E-Print Archive

There are 4035 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
Solar flare-related eruptions followed by long-lasting occultation of the emission in the He II 304 Å line and in microwaves View all abstracts by submitter

Victor Grechnev   Submitted: 2011-03-24 17:23

Plasma with a temperature close to the chromospheric one is ejected in solareruptions. Such plasma can occult some part of emission of compact sources inactive regions as well as quiet solar areas. Absorption phenomena can beobserved in the microwave range as the so-called 'negative bursts' and also inthe He II 304 Å line. The paper considers three eruptive events associated withrather powerful flares. Parameters of absorbing material of an eruption areestimated from multi-frequency records of a 'negative burst' in one event.'Destruction' of an eruptive filament and its dispersion like a cloud over ahuge area observed as a giant depression of the 304 Å line emission has beenrevealed in a few events. One such event out of three ones known to us isconsidered in this paper. Another event is a possibility.

Authors: V. V. Grechnev, I. V. Kuzmenko, I. M. Chertok, A. M. Uralov
Projects:

Publication Status: 2011 Accepted by Astronomy Reports
Last Modified: 2011-04-10 22:26
Go to main E-Print page  Observing Flux Rope Formation During the Impulsive Phase of a Solar Eruption  Time--Distance Helioseismology Data Analysis Pipeline for Helioseismic and Magnetic Imager onboard Solar Dynamics Observatory (SDO/HMI) and Its Initial Results  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
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