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020 _a9783030872779
_9978-3-030-87277-9
024 7 _a10.1007/978-3-030-87277-9
_2doi
050 4 _aTA1634
072 7 _aUYQV
_2bicssc
072 7 _aCOM012000
_2bisacsh
072 7 _aUYQV
_2thema
082 0 4 _a006.37
_223
100 1 _aPiana, Michele.
_eauthor.
_4aut
_4http://id.loc.gov/vocabulary/relators/aut
245 1 0 _aHard X-Ray Imaging of Solar Flares
_h[electronic resource] /
_cby Michele Piana, A. Gordon Emslie, Anna Maria Massone, Brian R. Dennis.
250 _a1st ed. 2022.
264 1 _aCham :
_bSpringer International Publishing :
_bImprint: Springer,
_c2022.
300 _aXVIII, 164 p. 53 illus., 33 illus. in color.
_bonline resource.
336 _atext
_btxt
_2rdacontent
337 _acomputer
_bc
_2rdamedia
338 _aonline resource
_bcr
_2rdacarrier
347 _atext file
_bPDF
_2rda
505 0 _a1. Hard X-ray Emission in Solar Flares -- 2. X-Ray Imaging Methods -- 3. RHESSI and STIX -- 4. Image Reconstruction Methods -- 5. Count-based Imaging Methods -- 6. Visibility-based Imaging Methods -- 7. Application to Solar Flares -- 8. Future Possibilities.
520 _aThe idea for this text emerged over several years as the authors participated in research projects related to analysis of data from NASA's RHESSI Small Explorer mission. The data produced over the operational lifetime of this mission inspired many investigations related to a specific science question: the when, where, and how of electron acceleration during solar flares in the stressed magnetic environment of the active Sun. A vital key to unlocking this science problem is the ability to produce high-quality images of hard X-rays produced by bremsstrahlung radiation from electrons accelerated during a solar flare. The only practical way to do this within the technological and budgetary limitations of the RHESSI era was to opt for indirect modalities in which imaging information is encoded as a set of two-dimensional spatial Fourier components. Radio astronomers had employed Fourier imaging for many years. However, differently than for radio astronomy, X-ray images produced by RHESSI had to be constructed from a very limited number of sparsely distributed and very noisy Fourier components. Further, Fourier imaging is hardly intuitive, and extensive validation of the methods was necessary to ensure that they produced images with sufficient accuracy and fidelity for scientific applications. This book summarizes the results of this development of imaging techniques specifically designed for this form of data. It covers a set of published works that span over two decades, during which various imaging methods were introduced, validated, and applied to observations. Also considering that a new Fourier-based telescope, STIX, is now entering its nominal phase on-board the ESA Solar Orbiter, it became more and more apparent to the authors that it would be a good idea to put together a compendium of these imaging methods and their applications. Hence the book you are now reading.
650 0 _aComputer vision.
650 0 _aLasers.
650 0 _aMathematical physics.
650 1 4 _aComputer Vision.
650 2 4 _aLaser.
650 2 4 _aTheoretical, Mathematical and Computational Physics.
700 1 _aEmslie, A. Gordon.
_eauthor.
_4aut
_4http://id.loc.gov/vocabulary/relators/aut
700 1 _aMassone, Anna Maria.
_eauthor.
_4aut
_4http://id.loc.gov/vocabulary/relators/aut
700 1 _aDennis, Brian R.
_eauthor.
_4aut
_4http://id.loc.gov/vocabulary/relators/aut
710 2 _aSpringerLink (Online service)
773 0 _tSpringer Nature eBook
776 0 8 _iPrinted edition:
_z9783030872762
776 0 8 _iPrinted edition:
_z9783030872786
776 0 8 _iPrinted edition:
_z9783030872793
856 4 0 _uhttps://doi.org/10.1007/978-3-030-87277-9
912 _aZDB-2-SCS
912 _aZDB-2-SXCS
942 _cSPRINGER
999 _c179119
_d179119