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We present an estimation of the lower limits of local magnetic fields inquiescent, activated, and active (surges) promineces, based on reconstructed3-dimensional (3D) trajectories of individual prominence knots. The 3Dtrajectories, velocities, tangential and centripetal accelerations of the knotswere reconstructed using observational data collected with a singleground-based telescope equipped with a Multi-channel Subtractive Double Passimaging spectrograph. Lower limits of magnetic fields channeling observedplasma flows were estimated under assumption of the equipartition principle.Assuming approximate electron densities of the plasma n_e = 5*10^{11} cm^{-3}in surges and n_e = 5*10^{10} cm^{-3} in quiescent/activated prominences, wefound that the magnetic fields channeling two observed surges range from 16 to40 Gauss, while in quiescent and activated prominences they were less than 10Gauss. Our results are consistent with previous detections of weak localmagnetic fields in the solar prominences.

Estimation of solar prominence magnetic fields based on the reconstructed 3D trajectories of prominence knots