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is underestimated if no linear polarization spectra is available from observations. Since linear polarization signatures are weaker compared circular polarization their detections are not as reliable, particularly for cool stars. With more modern spectropolarimeters such as the recently installed SPIRou at CFHT and CRIRES+, currently in the process of installation, at the
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114:. It is now offering the opportunity to undertake systematic studies of stellar magnetism and is also yielding information on the geometry of large arches that magnetic fields are able to develop above stellar surfaces. To collect the observations related to Zeeman-Doppler Imaging, astronomers use stellar spectropolarimeters like ESPaDOnS at
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The technique is very reliable, as the reconstruction of the magnetic field maps with different algorithms yield almost identical results, even with poorly sampled data sets. It has however been shown, from both numerical simulations and observations, that the magnetic field strength and complexity
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This technique is the first to enable the reconstruction of the vectorial magnetic geometry of stars similar to the
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The method was first proposed by Marsh and Horne in 1988, as a way to interpret the
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466:"First Zeeman Doppler Imaging of a Cool Star Using All Four Stokes Parameters"
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Donati, J.-F.; Howarth, I. D.; Jardine, M. M.; Petit, P.; et al. (2006).
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376:"Comparisons of images derived from independent Zeeman Doppler imaging codes"
222:"The surprising magnetic topology of τ Sco: fossil remnant or dynamo output?"
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image reconstruction; it yields the simplest magnetic field geometry (as a
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expansion) among the various solutions compatible with the data.
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This method makes use of the ability of magnetic fields to
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Stellar tomography: when medical imaging helps astronomy
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Rosén, L.; Kochukhov, O.; Wade, G. A. (2015-05-29).
181:"Images of accretion discs – II. Doppler tomography"
42:), reconstructed by means of Zeeman–Doppler Imaging
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380:Monthly Notices of the Royal Astronomical Society
227:Monthly Notices of the Royal Astronomical Society
185:Monthly Notices of the Royal Astronomical Society
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590:Recent examples of using Zeeman-Doppler Imaging
179:Marsh, T. R.; Horne, K. (1 November 1988).
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330:: CS1 maint: archived copy as title (
77:formed in the stellar atmosphere (the
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73:the light emitted (or absorbed) in
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58:technique dedicated to the
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442:10.1051/0004-6361:20020300
97:cataclysmic variable stars
34:Surface magnetic field of
470:The Astrophysical Journal
138:), as well as NARVAL at
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206:10.1093/mnras/235.1.269
580:Zeeman-Doppler Imaging
144:Pic du Midi de Bigorre
140:Bernard Lyot Telescope
52:Zeeman–Doppler imaging
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18:Zeeman-Doppler imaging
346:"Home Page of Narval"
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156:Very Large Telescope
132:La Silla Observatory
128:ESO's 3.6m telescope
126:), HARPSpol at the
88:at stellar surface.
492:2015ApJ...805..169R
392:2000MNRAS.318..961H
250:2006MNRAS.370..629D
197:1988MNRAS.235..269M
105:spherical harmonics
350:www.ast.obs-mip.fr
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599:Categories
526:2020-10-12
483:1504.00176
476:(2): 169.
360:2021-10-28
317:2015-09-08
292:2021-10-28
282:"ESPaDOnS"
166:References
559:"CRIRES+"
516:118833875
508:1538-4357
451:0004-6361
120:Mauna Kea
83:vectorial
563:Archived
545:Archived
541:"SPIRou"
520:Archived
354:Archived
326:cite web
311:Archived
286:Archived
71:polarize
488:Bibcode
429:Bibcode
388:Bibcode
268:7054292
246:Bibcode
193:Bibcode
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148:France
124:Hawaii
512:S2CID
478:arXiv
264:S2CID
236:arXiv
160:Chile
136:Chile
54:is a
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332:link
116:CFHT
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474:805
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425:388
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