Surface magnetic fields on two accreting T Tauri stars: CV Cha and CR Cha
Identifieur interne : 002230 ( Istex/Curation ); précédent : 002229; suivant : 002231Surface magnetic fields on two accreting T Tauri stars: CV Cha and CR Cha
Auteurs : G. A. J. Hussain [Allemagne] ; A. Collier Cameron ; M. M. Jardine ; N. Dunstone ; J. Ramirez Velez [France] ; H. C. Stempels ; J. Donati [France] ; M. Semel [France] ; G. Aulanier [France] ; T. Harries ; J. Bouvier [France] ; C. Dougados [France] ; J. Ferreira [France] ; B. D. Carter [Australie] ; W. A. Lawson [Australie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009-09-01.
English descriptors
- KwdEn :
- Accreting, Accretion, Accretion diagnostics, Accretion funnels, Accretion state, Accretion states, Active stars, April, Ardila basri, Azimuthal, Balmer line, Blueshifted component, Blueshifted emission, Bootstrap analysis, Brightness maps, Cambridge univ, Cameron, Cent linewidths, Circularly, Circumstellar discs, Collier, Collier cameron, Collier cameron unruh, Complex modes, Complex multipolar, Convective, Convective ctts, Convective stars, Cool stars, Corotation radius, Ctts, Ctts systems, Diagnostics, Donati, Donati collier cameron, Doppler, Doppler images, Doppler imaging, Eld, Equal strength, Evolutionary status, Further details, Further evidence, Future studies, Gauvin strom, Hussain, Image reconstructions, Imaging, Interstellar absorption, Journal compilation, Last night, Line depths, Line list, Line mask, Lling factors, Longitude, Magnetic structure, Magnetospheric accretion models, Map, Maps show, Mnras, Molecular cloud, More details, Other ctts, Other hand, Palla stahler, Phase coverage, Photospheric, Photospheric line, Photospheric lines, Piskunov, Poor phase coverage, Radiative, Radiative core, Radiative cores, Radiative ctts, Reiners basri, Similar level, Small radiative core, Solid lines, Spatial resolution, Spot coverage, Spot groups, Spot patterns, Stellar, Stellar parameters, Stellar surface, Stellar systems, Stempels, Stempels piskunov, Stokes, Subsequent analysis, Tauri, Tauri star systems, Tauri stars, Unruh, Variance, Veiling, Veiling levels, Veiling measurements.
- Teeft :
- Accreting, Accretion, Accretion diagnostics, Accretion funnels, Accretion state, Accretion states, Active stars, April, Ardila basri, Azimuthal, Balmer line, Blueshifted component, Blueshifted emission, Bootstrap analysis, Brightness maps, Cambridge univ, Cameron, Cent linewidths, Circularly, Circumstellar discs, Collier, Collier cameron, Collier cameron unruh, Complex modes, Complex multipolar, Convective, Convective ctts, Convective stars, Cool stars, Corotation radius, Ctts, Ctts systems, Diagnostics, Donati, Donati collier cameron, Doppler, Doppler images, Doppler imaging, Eld, Equal strength, Evolutionary status, Further details, Further evidence, Future studies, Gauvin strom, Hussain, Image reconstructions, Imaging, Interstellar absorption, Journal compilation, Last night, Line depths, Line list, Line mask, Lling factors, Longitude, Magnetic structure, Magnetospheric accretion models, Map, Maps show, Mnras, Molecular cloud, More details, Other ctts, Other hand, Palla stahler, Phase coverage, Photospheric, Photospheric line, Photospheric lines, Piskunov, Poor phase coverage, Radiative, Radiative core, Radiative cores, Radiative ctts, Reiners basri, Similar level, Small radiative core, Solid lines, Spatial resolution, Spot coverage, Spot groups, Spot patterns, Stellar, Stellar parameters, Stellar surface, Stellar systems, Stempels, Stempels piskunov, Stokes, Subsequent analysis, Tauri, Tauri star systems, Tauri stars, Unruh, Variance, Veiling, Veiling levels, Veiling measurements.
