Study Of The Morphology And Fluctuation Of Solar Spicules

The chromosphere, one of the most important atmosphere of the sun, issandwiched between the photosphere and the transition region and the corona.Its thickness is about1500km. Lots of signifcant structures and eruptions can beseen in chromospheric spectral lines (Hα, CaiiH or K), such as spicules, plages,networks, flaments, mottles, fbrils, RBEs (Rapid Blueshift Events) and so on.Owing to the use of the solar high resolution telescopes (SST and SOT/Hinode)there are great breakthroughs on the research about spicules, mottles and fbrils.In this thesis we focus on the high resolution observations and related theoreticalresearch of spicules. The structure of the thesis is as follows:In chapter one, we introduce the morphology and classifcation of spicules.The counterparts of spicules in other regions and lines are also discussed.In chapter two, we introduce the oscillation and related fuctuation of spicules.Spicules undergo transverse oscillation, i.e., oscillation that appears to be trans-verse to the spicule long axis when they propagate upward. The oscillation periodis about100-500s and the velocity is about10-25km/s. The oscillation may bemotivated by alfv′en or kink wave.In chapter three, we introduce the driving mechanisms of spicules, and wefocus on the shock and magnetic reconnection mechanisms.In chapter four, we study the morphology and fuctuation of spicules ob-served by SOT on-board Hinode. We think we should use extrapolation methodto estimate the lifetime of spicules which is infuenced seriously by background.The oscillation may afect the classifcation of spicules. We fnd oscillation damp-ing decrease with height. By using the NVST (the New Vacuum Solar Telescope)in Yunnan Observatories, the future work contains two sections:(1) how oscil-lation afects classifcation;(2) the relationship between damping decrease andmass density. Finally, it is the study conclusion and adaptation prospect.