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
The RHESSI Imaging Concept View all abstracts by submitter

Gordon J. Hurford   Submitted: 2002-09-19 14:24

The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) images solar hard X-ray and gamma-rays from 3 keV to 15 MeV with spatial resolution as high as 2.3 arcseconds. Instead of conventional optics, nine rotating modulation collimators are used to time-modulate the incident flux as the spacecraft rotates in a manner which depends on the location and morphology of the source. Starting from the arrival time of individual photons, ground-based software then uses the time-modulated signals to reconstruct the image of the source. The purpose of this paper is to convey both and intuitive feel and the mathematical basis for this imaging process along with its strengths and weaknesses. Following a review of the relevant hardware, the imaging principles and the basic back projection method are described, along with their relation to Fourier Transforms. Several specific algorithms (CLEAN, MEM. PIXONS and Forward Fitting) applicable to RHESSI imaging are briefly described.

Authors: G. J. Hurford, E. J. Schmahl, A. J. Conway, B. R. Dennis, R. A. Schwartz, R.P.Lin, J. McTiernan, D. M. Smith, C. Johns-Krull, A. Csillaghy, M. J. Aschwanden and T. R. Metcalf

Publication Status: Solar Physics (in press)
Last Modified: 2002-09-20 11:37
Go to main E-Print page  The PMTRAS Roll Aspect System on RHESSI  The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI)  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