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 Microflares Observed by SphinX and RHESSI View all abstracts by submitter

Tomasz Mrozek   Submitted: 2018-07-12 02:19

In 2009 the Russian Complex Orbital Observations Near-Earth of Activity of the Sun (CORONAS-Photon) satellite was launched carrying the Polish Solar PHotometer In X-rays (SphinX). The SphinX was the most sensitive in the spectral range 1.2-15 keV thus an excellent opportunity appeared for comparison with low-energy end of Ramaty High Energy Solar Spectroscopic Imager (RHESSI) spectra. Common spectral measurements with these instruments cover the range where most of the flare energy is accumulated. We have chosen four consecutive small solar events observed on 4 July 2009 at 13:43 UT, 13:48 UT, 13:52 UT, and 13:55 UT, ( RHESSI flare peak times) and used them for comparison of the data and results from both instruments. Moreover, we included Geostationary Operational Environmental Satellite (GOES) records in our analysis. In practice the range of comparison performed for SphinX and RHESSI is limited roughly to 3-6 keV. RHESSI's fluxes measured with a use of one, four, and nine detectors in the 3-4 keV energy band agree with SphinX measurements. However, we observed that SphinX spectral irradiances are three times higher than RHESSI in the 4-6 keV energy band. This effect contributes to the difference in obtained emission measures, but the derived temperatures of plasma components are similar. RHESSI spectra were fitted using a model with two thermal components. We have found that RHESSI hot component is in agreement with GOES and RHESSI hotter component fits well with the SphinX flaring component.Moreover, we calculated the so-called thermodynamic measure and the total thermal energy content in the four microflares studied. The results obtained show that SphinX is a very sensitive complementary observatory for RHESSI and GOES.

Authors: Tomasz Mrozek, Szymon Gburek, Marek Siarkowski, Barbara Sylwester, Janusz Sylwester, Anna Kepa, Magdalena Gryciuk
Projects: CORONAS-F/SphinX,RHESSI

Publication Status: published
Last Modified: 2018-07-17 10:51
Go to main E-Print page  Linear Polarization Features in the Quiet-Sun Photosphere: Structure and Dynamics  Two Kinds of Dynamic Behavior in a Quiescent Prominence Observed by the NVST  Edit Entry  Download Preprint  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