Direct observation of magnetic cycles in Sun‐like stars
Identifieur interne : 000480 ( Istex/Corpus ); précédent : 000479; suivant : 000481Direct observation of magnetic cycles in Sun‐like stars
Auteurs : A. Morgenthaler ; P. Petit ; J. Morin ; M. Aurière ; B. Dintrans ; R. Konstantinova-Antova ; S. MarsdenSource :
- Astronomische Nachrichten [ 0004-6337 ] ; 2011-12.
English descriptors
- KwdEn :
- Chromospheric, Chromospheric activity, Chromospheric emission, Collier cameron, Cool stars, Cycle lengths, Data reduction, Data sets, Different types, Direct observation, Donati, Gmbh, Instrumental setup, Kgaa, Magnetic activity, Magnetic cycles, Magnetic geometry, Magnetic maps, Magnetic variability, Magnetic vector, Mnras, Narval, Narval spectropolarimeter, Online colour, Polarity reversals, Polarity switches, Radial velocity, Representative examples, Reversal, Rotation period, Rotation periods, Rotational modulation, Stellar, Stellar masses, Stellar sample, Temporal evolution, Variability, Verlag, Verlag gmbh, Weinheim, Wide range, Zeeman signatures.
- Teeft :
- Chromospheric, Chromospheric activity, Chromospheric emission, Collier cameron, Cool stars, Cycle lengths, Data reduction, Data sets, Different types, Direct observation, Donati, Gmbh, Instrumental setup, Kgaa, Magnetic activity, Magnetic cycles, Magnetic geometry, Magnetic maps, Magnetic variability, Magnetic vector, Mnras, Narval, Narval spectropolarimeter, Online colour, Polarity reversals, Polarity switches, Radial velocity, Representative examples, Reversal, Rotation period, Rotation periods, Rotational modulation, Stellar, Stellar masses, Stellar sample, Temporal evolution, Variability, Verlag, Verlag gmbh, Weinheim, Wide range, Zeeman signatures.
Abstract
A sample of 19 solar‐type stars, probing masses between 0.6 and 1.4 solar masses and rotation periods between 3.4 and 43 days, was regularly observed using the NARVAL spectropolarimeter at Telescope Bernard Lyot (Pic du Midi, France) between 2007 and 2011. The Zeeman‐Doppler Imaging technique is employed to reconstruct the large‐scale photospheric magnetic field structure of the targets and investigate its long‐term temporal evolution. We present here the first results of this project with the observation of short magnetic cycles in several stars, showing up a succession of polarity reversals over the timespan of our monitoring. Preliminary trends suggest that short cycles are more frequent for stellar periods below a dozen days and for stellar masses above about one solar mass. The cycles lengths unveiled by the direct tracking of polarity switches are significantly shorter than those derived from previous studies based on chromospheric activity monitoring, suggesting the coexistence of several magnetic timescales in a same star (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Url:
DOI: 10.1002/asna.201111592
Links to Exploration step
ISTEX:1908BA3C88460D395B98E5EAB0B43CD6ED563BA2Le document en format XML
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Morgenthaler</name><affiliation><mods:affiliation>Université de Toulouse, UPS‐OMP, Institut de Recherche en Astrophysique et Planétologie, Toulouse, France</mods:affiliation></affiliation><affiliation><mods:affiliation>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 Avenue Edouard Belin, F‐31400, Toulouse, France</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: amorgent@ast.obs‐mip.fr</mods:affiliation></affiliation><affiliation><mods:affiliation>Correspondence address: Université de Toulouse, UPS‐OMP, Institut de Recherche en Astrophysique et Planétologie, Toulouse, France</mods:affiliation></affiliation></author><author><name sortKey="Petit, P" sort="Petit, P" uniqKey="Petit P" first="P." last="Petit">P. 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Marsden</name><affiliation><mods:affiliation>Centre for Astronomy, School of Engineering and Physical Sciences, James Cook University, Townsville 4811, Australia</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Astronomische Nachrichten</title><title level="j" type="sub">Magnetic fields in stars and exoplanets</title><title level="j" type="alt">ASTRONOMISCHE NACHRICHTEN</title><idno type="ISSN">0004-6337</idno><idno type="eISSN">1521-3994</idno><imprint><biblScope unit="vol">332</biblScope><biblScope unit="issue">9‐10</biblScope><biblScope unit="page" from="866">866</biblScope><biblScope unit="page" to="871">871</biblScope><biblScope unit="page-count">6</biblScope><publisher>WILEY‐VCH Verlag</publisher><pubPlace>Berlin</pubPlace><date type="published" when="2011-12">2011-12</date></imprint><idno type="ISSN">0004-6337</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0004-6337</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Chromospheric</term><term>Chromospheric activity</term><term>Chromospheric emission</term><term>Collier cameron</term><term>Cool stars</term><term>Cycle lengths</term><term>Data reduction</term><term>Data sets</term><term>Different types</term><term>Direct observation</term><term>Donati</term><term>Gmbh</term><term>Instrumental