E-Print Archive

There are 4396 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
ERRATUM: "Exact Analytical Solutions of Continuity Equation for Electron Beams Precipitating in Coulomb Collisions" View all abstracts by submitter

Valentina Zharkova   Submitted: 2014-08-19 03:21

In this erratum letter we correct a mistake in the characteristics for differential density N obtained in 2014ApJ...788...42D} from the updated continuity equation for electron density and compare the solutions for electron density N obtained from continuity equations (CEs) for electron flux Nv and for electron density. We show that the corrected solution for N obtained from CE for electron density still has an additional exponential term of (E2+2a\xi)-1/4 comparing to the solution found from continuity equation for electron flux. This updated solution produces power law differential spectra of beam electrons as function of E2+2a\xi having a spectral index equal to -\frac{\gamma+1}{2} and not to -\frac{\gamma+0.5}{2} as it appears from the continuity equation for electron flux Nv. This updated solution is exactly the one reported by \citet{Syrovatsky72} indicating that their solution has been derived from CE for electron density and not for electron flux as stated in their paper. The difference in the spectral indices in energy spectra is also reflected in the spectral indices for mean electron spectra with a spectral index to be equal to \gamma-2, similar to \citet{Syrovatsky72, for the solutions from CE for electron density and equal to \gamma-2.5 if continuity equation for electron flux is used.

Authors: Dobranskis R.R. and Zharkova V.V.
Projects: None

Publication Status: ApJ subm. on 26 July '14
Last Modified: 2014-08-20 09:47
Go to main E-Print page  A study of density modulation index in the inner heliospheric solar  wind during solar cycle 23  Waiting time distribution of solar energetic particle events modeled with a non-stationary Poisson process  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
The Solar Memory From Hours to Decades
Solar chromosphere heating and generation of plasma outflows by impulsively generated two-fluid Alfvén waves
Radio evidence for a shock wave reflected by a coronal hole
Hemispheric sunspot numbers 1874 - 2020
Temperature in Solar Sources of 3He-rich Solar Energetic Particles and Relation to Ion Abundances
The long period of 3He-rich solar energetic particles measured by Solar Orbiter 2020 November 1723
Tracing Hα Fibrils through Bayesian Deep Learning
Energetics and 3-D Structure of Elementary Events in Solar Coronal Heating
Forecasting the Remaining Duration of an Ongoing Solar Flare
A fundamental mechanism of solar eruption initiation
Thermal Trigger for Solar Flares III: Effect of the Oblique Layer Fragmentation
Measurements of Coronal Magnetic Field Strengths in Solar Active Region Loops
Characteristic time of stellar flares on Sun-like stars
M-dwarf's Chromosphere, Corona and Wind Connection via the Nonlinear Alfvén Wave
Bayesian evidence for a nonlinear damping model for coronal loop oscillations
Small-scale Turbulent Motion of the Plasma in a Solar Filament as the Precursor of Eruption
Validation of the PDFI_SS method for electric field inversions using a magnetic flux emergence simulation
Investigation on the Spatiotemporal Structures of Supra-Arcade Spikes
Magnetic helicity and energy budget around large confined and eruptive solar flares
One dimensional prominence threads: I. Equilibrium models

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