E-Print Archive

There are 3914 abstracts currently viewable.


Search:

Advanced Search
Options
Main Page Add New E-Print Submitter
Information
Feedback
News Help/FAQ About Preferences
Manage Key Phrase
Notification
Comparing UV/EUV line parameters and magnetic field in a quiescent prominence with tornadoes View all abstracts by submitter

Peter Levens   Submitted: 2017-08-21 08:45

Context. Understanding the close relationship between the plasma and the magnetic field is important to describe and explain the observed complex dynamics of solar prominences. Aims. We determine if a close relationship between plasma and magnetic field parameters measured in a well-observed solar prominence with high spatial resolution can be found. Methods. We select a prominence observed on 15 July 2014 from space (IRIS, Hinode, SDO) and from the ground (THEMIS). We perform a robust co-alignment of the data sets using a 2D cross-correlation technique. We derive the magnetic field parameters from spectropolarimetric measurements of the He I D3 line taken by THEMIS. Line ratios and line-of-sight velocities from the Mg II h and k lines observed by IRIS are compared with magnetic field strength, inclination and azimuth. Electron densities are calculated using Hinode/EIS Fe XII line ratios and also compared with THEMIS and IRIS data. Results. We find Mg II k/h ratios of around 1.4 everywhere, similar to values found previously in prominences. We also find that the magnetic field is strongest (around 30 G) and predominantly horizontal in the tornado-like legs of the prominence. The k3 Doppler shift is found to be between ± 10 km s-1 everywhere. Electron densities at a temperature of 1.5e6 K are found to be around 1e9 /cm3. No significant correlations are found between the magnetic field parameters, and any of the other plasma parameters inferred from EUV spectroscopy, which may be explained by the large differences in the temperatures of the lines used in this study. Conclusions. This is the first time that a detailed statistical study of plasma and magnetic field parameters has been carried out at high spatial resolution in a prominence. Our results provide important constraints on future models of the plasma and magnetic field in these structures.

Authors: P. J. Levens, N. Labrosse, B. Schmieder, A. López Ariste, L. Fletcher
Projects: Hinode/EIS,Hinode/SOT,IRIS,THEMIS/MTR

Publication Status: A&A (accepted)
Last Modified: 2017-08-23 12:50
Go to main E-Print page  Seismology of contracting and expanding coronal loops using damping of kink oscillations by mode coupling  Modeling Coronal Response in Decaying Active Regions with Magnetic Flux  Transport and Steady Heating  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Key
Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Linear Polarization Features in the Quiet-Sun Photosphere: Structure and Dynamics
Solar Microflares Observed by SphinX and RHESSI
Two Kinds of Dynamic Behavior in a Quiescent Prominence Observed by the NVST
Resistively-limited current sheet implosions in planar anti-parallel (1D) and null-point containing (2D) magnetic field geometries
Is It Small-scale Weak Magnetic Activity That Effectively Heats the Upper Solar Atmosphere?
Self-Similar Approach for Rotating Magnetohydrodynamic Solar and Astrophysical Structures
Spectroscopic and imaging observations of small-scale reconnection events
A Study of Magnetic Field Characteristics of Flaring Active Region Based on Nonlinear Force-free Field Extrapolation
A Study of a Compound Solar Eruption with Two Consecutive Erupting Magnetic Structures
Non-potential magnetic helicity ratios at the onset of eruptions
Solar Cycle Observations of the Neon Abundance in the Sun-as-a-star
Subresolution Activity in Solar and Stellar Coronae from Magnetic Field Line Tangling
A Model of Zebra Patterns in Solar Radio Emission
Three-dimensional magnetic reconnection in a collapsing coronal loop system
On the Synthesis of GOES Light Curves from Numerical Models
Efficient Calculation of Non-Local Thermodynamic Equilibrium Effects in Multithreaded Hydrodynamic Simulations of Solar Flares
2D solar wind speeds from 6 to 26 solar radii in solar cycle 24 by using Fourier filtering
Non-damping oscillations at flaring loops
An Event-Based Verification Scheme for the Real-Time Flare Detection System at Kanzelhöhe Observatory
Computation of Relative Magnetic Helicity in Spherical Coordinates

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey



© 2003 Solar Physics Group - Montana State University