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Surface magnetism of cool stars
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
Univ Toulouse, UPS OMP, IRAP, Toulouse, France.;CNRS, Inst Rech Astrophys & Planetol, Toulouse, France..
Leibniz Inst Astrophys Potsdam AIP, Potsdam, Germany..
Leibniz Inst Astrophys Potsdam AIP, Potsdam, Germany..
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2017 (English)In: Astronomical Notes - Astronomische Nachrichten, ISSN 0004-6337, E-ISSN 1521-3994, Vol. 338, no 4, 428-441 p.Article in journal (Refereed) Published
Abstract [en]

Magnetic fields are essential ingredients of many physical processes in the interiors and envelopes of cool stars. Yet their direct detection and characterization is notoriously difficult, requiring high-quality observations and advanced analysis techniques. Significant progress has been recently achieved by several types of direct magnetic field studies on the surfaces of cool, active stars. In particular, complementary techniques of field topology mapping with polarization data and total magnetic flux measurements from intensity spectra have been systematically applied to different classes of active stars, leading to interesting and occasionally controversial results. In this paper, we summarize the current status of direct magnetic field studies of cool stars and investigations of surface inhomogeneities caused by the field, based on the material presented at the Cool Stars 19 splinter session.

Place, publisher, year, edition, pages
WILEY-V C H VERLAG GMBH , 2017. Vol. 338, no 4, 428-441 p.
Keyword [en]
stars: activity, stars: late-type, stars: low-mass, stars: magnetic field, starspots
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-324614DOI: 10.1002/asna.201713310ISI: 000400944700007OAI: oai:DiVA.org:uu-324614DiVA: diva2:1110708
Funder
Swedish Research CouncilSwedish National Space Board
Available from: 2017-06-16 Created: 2017-06-16 Last updated: 2017-06-16Bibliographically approved

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Kochukhov, OlegRosén, Lisa
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