setup</term><term>Kgaa</term><term>Magnetic activity</term><term>Magnetic cycles</term><term>Magnetic geometry</term><term>Magnetic maps</term><term>Magnetic variability</term><term>Magnetic vector</term><term>Mnras</term><term>Narval</term><term>Narval spectropolarimeter</term><term>Online colour</term><term>Polarity reversals</term><term>Polarity switches</term><term>Radial velocity</term><term>Representative examples</term><term>Reversal</term><term>Rotation period</term><term>Rotation periods</term><term>Rotational modulation</term><term>Stellar</term><term>Stellar masses</term><term>Stellar sample</term><term>Temporal evolution</term><term>Variability</term><term>Verlag</term><term>Verlag gmbh</term><term>Weinheim</term><term>Wide range</term><term>Zeeman signatures</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Chromospheric</term><term>Chromospheric activity</term><term>Chromospheric emission</term><term>Collier cameron</term><term>Cool stars</term><term>Cycle lengths</term><term>Data reduction</term><term>Data sets</term><term>Different types</term><term>Direct observation</term><term>Donati</term><term>Gmbh</term><term>Instrumental setup</term><term>Kgaa</term><term>Magnetic activity</term><term>Magnetic cycles</term><term>Magnetic geometry</term><term>Magnetic maps</term><term>Magnetic variability</term><term>Magnetic vector</term><term>Mnras</term><term>Narval</term><term>Narval spectropolarimeter</term><term>Online colour</term><term>Polarity reversals</term><term>Polarity switches</term><term>Radial velocity</term><term>Representative examples</term><term>Reversal</term><term>Rotation period</term><term>Rotation periods</term><term>Rotational modulation</term><term>Stellar</term><term>Stellar masses</term><term>Stellar sample</term><term>Temporal evolution</term><term>Variability</term><term>Verlag</term><term>Verlag gmbh</term><term>Weinheim</term><term>Wide range</term><term>Zeeman signatures</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">A sample of 19 solar‐type stars, probing masses between 0.6 and 1.4 solar masses and rotation periods between 3.4 and 43 days, was regularly observed using the NARVAL spectropolarimeter at Telescope Bernard Lyot (Pic du Midi, France) between 2007 and 2011. The Zeeman‐Doppler Imaging technique is employed to reconstruct the large‐scale photospheric magnetic field structure of the targets and investigate its long‐term temporal evolution. We present here the first results of this project with the observation of short magnetic cycles in several stars, showing up a succession of polarity reversals over the timespan of our monitoring. Preliminary trends suggest that short cycles are more frequent for stellar periods below a dozen days and for stellar masses above about one solar mass. The cycles lengths unveiled by the direct tracking of polarity switches are significantly shorter than those derived from previous studies based on chromospheric activity monitoring, suggesting the coexistence of several magnetic timescales in a same star (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>chromospheric</json:string><json:string>donati</json:string><json:string>mnras</json:string><json:string>weinheim</json:string><json:string>kgaa</json:string><json:string>verlag gmbh</json:string><json:string>verlag</json:string><json:string>narval</json:string><json:string>gmbh</json:string><json:string>magnetic cycles</json:string><json:string>online colour</json:string><json:string>polarity reversals</json:string><json:string>data sets</json:string><json:string>stellar</json:string><json:string>magnetic maps</json:string><json:string>chromospheric emission</json:string><json:string>direct observation</json:string><json:string>rotation period</json:string><json:string>zeeman signatures</json:string><json:string>magnetic activity</json:string><json:string>instrumental setup</json:string><json:string>rotation periods</json:string><json:string>stellar masses</json:string><json:string>magnetic variability</json:string><json:string>data reduction</json:string><json:string>wide range</json:string><json:string>representative examples</json:string><json:string>different types</json:string><json:string>collier cameron</json:string><json:string>cool stars</json:string><json:string>polarity switches</json:string><json:string>magnetic vector</json:string><json:string>chromospheric activity</json:string><json:string>rotational modulation</json:string><json:string>radial velocity</json:string><json:string>stellar sample</json:string><json:string>temporal evolution</json:string><json:string>narval spectropolarimeter</json:string><json:string>magnetic geometry</json:string><json:string>cycle lengths</json:string><json:string>variability</json:string><json:string>reversal</json:string></teeft></keywords><author><json:item><name>A. Morgenthaler</name><affiliations><json:string>Université de Toulouse, UPS‐OMP, Institut de Recherche en Astrophysique et Planétologie, Toulouse, France</json:string><json:string>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 Avenue Edouard