Abstract
We have produced brightness and magnetic field maps of the surfaces of CV Cha and CR Cha: two actively accreting G‐ and K‐type T Tauri stars in the Chamaeleon I star‐forming cloud with ages of 3–5 Myr. Our magnetic field maps show evidence for strong, complex multipolar fields similar to those obtained for young rapidly rotating main‐sequence stars. Brightness maps indicate the presence of dark polar caps and low‐latitude spots – these brightness maps are very similar to those obtained for other pre‐main‐sequence and rapidly rotating main‐sequence stars. Only two other classical T Tauri stars have been studied using similar techniques so far: V2129 Oph and BP Tau. CV Cha and CR Cha show magnetic field patterns that are significantly more complex than those recovered for BP Tau, a fully convective T Tauri star. We discuss possible reasons for this difference and suggest that the complexity of the stellar magnetic field is related to the convection zone; with more complex fields being found in T Tauri stars with radiative cores (V2129 Oph, CV Cha and CR Cha). However, it is clearly necessary to conduct magnetic field studies of T Tauri star systems, exploring a wide range of stellar parameters in order to establish how they affect magnetic field generation, and thus how these magnetic fields are likely to affect the evolution of T Tauri star systems as they approach the main sequence.
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DOI: 10.1111/j.1365-2966.2009.14881.x
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A. Collier Cameron<affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation><affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation><affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation><affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation><affiliation><mods:affiliation>School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL</mods:affiliation><wicri:noCountry code="subField">4QL</wicri:noCountry></affiliation>Le document en format XML
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Lawson</name><affiliation wicri:level="1"><mods:affiliation>School of Physical, Environmental and Mathematical Sciences, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>School of Physical, Environmental and Mathematical Sciences, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600</wicri:regionArea></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:B4AB78937BE6BC0C3A79CA3C77770EDD0B166606</idno><date when="2009" year="2009">2009</date><idno type="doi">10.1111/j.1365-2966.2009.14881.x</idno><idno type="url">https://api.istex.fr/document/B4AB78937BE6BC0C3A79CA3C77770EDD0B166606/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">002230</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">002230</idno><idno type="wicri:Area/Istex/Curation">002230</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">Surface magnetic fields on two accreting T Tauri stars: CV Cha and CR Cha</title><author><name sortKey="Hussain, G A J" sort="Hussain, G A J" uniqKey="Hussain G" first="G. A. J." last="Hussain">G. A. J. Hussain</name><affiliation wicri:level="1"><mods:affiliation>ESO, Karl‐Schwarzschild‐Strasse 2, 85748 Garching bei München, Germany</mods:affiliation><country xml:lang="fr">Allemagne</country><wicri:regionArea>ESO, Karl‐Schwarzschild‐Strasse 2, 85748 Garching bei München</wicri:regionArea></affiliation><affiliation><mods:affiliation>E-mail: ghussain@eso.org</mods:affiliation></affiliation></author><author><name sortKey="Collier Cameron, A" sort="Collier Cameron, A" uniqKey="Collier Cameron A" first="A." last="Collier Cameron">A. Collier Cameron</name><affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation></author><author><name sortKey="Jardine, M M" sort="Jardine, M M" uniqKey="Jardine M" first="M. M." last="Jardine">M. M. Jardine</name><affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation></author><author><name sortKey="Dunstone, N" sort="Dunstone, N" uniqKey="Dunstone N" first="N." last="Dunstone">N. Dunstone</name><affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation></author><author><name sortKey="Velez, J Ramirez" sort="Velez, J Ramirez" uniqKey="Velez J" first="J. Ramirez" last="Velez">J. Ramirez Velez</name><affiliation wicri:level="1"><mods:affiliation>LESIA, Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>LESIA, Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex</wicri:regionArea></affiliation></author><author><name sortKey="Stempels, H C" sort="Stempels, H C" uniqKey="Stempels H" first="H. C." last="Stempels">H. C. Stempels</name><affiliation><mods:affiliation>SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation></author><author><name sortKey="Donati, J" sort="Donati, J" uniqKey="Donati J" first="J." last="Donati">J. Donati</name><affiliation wicri:level="1"><mods:affiliation>LATT, CNRS‐UMR 5572, Obs. Midi‐Pyrénées, 14 Av. E. Belin, F‐31400 Toulouse, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>LATT, CNRS‐UMR 5572, Obs. Midi‐Pyrénées, 14 Av. E. Belin, F‐31400 Toulouse</wicri:regionArea></affiliation></author><author><name sortKey="Semel, M" sort="Semel, M" uniqKey="Semel M" first="M." last="Semel">M. Semel</name><affiliation wicri:level="1"><mods:affiliation>LESIA, Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>LESIA, Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex</wicri:regionArea></affiliation></author><author><name sortKey="Aulanier, G" sort="Aulanier, G" uniqKey="Aulanier G" first="G." last="Aulanier">G. Aulanier</name><affiliation wicri:level="1"><mods:affiliation>LESIA, Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>LESIA, Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex</wicri:regionArea></affiliation></author><author><name sortKey="Harries, T" sort="Harries, T" uniqKey="Harries T" first="T." last="Harries">T. Harries</name><affiliation><mods:affiliation>School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL</mods:affiliation><wicri:noCountry code="subField">4QL</wicri:noCountry></affiliation></author><author><name sortKey="Bouvier, J" sort="Bouvier, J" uniqKey="Bouvier J" first="J." last="Bouvier">J. Bouvier</name><affiliation wicri:level="1"><mods:affiliation>LAOG, Laboratoire d'Astrophysique, Obs. de Grenoble, UMR‐5571, CNRS, Univ. J Fourier, F‐38041 Grenoble, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>LAOG, Laboratoire d'Astrophysique, Obs. de Grenoble, UMR‐5571, CNRS, Univ. J Fourier, F‐38041 Grenoble</wicri:regionArea></affiliation></author><author><name sortKey="Dougados, C" sort="Dougados, C" uniqKey="Dougados C" first="C." last="Dougados">C. Dougados</name><affiliation wicri:level="1"><mods:affiliation>LAOG, Laboratoire d'Astrophysique, Obs. de Grenoble, UMR‐5571, CNRS, Univ. J Fourier, F‐38041 Grenoble, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>LAOG, Laboratoire d'Astrophysique, Obs. de Grenoble, UMR‐5571, CNRS, Univ. J Fourier, F‐38041 Grenoble</wicri:regionArea></affiliation></author><author><name sortKey="Ferreira, J" sort="Ferreira, J" uniqKey="Ferreira J" first="J." last="Ferreira">J. Ferreira</name><affiliation wicri:level="1"><mods:affiliation>LAOG, Laboratoire d'Astrophysique, Obs. de Grenoble, UMR‐5571, CNRS, Univ. J Fourier, F‐38041 Grenoble, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>LAOG, Laboratoire d'Astrophysique, Obs. de Grenoble, UMR‐5571, CNRS, Univ. J Fourier, F‐38041 Grenoble</wicri:regionArea></affiliation></author><author><name sortKey="Carter, B D" sort="Carter, B D" uniqKey="Carter B" first="B. D." last="Carter">B. D. Carter</name><affiliation wicri:level="1"><mods:affiliation>Faculty of Sciences, University of Southern Queensland, Toowoomba 4350, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Faculty of Sciences, University of Southern Queensland, Toowoomba 4350</wicri:regionArea></affiliation></author><author><name sortKey="Lawson, W A" sort="Lawson, W A" uniqKey="Lawson W" first="W. A." last="Lawson">W. A. Lawson</name><affiliation wicri:level="1"><mods:affiliation>School of Physical, Environmental and Mathematical Sciences, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>School of Physical, Environmental and Mathematical Sciences, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600</wicri:regionArea></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">398</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="189">189</biblScope><biblScope unit="page" to="200">200</biblScope><biblScope unit="page-count">12</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2009-09-01">2009-09-01</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accreting</term><term>Accretion</term><term>Accretion diagnostics</term><term>Accretion funnels</term><term>Accretion state</term><term>Accretion states</term><term>Active stars</term><term>April</term><term>Ardila basri</term><term>Azimuthal</term><term>Balmer line</term><term>Blueshifted component</term><term>Blueshifted emission</term><term>Bootstrap analysis</term><term>Brightness maps</term><term>Cambridge univ</term><term>Cameron</term><term>Cent linewidths</term><term>Circularly</term><term>Circumstellar discs</term><term>Collier</term><term>Collier cameron</term><term>Collier cameron unruh</term><term>Complex modes</term><term>Complex multipolar</term><term>Convective</term><term>Convective ctts</term><term>Convective stars</term><term>Cool stars</term><term>Corotation radius</term><term>Ctts</term><term>Ctts systems</term><term>Diagnostics</term><term>Donati</term><term>Donati collier cameron</term><term>Doppler</term><term>Doppler images</term><term>Doppler imaging</term><term>Eld</term><term>Equal strength</term><term>Evolutionary status</term><term>Further details</term><term>Further evidence</term><term>Future studies</term><term>Gauvin strom</term><term>Hussain</term><term>Image reconstructions</term><term>Imaging</term><term>Interstellar absorption</term><term>Journal compilation</term><term>Last night</term><term>Line depths</term><term>Line list</term><term>Line mask</term><term>Lling factors</term><term>Longitude</term><term>Magnetic structure</term><term>Magnetospheric accretion models</term><term>Map</term><term>Maps show</term><term>Mnras</term><term>Molecular cloud</term><term>More details</term><term>Other