Study On Observation And Theory Of Prominence Oscillations

Solar prominence oscillations are related to many aspects of solar activity, including active region eruptions (primarily flare and CME) and coronal wave, which mostly are EUV waves. We analyzed three large prominence oscillations, these events give us a chance to study the prominence oscillations carried by the same prominence and disturbed by a series of eruptions from the same active region. And it is a very important method for measuring the magnetic field by prominence coronal seismology. So studying the prominence oscillations has vital scientific significance.In this paper, we used the observations of SDO/AIA, analyzed the triggers and dynamic parameters of prominence oscillations, the primary contents and conclusions as follows:We analyze three large amplitude traverse prominence oscillations. Firstly, we analyze the flare and CME of the source region. It is found that three of the eruptions have M class flares, with the later two eruptions accompanied with CMEs. We observe the two EUV wave fronts driven by the CMEs in the running difference and calculate their speeds according to the time lag between the CME and beginning of prominence oscillations. These EUV waves are the cause of the prominence oscillations. However, we could not observe the EUV wave front for the first eruption Yet according to the propagating speed, v=967±50 Km/s, estimated from the timing difference between the flare peak time and the start of the prominence oscillation. we suggest that the first wave is possibly by as Morten wave or blast wave driven by flare.We make several slits in different heights of prominence in the same oscillation and measure the beginning time and period of every oscillation. We compare the three oscillations, considering their oscillation modes are global kink. In addition, we examine the horn oscillations in the same way and compare with the prominence oscillations. We conclude that the horn oscillations have different periods and amplitudes, possibly due to the spatial extension of horns into the corona.Moreover, we fit the parameter for prominence oscillations, considering a damping sin function and a linear shift function, we get the periods, which are 25 ±2 min,36±2 min,28±2 min; amplitudes, which are 2.62±1.0 arcsec,8.59±1.0 arcsec, 9.07±1.0 arcsec; damping times, which are 120±20 min,145±20 min,165±10 min. we also analyze the damping mechanism. In addition, we estimate the magnetic field by the published models of prominence seismology.