Belin, F‐31400, Toulouse, France</json:string><json:string>E-mail: amorgent@ast.obs‐mip.fr</json:string><json:string>Correspondence address: Université de Toulouse, UPS‐OMP, Institut de Recherche en Astrophysique et Planétologie, Toulouse, France</json:string></affiliations></json:item><json:item><name>P. Petit</name><affiliations><json:string>Université de Toulouse, UPS‐OMP, Institut de Recherche en Astrophysique et Planétologie, Toulouse, France</json:string><json:string>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 Avenue Edouard Belin, F‐31400, Toulouse, France</json:string></affiliations></json:item><json:item><name>J. Morin</name><affiliations><json:string>Dublin Institute for Advanced Studies, School of Cosmic Physics, 31 Fitzwilliam Place, Dublin 2, Ireland</json:string></affiliations></json:item><json:item><name>M. Aurière</name><affiliations><json:string>Université de Toulouse, UPS‐OMP, Institut de Recherche en Astrophysique et Planétologie, Toulouse, France</json:string><json:string>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 Avenue Edouard Belin, F‐31400, Toulouse, France</json:string></affiliations></json:item><json:item><name>B. Dintrans</name><affiliations><json:string>Université de Toulouse, UPS‐OMP, Institut de Recherche en Astrophysique et Planétologie, Toulouse, France</json:string><json:string>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 Avenue Edouard Belin, F‐31400, Toulouse, France</json:string></affiliations></json:item><json:item><name>R. Konstantinova‐Antova</name><affiliations><json:string>Institute of Astronomy, Bulgarian Academy of Sciences, 72 Tsarigradsko shose, 1784 Sofia, Bulgaria</json:string></affiliations></json:item><json:item><name>S. Marsden</name><affiliations><json:string>Centre for Astronomy, School of Engineering and Physical Sciences, James Cook University, Townsville 4811, Australia</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>stars: magnetic fields</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: activity</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: rotation</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>techniques: polarimetric</value></json:item></subject><articleId><json:string>ASNA201111592</json:string></articleId><arkIstex>ark:/67375/WNG-6ZZQ1SKL-5</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>editorial</json:string></originalGenre><abstract>A sample of 19 solar‐type stars, probing masses between 0.6 and 1.4 solar masses and rotation periods between 3.4 and 43 days, was regularly observed using the NARVAL spectropolarimeter at Telescope Bernard Lyot (Pic du Midi, France) between 2007 and 2011. The Zeeman‐Doppler Imaging technique is employed to reconstruct the large‐scale photospheric magnetic field structure of the targets and investigate its long‐term temporal evolution. We present here the first results of this project with the observation of short magnetic cycles in several stars, showing up a succession of polarity reversals over the timespan of our monitoring. Preliminary trends suggest that short cycles are more frequent for stellar periods below a dozen days and for stellar masses above about one solar mass. The cycles lengths unveiled by the direct tracking of polarity switches are significantly shorter than those derived from previous studies based on chromospheric activity monitoring, suggesting the coexistence of several magnetic timescales in a same star (© 2011 WILEY‐VCH Verlag GmbH & Co. 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(2005)</json:string><json:string>Donati et al. 2003</json:string><json:string>Baliunas et al. 1995</json:string><json:string>Wright et al. (2004)</json:string><json:string>Brown et al. 2011</json:string><json:string>Fares et al. 2009</json:string><json:string>A. Morgenthaler et al.</json:string><json:string>Morgenthaler et al.</json:string><json:string>Ghizaru et al. 2010</json:string><json:string>Donati & Brown 1997</json:string><json:string>Duncan et al. (1991)</json:string><json:string>Donati et al. 2006</json:string><json:string>Petit et al. 2009</json:string><json:string>Wilson 1978</json:string><json:string>Petit et al. 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The Zeeman‐Doppler Imaging technique is employed to reconstruct the large‐scale photospheric magnetic field structure of the targets and investigate its long‐term temporal evolution. We present here the first results of this project with the observation of short magnetic cycles in several stars, showing up a succession of polarity reversals over the timespan of our monitoring. Preliminary trends suggest that short cycles are more frequent for stellar periods below a dozen days and for stellar masses above about one solar mass. The cycles lengths unveiled by the direct tracking of polarity switches are significantly shorter than those derived from previous studies based on chromospheric activity monitoring, suggesting the coexistence of several magnetic timescales in a same star (© 2011 WILEY‐VCH Verlag GmbH & Co. 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