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
Differential Emission Measures from the Regularized Inversion of Hinode and SDO data View all abstracts by submitter

Iain Hannah   Submitted: 2012-01-23 11:24

We develop and apply an enhanced regularization algorithm, used inRHESSI X-ray spectral analysis, to constrain the ill-posed inverseproblem that is determining the DEM from solar observations. Wedemonstrate this computationally fast technique applied to a range ofDEM models simulating broadband imaging data from SDO/AIA and highresolution line spectra from Hinode/EIS, as well as actual activeregion observations with Hinode/EIS and XRT. As this regularizationmethod naturally provides both vertical and horizontal (temperatureresolution) error bars we are able to test the role of uncertaintiesin the data and response functions. The regularization method is ableto successfully recover the DEM from simulated data of a variety ofmodel DEMs (single Gaussian, multiple Gaussians and CHIANTI DEMmodels). It is able to do this, at best, to over four orders ofmagnitude in DEM space but typically over two orders of magnitude frompeak emission. The combination of horizontal and vertical error barsand the regularized solution matrix allows us to easily determine theaccuracy and robustness of the regularized DEM. We find that thetypical range for the horizontal errors is DeltalogTapprox 0.1-0.5 and this is dependent on the observed signal to noise,uncertainty in the response functions as well as the source model andtemperature. With Hinode/EIS an uncertainty of 20% greatly broadensthe regularized DEMs for both Gaussian and CHIANTI models althoughinformation about the underlying DEMs is still recoverable. Whenapplied to real active region observations with Hinode/EIS and XRT theregularization method is able to recover a DEM similar to that foundvia a MCMC method but in considerably less computational time.

Download page contains links to both the preprint in arXiv as well as the codes used.

Authors: I. G. Hannah, E. P. Kontar
Projects: Hinode/EIS,Hinode/XRT,SDO-AIA,SDO-EVE

Publication Status: A&A (accepted)
Last Modified: 2012-01-24 11:24
Go to main E-Print page  Stability of thermal modes in cool prominence plasmas  WAVE LEAKAGE AND RESONANT ABSORPTION IN A LOOP EMBEDDED IN A CORONAL ARCADE  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