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Prominence eruption is closely related to coronal mass ejections and is animportant topic in solar physics. Spectroscopic observation is an effective wayto explore the plasma properties, but the spectral observations of eruptiveprominences are rare. In this paper we will introduce an eruptive polar crownprominence with spectral observations from the Interface Region ImagingSpectrograph (IRIS), and try to explain some phenomena that are rarely reportedin previous works. The eruptive prominence experiences a slow-rise andfast-rise phase, while the line-of-sight motions of the prominence plasma couldbe divided into three periods: two hours before the fast-rise phase, oppositeDoppler shifts are found at the two sides of the prominence axis;then, redshifts dominate the prominence gradually; in the fast-rise phase, theprominence gets to be blue-shifted. During the second period, a faint componentappears in Mg II k window with a narrow line width and a large red shift. Afaint region is also found in AIA 304-angstrom images along the prominencespine, and the faint region gets darker during the expansion of the spine. Wepropose that the opposite Doppler shifts in the first period are a feature ofthe polar crown prominence that we studied. The red shifts in the second periodare possibly due to mass drainage during the elevation of the prominence spine,which could accelerate the eruption in return. The blue shifts in the thirdperiod are due to that the prominence erupts toward the observer. We suggestthat the faint component appears due to the decreasing of the plasma density,and the latter results from the expansion of the prominence spine.

Spectral evolution of an eruptive polar crown prominence with IRIS observations