E-Print Archive

There are 4036 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Pulse-driven nonlinear Alfvén waves and and their role in e the spectral line broadening View all abstracts by submitter

Piotr Chmielewski   Submitted: 2012-07-25 13:21

We study the impulsively generated non-linear Alfvén waves in the solar atmosphere, and describe their most likely role in the observed non-thermal broadening of some spectral lines in solar coronal holes. We solve numerically the time-dependent magnetohydrodynamic equations to find temporal signatures of large-amplitude Alfvén waves in the model atmosphere of open and expanding magnetic field configuration, with a realistic temperature distribution. We calculate the temporally and spatially averaged, instantaneous transversal velocity of non-linear Alfvén waves at different heights of the model atmosphere, and estimate its contribution in the unresolved non-thermal motions caused by the waves. We find that the non-linear, pulse-driven Alfvén waves with the amplitude Av =50 km s-1 are the most likely candidates for the non-thermal broadening of Si VIII λ1445.75? line profiles in the polar coronal hole as reported by Banerjee et al. (1998). We also demonstrate that the Alfvén waves driven by comparatively smaller velocity pulse with its amplitude Av =25 km s-1 may contribute to the spectral line width of Si VIII λ1445.75? at various heights in coronal hole as reported by Dolla & Soloman (2008), however, without any significant role in its observed broadening. Some agreement of our results with observational data gives an indirect evidence for the existence of larger amplitude, pulse-driven Alfvén waves in solar coronal holes. The main conclusion of this paper is that non-linear Alfvén waves excited impulsively in the lower solar atmosphere of polar coronal holes are responsible for some observed spectral line broadening. This is an important result as it allows us to conclude that such large amplitude and pulse-driven Alfvén waves do indeed exist in solar coronal holes. The existence of these waves and their undamped growth may impart the required momentum to accelerate the solar wind.

Authors: P. Chmielewski, A.K. Srivastava, K. Murawski, and Z.E. Musielak
Projects: None

Publication Status: Submitted
Last Modified: 2012-07-25 14:18
Go to main E-Print page  X-raying hot plasma in solar active regions with the SphinX spectrometer  The Role of fast magnetosonic waves in the release and conversion via reconnection of energy stored by a current sheet  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
Flare reconnection-driven magnetic field and Lorentz force variations at the Sun's surface
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

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