A prevalence of dynamo-generated magnetic fields in the cores of intermediate-mass stars.
Identifieur interne : 002340 ( PubMed/Curation ); précédent : 002339; suivant : 002341A prevalence of dynamo-generated magnetic fields in the cores of intermediate-mass stars.
Auteurs : Dennis Stello [Australie] ; Matteo Cantiello [États-Unis] ; Jim Fuller [États-Unis] ; Daniel Huber [Australie] ; Rafael A. García [France] ; Timothy R. Bedding [Australie] ; Lars Bildsten [États-Unis] ; Victor Silva Aguirre [Danemark]Source :
- Nature [ 1476-4687 ] ; 2016.
Abstract
Magnetic fields play a part in almost all stages of stellar evolution. Most low-mass stars, including the Sun, show surface fields that are generated by dynamo processes in their convective envelopes. Intermediate-mass stars do not have deep convective envelopes, although 10 per cent exhibit strong surface fields that are presumed to be residuals from the star formation process. These stars do have convective cores that might produce internal magnetic fields, and these fields might survive into later stages of stellar evolution, but information has been limited by our inability to measure the fields below the stellar surface. Here we report the strength of dipolar oscillation modes for a sample of 3,600 red giant stars. About 20 per cent of our sample show mode suppression, by strong magnetic fields in the cores, but this fraction is a strong function of mass. Strong core fields occur only in red giants heavier than 1.1 solar masses, and the occurrence rate is at least 50 per cent for intermediate-mass stars (1.6-2.0 solar masses), indicating that powerful dynamos were very common in the previously convective cores of these stars.
DOI: 10.1038/nature16171
PubMed: 26727160
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García</name><affiliation wicri:level="1"><nlm:affiliation>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot-IRFU/SAp Centre de Saclay, 91191 Gif-sur-Yvette Cedex, France.</nlm:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot-IRFU/SAp Centre de Saclay, 91191 Gif-sur-Yvette Cedex</wicri:regionArea></affiliation></author><author><name sortKey="Bedding, Timothy R" sort="Bedding, Timothy R" uniqKey="Bedding T" first="Timothy R" last="Bedding">Timothy R. Bedding</name><affiliation wicri:level="1"><nlm:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.</nlm:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, New South Wales 2006</wicri:regionArea></affiliation></author><author><name sortKey="Bildsten, Lars" sort="Bildsten, Lars" uniqKey="Bildsten L" first="Lars" last="Bildsten">Lars Bildsten</name><affiliation wicri:level="1"><nlm:affiliation>Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA.</nlm:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106</wicri:regionArea></affiliation></author><author><name sortKey="Aguirre, Victor Silva" sort="Aguirre, Victor Silva" uniqKey="Aguirre V" first="Victor Silva" last="Aguirre">Victor Silva Aguirre</name><affiliation wicri:level="1"><nlm:affiliation>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.</nlm:affiliation><country xml:lang="fr">Danemark</country><wicri:regionArea>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C</wicri:regionArea></affiliation></author></analytic><series><title level="j">Nature</title><idno type="eISSN">1476-4687</idno><imprint><date when="2016" type="published">2016</date></imprint></series></biblStruct></sourceDesc></fileDesc><profileDesc><textClass></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Magnetic fields play a part in almost all stages of stellar evolution. Most low-mass stars, including the Sun, show surface fields that are generated by dynamo processes in their convective envelopes. Intermediate-mass stars do not have deep convective envelopes, although 10 per cent exhibit strong surface fields that are presumed to be residuals from the star formation process. These stars do have convective cores that might produce internal magnetic fields, and these fields might survive into later stages of stellar evolution, but information has been limited by our inability to measure the fields below the stellar surface. Here we report the strength of dipolar oscillation modes for a sample of 3,600 red giant stars. About 20 per cent of our sample show mode suppression, by strong magnetic fields in the cores, but this fraction is a strong function of mass. Strong core fields occur only in red giants heavier than 1.1 solar masses, and the occurrence rate is at least 50 per cent for intermediate-mass stars (1.6-2.0 solar masses), indicating that powerful dynamos were very common in the previously convective cores of these stars.</div></front></TEI><pubmed><MedlineCitation Status="PubMed-not-MEDLINE" Owner="NLM"><PMID Version="1">26727160</PMID><DateCreated><Year>2016</Year><Month>01</Month><Day>21</Day></DateCreated><DateCompleted><Year>2016</Year><Month>04</Month><Day>28</Day></DateCompleted><DateRevised><Year>2016</Year><Month>01</Month><Day>21</Day></DateRevised><Article PubModel="Print-Electronic"><Journal><ISSN IssnType="Electronic">1476-4687</ISSN><JournalIssue CitedMedium="Internet"><Volume>529</Volume><Issue>7586</Issue><PubDate><Year>2016</Year><Month>Jan</Month><Day>21</Day></PubDate></JournalIssue><Title>Nature</Title><ISOAbbreviation>Nature</ISOAbbreviation></Journal><ArticleTitle>A prevalence of dynamo-generated magnetic fields in the cores of intermediate-mass stars.