ctts</term><term>Other hand</term><term>Palla stahler</term><term>Phase coverage</term><term>Photospheric</term><term>Photospheric line</term><term>Photospheric lines</term><term>Piskunov</term><term>Poor phase coverage</term><term>Radiative</term><term>Radiative core</term><term>Radiative cores</term><term>Radiative ctts</term><term>Reiners basri</term><term>Similar level</term><term>Small radiative core</term><term>Solid lines</term><term>Spatial resolution</term><term>Spot coverage</term><term>Spot groups</term><term>Spot patterns</term><term>Stellar</term><term>Stellar parameters</term><term>Stellar surface</term><term>Stellar systems</term><term>Stempels</term><term>Stempels piskunov</term><term>Stokes</term><term>Subsequent analysis</term><term>Tauri</term><term>Tauri star systems</term><term>Tauri stars</term><term>Unruh</term><term>Variance</term><term>Veiling</term><term>Veiling levels</term><term>Veiling measurements</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Accreting</term><term>Accretion</term><term>Accretion diagnostics</term><term>Accretion funnels</term><term>Accretion state</term><term>Accretion states</term><term>Active stars</term><term>April</term><term>Ardila basri</term><term>Azimuthal</term><term>Balmer line</term><term>Blueshifted component</term><term>Blueshifted emission</term><term>Bootstrap analysis</term><term>Brightness maps</term><term>Cambridge univ</term><term>Cameron</term><term>Cent linewidths</term><term>Circularly</term><term>Circumstellar discs</term><term>Collier</term><term>Collier cameron</term><term>Collier cameron unruh</term><term>Complex modes</term><term>Complex multipolar</term><term>Convective</term><term>Convective ctts</term><term>Convective stars</term><term>Cool stars</term><term>Corotation radius</term><term>Ctts</term><term>Ctts systems</term><term>Diagnostics</term><term>Donati</term><term>Donati collier cameron</term><term>Doppler</term><term>Doppler images</term><term>Doppler imaging</term><term>Eld</term><term>Equal strength</term><term>Evolutionary status</term><term>Further details</term><term>Further evidence</term><term>Future studies</term><term>Gauvin strom</term><term>Hussain</term><term>Image reconstructions</term><term>Imaging</term><term>Interstellar absorption</term><term>Journal compilation</term><term>Last night</term><term>Line depths</term><term>Line list</term><term>Line mask</term><term>Lling factors</term><term>Longitude</term><term>Magnetic structure</term><term>Magnetospheric accretion models</term><term>Map</term><term>Maps show</term><term>Mnras</term><term>Molecular cloud</term><term>More details</term><term>Other ctts</term><term>Other hand</term><term>Palla stahler</term><term>Phase coverage</term><term>Photospheric</term><term>Photospheric line</term><term>Photospheric lines</term><term>Piskunov</term><term>Poor phase coverage</term><term>Radiative</term><term>Radiative core</term><term>Radiative cores</term><term>Radiative ctts</term><term>Reiners basri</term><term>Similar level</term><term>Small radiative core</term><term>Solid lines</term><term>Spatial resolution</term><term>Spot coverage</term><term>Spot groups</term><term>Spot patterns</term><term>Stellar</term><term>Stellar parameters</term><term>Stellar surface</term><term>Stellar systems</term><term>Stempels</term><term>Stempels piskunov</term><term>Stokes</term><term>Subsequent analysis</term><term>Tauri</term><term>Tauri star systems</term><term>Tauri stars</term><term>Unruh</term><term>Variance</term><term>Veiling</term><term>Veiling levels</term><term>Veiling measurements</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have produced brightness and magnetic field maps of the surfaces of CV Cha and CR Cha: two actively accreting G‐ and K‐type T Tauri stars in the Chamaeleon I star‐forming cloud with ages of 3–5 Myr. Our magnetic field maps show evidence for strong, complex multipolar fields similar to those obtained for young rapidly rotating main‐sequence stars. Brightness maps indicate the presence of dark polar caps and low‐latitude spots – these brightness maps are very similar to those obtained for other pre‐main‐sequence and rapidly rotating main‐sequence stars. Only two other classical T Tauri stars have been studied using similar techniques so far: V2129 Oph and BP Tau. CV Cha and CR Cha show magnetic field patterns that are significantly more complex than those recovered for BP Tau, a fully convective T Tauri star. We discuss possible reasons for this difference and suggest that the complexity of the stellar magnetic field is related to the convection zone; with more complex fields being found in T Tauri stars with radiative cores (V2129 Oph, CV Cha and CR Cha). However, it is clearly necessary to conduct magnetic field studies of T Tauri star systems, exploring a wide range of stellar parameters in order to establish how they affect magnetic field generation, and thus how these magnetic fields are likely to affect the evolution of T Tauri star systems as they approach the main sequence.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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