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Filament longitudinal oscillations have been observed on the solar disk inH$\alpha$. We intend to find an example of the longitudinal oscillations of aprominence, where the magnetic dip can be seen directly, and examine what isthe restoring force of such kind of oscillations. We carry out amultiwavelength data analysis of the active region prominence oscillationsabove the western limb on 2007 February 8. Besides, we perform aone-dimensional hydrodynamic simulation of the longitudinal oscillations. Thehigh-resolution observations by Hinode/SOT indicate that the prominence, seenas a concave-inward shape in lower-resolution Extreme Ultraviolet (EUV) images,actually consists of many concave-outward threads, which is indicative of theexistence of magnetic dips. After being injected into the dip region, a bulk ofprominence material started to oscillate for more than 3.5 hours, with theperiod being 52 min. The oscillation decayed with time, with the decaytimescale being 133 min. Our hydrodynamic simulation can well reproduce theoscillation period, but the damping timescale in the simulation is 1.5 times aslong as the observations. The results clearly show the prominence longitudinaloscillations around the dip of the prominence and our study suggests that therestoring force of the longitudinal oscillations might be the gravity.Radiation and heat conduction are insufficient to explain the decay of theoscillations. Other mechanisms, such as wave leakage and mass accretion, haveto be considered. The possible relation between the longitudinal oscillationsand the later eruption of a prominence thread, as well as a coronal massejection (CME), is also discussed.

Observation and Simulation of Longitudinal Oscillations of an Active Region Prominence