</ArticleTitle><Pagination><MedlinePgn>364-7</MedlinePgn></Pagination><ELocationID EIdType="doi" ValidYN="Y">10.1038/nature16171</ELocationID><Abstract><AbstractText>Magnetic fields play a part in almost all stages of stellar evolution. Most low-mass stars, including the Sun, show surface fields that are generated by dynamo processes in their convective envelopes. Intermediate-mass stars do not have deep convective envelopes, although 10 per cent exhibit strong surface fields that are presumed to be residuals from the star formation process. These stars do have convective cores that might produce internal magnetic fields, and these fields might survive into later stages of stellar evolution, but information has been limited by our inability to measure the fields below the stellar surface. Here we report the strength of dipolar oscillation modes for a sample of 3,600 red giant stars. About 20 per cent of our sample show mode suppression, by strong magnetic fields in the cores, but this fraction is a strong function of mass. Strong core fields occur only in red giants heavier than 1.1 solar masses, and the occurrence rate is at least 50 per cent for intermediate-mass stars (1.6-2.0 solar masses), indicating that powerful dynamos were very common in the previously convective cores of these stars.</AbstractText></Abstract><AuthorList CompleteYN="Y"><Author ValidYN="Y"><LastName>Stello</LastName><ForeName>Dennis</ForeName><Initials>D</Initials><AffiliationInfo><Affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.</Affiliation></AffiliationInfo><AffiliationInfo><Affiliation>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Cantiello</LastName><ForeName>Matteo</ForeName><Initials>M</Initials><AffiliationInfo><Affiliation>Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Fuller</LastName><ForeName>Jim</ForeName><Initials>J</Initials><AffiliationInfo><Affiliation>Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA.</Affiliation></AffiliationInfo><AffiliationInfo><Affiliation>TAPIR, Walter Burke Institute for Theoretical Physics, Mailcode 350-17, California Institute of Technology, Pasadena, California 91125, USA.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Huber</LastName><ForeName>Daniel</ForeName><Initials>D</Initials><AffiliationInfo><Affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.</Affiliation></AffiliationInfo><AffiliationInfo><Affiliation>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.</Affiliation></AffiliationInfo><AffiliationInfo><Affiliation>SETI Institute, 189 Bernardo Avenue, Mountain View, California 94043, USA.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>García</LastName><ForeName>Rafael A</ForeName><Initials>RA</Initials><AffiliationInfo><Affiliation>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot-IRFU/SAp Centre de Saclay, 91191 Gif-sur-Yvette Cedex, France.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Bedding</LastName><ForeName>Timothy R</ForeName><Initials>TR</Initials><AffiliationInfo><Affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.</Affiliation></AffiliationInfo><AffiliationInfo><Affiliation>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Bildsten</LastName><ForeName>Lars</ForeName><Initials>L</Initials><AffiliationInfo><Affiliation>Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA.</Affiliation></AffiliationInfo><AffiliationInfo><Affiliation>Department of Physics, University of California, Santa Barbara, California 93106, USA.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Aguirre</LastName><ForeName>Victor Silva</ForeName><Initials>VS</Initials><AffiliationInfo><Affiliation>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.</Affiliation></AffiliationInfo></Author></AuthorList><Language>eng</Language><PublicationTypeList><PublicationType UI="D016428">Journal Article</PublicationType><PublicationType UI="D013485">Research Support, Non-U.S. Gov't</PublicationType><PublicationType UI="D013486">Research Support, U.S. Gov't, Non-P.H.S.</PublicationType></PublicationTypeList><ArticleDate DateType="Electronic"><Year>2016</Year><Month>01</Month><Day>04</Day></ArticleDate></Article><MedlineJournalInfo><Country>England</Country><MedlineTA>Nature</MedlineTA><NlmUniqueID>0410462</NlmUniqueID><ISSNLinking>0028-0836</ISSNLinking></MedlineJournalInfo></MedlineCitation><PubmedData><History><PubMedPubDate PubStatus="received"><Year>2015</Year><Month>06</Month><Day>25</Day></PubMedPubDate><PubMedPubDate PubStatus="accepted"><Year>2015</Year><Month>10</Month><Day>15</Day></PubMedPubDate><PubMedPubDate PubStatus="entrez"><Year>2016</Year><Month>1</Month><Day>5</Day><Hour>6</Hour><Minute>0</Minute></PubMedPubDate><PubMedPubDate PubStatus="pubmed"><Year>2016</Year><Month>1</Month><Day>5</Day><Hour>6</Hour><Minute>0</Minute></PubMedPubDate><PubMedPubDate 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