E-Print Archive

There are 4414 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
One dimensional prominence threads: I. Equilibrium models View all abstracts by submitter

Jaume Terradas   Submitted: 2021-06-15 10:49

Threads are the building blocks of solar prominences and very often show longitudinal oscillatory motions that are strongly attenuated with time. The damping mechanism responsible for the reported oscillations is not fully understood yet. To understand the oscillations and damping of prominence threads it is mandatory to investigate first the nature of the equilibrium solutions that arise under static conditions and under the presence of radiative losses, thermal conduction and background heating. This provides the basis to calculate the eigenmodes of the thread models. The nonlinear ordinary differential equations for hydrostatic and thermal equilibrium under the presence of gravity are solved using standard numerical techniques and simple analytical expressions are derived under certain approximations. The solutions to the equations represent a prominence thread, i.e., a dense and cold plasma region of a certain length that connects with the corona through a prominence corona transition region (PCTR). The solutions can also match with a chromospheric-like layer if a spatially dependent heating function localised around the footpoints is considered. We have obtained static solutions representing prominence threads and have investigated in detail the dependence of these solutions on the different parameters of the model. Among other results, we have shown that multiple condensations along a magnetic field line are possible, and that the effect of partial ionisation in the model can significantly modify the thermal balance in the thread and therefore their length. This last parameter is also shown to be comparable to that reported in the observations when the radiative losses are reduced for typical thread temperatures.

Authors: J. Terradas, M. Luna, R. Soler, R. Oliver, M. Carbonell, J. L Ballester
Projects: None

Publication Status: Accepted for publication in A&A
Last Modified: 2021-06-16 08:40
Go to main E-Print page  Magnetic helicity and energy budget around large confined and eruptive solar flares  Time-dependent properties of sunspot groups -- I. Lifetime and asymmetric evolution  Edit Entry  Download Preprint  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
Formation of Magnetic Flux Rope during Solar Eruption. I. Evolution of Toroidal Flux and Reconnection Flux
Stereoscopy of extreme UV quiet Sun brightenings observed by Solar Orbiter/EUI
Solar Flare Effects on the Earth’s Lower Ionosphere
Measurements of Photospheric and Chromospheric Magnetic Field Structures Associated with Chromospheric Heating over a Solar Plage Region
Probing Current Sheet Instabilities from Flare Ribbon Dynamics
Global Nature of Solar Coronal Shock Waves shown by Inconsistency between EUV Waves and Type II Radio Bursts
Solar surges related to UV bursts: Characterization through k-means, inversions and density diagnostics
A revised cone model and its application to non-radial prominence eruptions
Zonal harmonics of solar magnetic field for solar cycle forecast
TESS observations of flares and quasi-periodic pulsations from low mass stars and potential impact on exoplanets
Kink oscillations of coronal loops
First Frequency-Time-Resolved Imaging Spectroscopy Observations of Solar Radio Spikes
Magnetic Flux and Magnetic Non-potentiality of Active Regions in Eruptive and Confined Solar Flares
Observations of shock propagation through turbulent plasma in the solar corona
The Formation and Lifetime of Outflows in a Solar Active Region
Localised acceleration of energetic particles by a weak shock in the solar corona
Stereoscopic Measurements of Coronal Doppler Velocities
Multi-wavelength Observations of a Metric Type-II Event
A physics-based method that can predict imminent large solar flares
The Solar Memory From Hours to Decades

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

© 2000-2020 Solar Physics Group - Montana State University