Estimation of Solar Prominence Magnetic Fields Based on the Reconstructed 3D Trajectories of Prominence KnotsReport as inadecuate




Estimation of Solar Prominence Magnetic Fields Based on the Reconstructed 3D Trajectories of Prominence Knots - Download this document for free, or read online. Document in PDF available to download.

Solar Physics

, Volume 280, Issue 2, pp 445–456

First Online: 31 July 2012Received: 15 November 2011Accepted: 09 July 2012

Abstract

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 ne=5×10 cm in surges and ne=5×10 cm 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.

KeywordsProminences, dynamics Prominences, magnetic fields Advances in European Solar Physics

Guest Editors: Valery M. Nakariakov, Manolis K. Georgoulis, and Stefaan Poedts

Download fulltext PDF



Author: Maciej Zapiór - Paweł Rudawy

Source: https://link.springer.com/







Related documents