Estimation of Solar Prominence Magnetic Fields Based on the Reconstructed 3D Trajectories of Prominence Knots

We present an estimation of the lower limits of local magnetic field strengths in quiescent, activated, and active (surges) prominences, based on reconstructed three-dimensional (3D) trajectories of individual prominence knots. The 3D trajectories, velocities, tangential and centripetal acceleration...

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Bibliographic Details
Published in:Solar physics 2012-10, Vol.280 (2), p.445-456
Main Authors: Zapiór, Maciej, Rudawy, Paweł
Format: Article
Language:English
Subjects:
Activated
Advances in European Solar Physics
Astrophysics and Astroparticles
Atmospheric Sciences
Knots
Magnetic fields
Physics
Physics and Astronomy
Prominences
Solar physics
Solar prominences
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Surges
Three dimensional
Trajectories
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Summary:We present an estimation of the lower limits of local magnetic field strengths in quiescent, activated, and active (surges) prominences, based on reconstructed three-dimensional (3D) trajectories of individual prominence knots. The 3D trajectories, velocities, tangential and centripetal accelerations of the knots were reconstructed using observational data collected with a single ground-based telescope equipped with a Multi-channel Subtractive Double Pass imaging spectrograph. Lower limits of magnetic fields channeling observed plasma 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, we found that the magnetic fields channeling two observed surges range from 16 to 40 Gauss, while in quiescent and activated prominences they were less than 10 Gauss. Our results are consistent with previous detections of weak local magnetic fields in the solar prominences.
ISSN:0038-0938
1573-093X
DOI:10.1007/s11207-012-0072-z