Precise stellar surface gravities from the time scales of convectively driven brightness variations.
Identifieur interne : 002332 ( PubMed/Curation ); précédent : 002331; suivant : 002333Precise stellar surface gravities from the time scales of convectively driven brightness variations.
Auteurs : Thomas Kallinger [Autriche] ; Saskia Hekker [Danemark] ; Rafael A. García [France] ; Daniel Huber [Danemark] ; Jaymie M. Matthews [Canada]Source :
- Science advances [ 2375-2548 ] ; 2016.
Descripteurs français
- KwdFr :
- MESH :
English descriptors
- KwdEn :
- MESH :
- methods : Astronomy.
- Extraterrestrial Environment, Gravitation, Stars, Celestial.
Abstract
A significant part of the intrinsic brightness variations in cool stars of low and intermediate mass arises from surface convection (seen as granulation) and acoustic oscillations (p-mode pulsations). The characteristics of these phenomena are largely determined by the stars' surface gravity (g). Detailed photometric measurements of either signal can yield an accurate value of g. However, even with ultraprecise photometry from NASA's Kepler mission, many stars are too faint for current methods or only moderate accuracy can be achieved in a limited range of stellar evolutionary stages. This means that many of the stars in the Kepler sample, including exoplanet hosts, are not sufficiently characterized to fully describe the sample and exoplanet properties. We present a novel way to measure surface gravities with accuracies of about 4%. Our technique exploits the tight relation between g and the characteristic time scale of the combined granulation and p-mode oscillation signal. It is applicable to all stars with a convective envelope, including active stars. It can measure g in stars for which no other analysis is now possible. Because it depends on the time scale (and no other properties) of the signal, our technique is largely independent of the type of measurement (for example, photometry or radial velocity measurements) and the calibration of the instrumentation used. However, the oscillation signal must be temporally resolved; thus, it cannot be applied to dwarf stars observed by Kepler in its long-cadence mode.
DOI: 10.1126/sciadv.1500654
PubMed: 26767193
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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, Gif-sur-Yvette Cedex 91191, France.</nlm:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Laboratoire AIM, CEA/DSM-CNRS, Université Paris Diderot-IRFU/SAp, Centre de Saclay, Gif-sur-Yvette Cedex 91191</wicri:regionArea></affiliation></author><author><name sortKey="Huber, Daniel" sort="Huber, Daniel" uniqKey="Huber D" first="Daniel" last="Huber">Daniel Huber</name><affiliation wicri:level="1"><nlm:affiliation>Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.; SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA.; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C 8000, Denmark.</nlm:affiliation><country xml:lang="fr">Danemark</country><wicri:regionArea>Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.; SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA.; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C 8000</wicri:regionArea></affiliation></author><author><name sortKey="Matthews, Jaymie M" sort="Matthews, Jaymie M" uniqKey="Matthews J" first="Jaymie M" last="Matthews">Jaymie M. Matthews</name><affiliation wicri:level="1"><nlm:affiliation>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada.</nlm:affiliation><country xml:lang="fr">Canada</country><wicri:regionArea>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1</wicri:regionArea></affiliation></author></analytic><series><title level="j">Science advances</title><idno type="ISSN">2375-2548</idno><imprint><date when="2016" type="published">2016</date></imprint></series></biblStruct></sourceDesc></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Astronomy (methods)</term><term>Extraterrestrial Environment</term><term>Gravitation</term><term>Stars, Celestial</term></keywords><keywords scheme="KwdFr" xml:lang="fr"><term>Astronomie ()</term><term>Environnement extraterrestre</term><term>Gravitation</term><term>Étoiles</term></keywords><keywords scheme="MESH" qualifier="methods" xml:lang="en"><term>Astronomy</term></keywords><keywords scheme="MESH" xml:lang="en"><term>Extraterrestrial Environment</term><term>Gravitation</term><term>Stars, Celestial</term></keywords><keywords scheme="MESH" xml:lang="fr"><term>Astronomie</term><term>Environnement extraterrestre</term><term>Gravitation</term><term>Étoiles</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">A significant part of the intrinsic brightness variations in cool stars of low and intermediate mass arises from surface convection (seen as granulation) and acoustic oscillations (p-mode pulsations). The characteristics of these phenomena are largely determined by the stars' surface gravity (g). Detailed photometric measurements of either signal can yield an accurate value of g. However, even with ultraprecise photometry from NASA's Kepler mission, many stars are too faint for current methods or only moderate accuracy can be achieved in a limited range of stellar evolutionary stages. This means that many of the stars in the Kepler sample, including exoplanet hosts, are not sufficiently characterized to fully describe the sample and exoplanet properties. We present a novel way to measure surface gravities with accuracies of about 4%. Our technique exploits the tight relation between g and the characteristic time scale of the combined granulation and p-mode oscillation signal. It is applicable to all stars with a convective envelope, including active stars. It can measure g in stars for which no other analysis is now possible. Because it depends on the time scale (and no other properties) of the signal, our technique is largely independent of the type of measurement (for example, photometry or radial velocity measurements) and the calibration of the instrumentation used. However, the oscillation signal must be temporally resolved; thus, it cannot be applied to dwarf stars observed by Kepler in its long-cadence mode.</div></front></TEI><pubmed><MedlineCitation Status="MEDLINE" Owner="NLM"><PMID Version="1">26767193</PMID><DateCreated><Year>2016</Year><Month>01</Month><Day>15</Day></DateCreated><DateCompleted><Year>2016</Year><Month>09</Month><Day>12</Day></DateCompleted><DateRevised><Year>2017</Year><Month>02</Month><Day>20</Day></DateRevised><Article PubModel="Electronic-eCollection"><Journal><ISSN IssnType="Print">2375-2548</ISSN><JournalIssue CitedMedium="Print"><Volume>2</Volume><Issue>1</Issue><PubDate><Year>2016</Year><Month>Jan</Month></PubDate></JournalIssue><Title>Science advances</Title><ISOAbbreviation>Sci Adv</ISOAbbreviation></Journal><ArticleTitle>Precise stellar surface gravities from the time scales of convectively driven brightness variations.</ArticleTitle><Pagination><MedlinePgn>e1500654</MedlinePgn></Pagination><ELocationID EIdType="doi" ValidYN="Y">10.1126/sciadv.1500654</ELocationID><Abstract><AbstractText>A significant part of the intrinsic brightness variations in cool stars of low and intermediate mass arises from surface convection (seen as granulation) and acoustic oscillations (p-mode pulsations). The characteristics of these phenomena are largely determined by the stars' surface gravity (g). Detailed photometric measurements of either signal can yield an accurate value of g. However, even with ultraprecise photometry from NASA's Kepler mission, many stars are too faint for current methods or only moderate accuracy can be achieved in a limited range of stellar evolutionary stages. This means that many of the stars in the Kepler sample, including exoplanet hosts, are not sufficiently characterized to fully describe the sample and exoplanet properties. We present a novel way to measure surface gravities with accuracies of about 4%. Our technique exploits the tight relation between g and the characteristic time scale of the combined granulation and p-mode oscillation signal. It is applicable to all stars with a convective envelope, including active stars. It can measure g in stars for which no other analysis is now possible. Because it depends on the time scale (and no other properties) of the signal, our technique is largely independent of the type of measurement (for example, photometry or radial velocity measurements) and the calibration of the instrumentation used. However, the oscillation signal must be temporally resolved; thus, it cannot be applied to dwarf stars observed by Kepler in its long-cadence mode.</AbstractText></Abstract><AuthorList CompleteYN="Y"><Author ValidYN="Y"><LastName>Kallinger</LastName><ForeName>Thomas</ForeName><Initials>T</Initials><AffiliationInfo><Affiliation>Institute of Astrophysics, University of Vienna, Türkenschanzstrasse 17, Vienna 1180, Austria.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Hekker</LastName><ForeName>Saskia</ForeName><Initials>S</Initials><Identifier Source="ORCID">0000-0002-1463-726X</Identifier><AffiliationInfo><Affiliation>Max-Planck-Institute für Sonnensystemforschung, Justus-von-Liebig-Weg 3, Göttingen 37077, Germany.; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C 8000, Denmark.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>García</LastName><ForeName>Rafael A</ForeName><Initials>RA</Initials><Identifier Source="ORCID">0000-0002-8854-3776</Identifier><AffiliationInfo><Affiliation>Laboratoire AIM, CEA/DSM-CNRS, Université Paris Diderot-IRFU/SAp, Centre de Saclay, Gif-sur-Yvette Cedex 91191, France.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Huber</LastName><ForeName>Daniel</ForeName><Initials>D</Initials><AffiliationInfo><Affiliation>Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.; SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA.; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C 8000, Denmark.</Affiliation></AffiliationInfo></Author><Author ValidYN="Y"><LastName>Matthews</LastName><ForeName>Jaymie M</ForeName><Initials>JM</Initials><AffiliationInfo><Affiliation>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada.</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>01</Day></ArticleDate></Article><MedlineJournalInfo><Country>United States</Country><MedlineTA>Sci Adv</MedlineTA><NlmUniqueID>101653440</NlmUniqueID><ISSNLinking>2375-2548</ISSNLinking></MedlineJournalInfo><CitationSubset>IM</CitationSubset><CommentsCorrectionsList><CommentsCorrections RefType="Cites"><RefSource>Science. 2010 Feb 19;327(5968):977-80</RefSource><PMID Version="1">20056856</PMID></CommentsCorrections><CommentsCorrections RefType="Cites"><RefSource>Nature. 2013 Aug 22;500(7463):427-30</RefSource><PMID Version="1">23969460</PMID></CommentsCorrections></CommentsCorrectionsList><MeshHeadingList><MeshHeading><DescriptorName UI="D001256" MajorTopicYN="N">Astronomy</DescriptorName><QualifierName UI="Q000379" MajorTopicYN="Y">methods</QualifierName></MeshHeading><MeshHeading><DescriptorName UI="D005118" MajorTopicYN="N">Extraterrestrial Environment</DescriptorName></MeshHeading><MeshHeading><DescriptorName UI="D006112" MajorTopicYN="Y">Gravitation</DescriptorName></MeshHeading><MeshHeading><DescriptorName UI="D055609" MajorTopicYN="Y">Stars, Celestial</DescriptorName></MeshHeading></MeshHeadingList><OtherID Source="NLM">PMC4705039</OtherID><KeywordList Owner="NOTNLM"><Keyword MajorTopicYN="N">Stars</Keyword><Keyword MajorTopicYN="N">convection</Keyword><Keyword MajorTopicYN="N">granulation</Keyword><Keyword MajorTopicYN="N">stellar fundamental parameters</Keyword><Keyword MajorTopicYN="N">stellar oscillations</Keyword></KeywordList><GeneralNote Owner="NLM">Original DateCompleted: 20160115</GeneralNote></MedlineCitation><PubmedData><History><PubMedPubDate PubStatus="received"><Year>2015</Year><Month>05</Month><Day>21</Day></PubMedPubDate><PubMedPubDate PubStatus="accepted"><Year>2015</Year><Month>11</Month><Day>04</Day></PubMedPubDate><PubMedPubDate PubStatus="entrez"><Year>2016</Year><Month>1</Month><Day>15</Day><Hour>6</Hour><Minute>0</Minute></PubMedPubDate><PubMedPubDate PubStatus="pubmed"><Year>2016</Year><Month>1</Month><Day>15</Day><Hour>6</Hour><Minute>0</Minute></PubMedPubDate><PubMedPubDate PubStatus="medline"><Year>2016</Year><Month>1</Month><Day>15</Day><Hour>6</Hour><Minute>1</Minute></PubMedPubDate></History><PublicationStatus>epublish</PublicationStatus><ArticleIdList><ArticleId IdType="pubmed">26767193</ArticleId><ArticleId IdType="doi">10.1126/sciadv.1500654</ArticleId><ArticleId IdType="pii">1500654</ArticleId><ArticleId IdType="pmc">PMC4705039</ArticleId></ArticleIdList></PubmedData></pubmed></record>Pour manipuler ce document sous Unix (Dilib)
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