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008			211221s2022 sz | s |||| 0|eng d
020			_a9783030872779
024	7		_a10.1007/978-3-030-87277-9 _2doi
040			_aES-MaUEC _bspa _cES-MaUEC _dES-MaUEC
050		4	_aQB524 _b2022 EB
100	1		_aPiana, Michele _eautor _9683092
245	1	0	_aHard X-Ray Imaging of Solar Flares _cby Michele Piana, A. Gordon Emslie, Anna Maria Massone, Brian R. Dennis
250			_aFirst edition 2022
264		1	_aCham _bSpringer International Publising _c2022
300			_a1 recurso en línea (XVIII, 164 páginas) _b53 ilustraciones, 33 ilustraciones a color
336			_2rdacontent _aTexto _btxt
337			_2rdamedia _aelectrónico _bc
338			_2rdacarrier _arecurso electrónico _bcr
347			_aarchivo de texto _bPDF
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.
988			_aSpringer_Computer_2022
650		7	_2embne _9683091 _aActividad solar
650		7	_2embne _9139975 _aRayos X
700	1		_aEmslie, A. Gordon _eautor
700	1		_aMassone, Anna Maria _eautor
700	1		_aDennis, Brian R _eautor
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://go.openathens.net/redirector/universidadeuropea.es?url=https://doi.org/10.1007/978-3-030-87277-9 _zAcceso a este recurso digital (usuarios Universidad Europea de Madrid)
942			_2lcc _cLE _n0
998			_b03/2022 _dz _eu _zSI