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Context: As a ubiquitous phenomenon, large-amplitude longitudinal filamentoscillations usually decay in 1--4 periods. Recently, we observed a decaylesscase of such oscillations in the corona. Aims: We try to understand thephysical process that maintains the decayless oscillation of the filament.Methods: Multi-wavelength imaging observations and magnetograms are collectedto study the dynamics of the filament oscillation and its associated phenomena.To explain the decayless oscillations, we also perform one-dimensionalhydrodynamic numerical simulations using the MPI-AMRVAC code. Results: Inobservations, the filament oscillates decaylessly with a period of $36.4 \pm0.3$ min for almost 4 hours before eruption. During oscillations, fourquasi-periodic jets emanate from a magnetic cancellation site near thefilament. The time interval between neighboring jets is $\sim 68.9 \pm 1.0$min. Numerical simulations constrained by the observations reproduced thedecayless longitudinal oscillations. However, it is surprising to find that theperiod of the decayless oscillations is not consistent with the pendulum model.Conclusions: We propose that the decayless longitudinal oscillations of thefilament are maintained by quasi-periodic jets, which is verified by thehydrodynamic simulations. More importantly, it is found that, when driven byquasi-periodic jets, the period of the filament longitudinal oscillationsdepends also on the driving period of the jets, not simply the pendulum period.With a parameter survey in simulations, we derived a formula, by which one canderive the pendulum oscillation period using the observed period of decaylessfilament oscillations and the driving periods of jets.

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets