E-Print Archive

There are 4035 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Formation and evolution of a multi-threaded prominence View all abstracts by submitter

Manuel Luna   Submitted: 2012-01-18 09:22

We investigate the process of formation and subsequent evolution ofprominence plasma in a filament channel and its overlying arcade. We constructa three-dimensional time-dependent model of an intermediate quiescentprominence. We combine the magnetic field structure with one-dimensionalindependent simulations of many flux tubes, of a three-dimensional sheareddouble arcade, in which the thermal nonequilibrium process governs the plasmaevolution. We have found that the condensations in the corona can be dividedinto two populations: threads and blobs. Threads are massive condensations thatlinger in the field line dips. Blobs are ubiquitous small condensations thatare produced throughout the filament and overlying arcade magnetic structure,and rapidly fall to the chromosphere. The threads are the principalcontributors to the total mass. The total prominence mass is in agreement withobservations, assuming a reasonable filling factor. The motion of the threadsis basically horizontal, while blobs move in all directions along the field.The peak velocities for both populations are comparable. We have generatedsynthetic images of the whole structure in an Hα proxy and in two EUVchannels of the AIA instrument aboard SDO, thus showing the plasma at cool,warm, and hot temperatures. The predicted differential emission measure of oursystem agrees very well with observations. We conclude that the sheared-arcademagnetic structure and plasma behavior driven by thermal nonequilibrium fitwell the abundant observational evidence for typical intermediate prominences.

Authors: M. Luna, J. T. Karpen, C. R. DeVore
Projects: None

Publication Status: ApJ, in press (ApJ, 746, 30)
Last Modified: 2012-01-18 10:28
Go to main E-Print page  Magnetohydrodynamic Waves in Partially Ionized Prominence Plasmas  Evolution of Magnetic Field and Energy in A Major Eruptive Active Region Based on SDO/HMI Observation  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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
Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?
Impacts On Proton Fluxes Observed During Different Interplanetary Conditions
Coronal Loop Seismology Using Standing Kink Oscillations With a Lookup Table
Data-Optimized Coronal Field Model: I. Proof of Concept
Coronal Bright Points
Difference of source regions between fast and slow coronal mass ejections
Invited Review: Signatures of Magnetic Flux Ropes in the Low Solar Atmosphere Observed in High Resolution
Do Kepler superflare stars really include slowly-rotating Sun-like stars ? - Results using APO 3.5m telescope spectroscopic observations and Gaia-DR2 data -
Magnetically Induced Current Piston for Generating Extreme-ultraviolet Fronts in the Solar Corona
Magnetic Field Dynamics and Varying Plasma Emission in Large-scale Coronal Loops
Nonlinear Evolution of Ion Kinetic Instabilities in the Solar Wind
What determines the X-ray intensity and duration of a solar flare?
Fast Magnetoacoustic Wave Trains with Time-dependent Drivers
Three-dimensional reconstruction of CME-driven shock-streamer interaction from radio observations: a different take on the diagnostics of coronal magnetic fields
The soft X-ray spectrometer polarimeter SolpeX
Variable emission mechanism of a Type IV radio burst
Inference of magnetic field strength and density from damped transverse coronal waves
Frequency-Distance Structure of Solar Radio Sources Observed by LOFAR
The birth of a coronal mass ejection
Properties of slow magnetoacoustic oscillations of solar coronal loops by multi-instrumental observations

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