E-Print Archive

There are 4293 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
* News 04/04/20 * The archive is using a new backend database. This has thrown up a few SQL errors in the last few days. If you have any issues please email adavey@nso.edu with either the number of eprint you are trying to edit or a link to your preprint.

RESIK and RHESSI observations of the 20 September 2002 flare View all abstracts by submitter

Anna Kepa   Submitted: 2020-08-14 12:20

Soft X-ray spectra 3.33 A - 6.15 A from the RESIK instrument on CORONAS-F constitute a unique database for the study of the physical conditions of solar flare plasmas, enabling the calculation of differential emission measures. The two RESIK channels for the shortest wavelengths overlap with the lower end of RHESSI spectral energy range, which is located around 3 keV, making it possible to compare both data sets. We aim to compare observations from RESIK and RHESSI spectrometers and cross-correlate these instruments. Observations are compared with synthetic spectra calculated based on the results of one-dimensional hydrodynamical (1D-HD) modelling. The analysis was performed for the flare on 20 September 2002. We estimated the geometry of the flaring loop, necessary for 1D-HD modelling, based on images from RHESSI and SOHO/EIT. The distribution of non-thermal electrons (NTEs) was determined from RHESSI spectra. The 1D-HD model assumes that non-thermal electrons with a power-law spectrum were injected at the apex of the flaring loop. The NTEs then heat and evaporate the chromosphere, filling the loop with hot and dense plasma radiating in soft X-rays. The total energy of electrons was constrained by comparing observed and calculated fluxes from GOES 1 - 8 A data. We determined the temperature and density at every point of the flaring loop throughout the evolution of the flare, calculating the resulting X-ray spectra. The synthetic spectra calculated based on the results of hydrodynamic modelling for the 20 September 2002 flare are consistent within a factor of two with the observed RESIK spectra during most of the duration of the flare. This discrepancy factor is probably related to the uncertainty on the cross-calibration between RESIK and RHESSI instruments.

Authors: A. Kepa, R. Falewicz, M. Siarkowski, and M. Pietras

Publication Status: A&A (in press)
Last Modified: 2020-08-14 12:45
Go to main E-Print page  Sequential Lid Removal in a Triple-Decker Chain of CME-Producing Solar Eruptions  Starspot mapping with adaptive parallel tempering I: Implementation of computational code  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
Non-Neutralized Electric Current of Active Regions Explained as a Projection Effect
The effect of magnetic field on the damping of slow waves in the solar corona
Soft X-Ray Observations of Quiescent Solar Active Regions using Novel Dual-zone Aperture X-ray Solar Spectrometer (DAXSS)
Proper Orthogonal and Dynamic Mode Decomposition of Sunspot Data.
Statistical Properties of Superflares on Solar-type Stars: Results Using All of the Kepler Primary Mission Data
Turbulent viscosity and effective magnetic Prandtl number from simulations of isotropically forced turbulence
Time and Charge-Sign Dependence of the Heliospheric Modulation of Cosmic Rays
Bayesian Analysis of Quasi-periodic Pulsations in Stellar Flares
Cause and Kinematics of a Jetlike CME
The role of small-scale surface motions in the transfer of twist to a solar jet from a remote stable flux rope
Sub-second time evolution of Type III solar radio burst sources at fundamental and harmonic frequencies
Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare
Differential rotation of the solar corona: A new data-adaptive multiwavelength approach
Magnetic Helicity Flux across Solar Active Region Photospheres: I. Hemispheric Sign Preference in Solar Cycle 24
Seismological constraints on the solar coronal heating function
The Coronal Global Evolutionary Model: Using HMI Vector Magnetogram and Doppler Data to Determine Coronal Magnetic Field Evolution
Radio and X-ray Observations of Short-lived Episodes of Electron Acceleration in a Solar Microflare
Research progress based on observations of the New Vacuum Solar Telescope
Dynamics evolution of a solar active-region filament from quasi-static state to eruption: rolling motion, untwisting motion, material transfer, and chirality
Microwave Study of a Solar Circular Ribbon Flare

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