field models have been proposed, but it is still not clear which of them is most plausible. Every time a new observational feature of prominences is discovered, we are loaded with a new puzzle rather than a clue. Among the mysterious characters of prominences are chirality, barb bearing and the roll effect. This talk will introduce general audience to interesting observational features of prominences and review theoretical (speculative) explanation for them. The speaker’s (fragmentary) studies of solar prominences in the past two decades will also be interspersed throughout the presentation.