A search for solar-like oscillations in K giants in the globular cluster M 4
Identifieur interne : 003882 ( PascalFrancis/Corpus ); précédent : 003881; suivant : 003883A search for solar-like oscillations in K giants in the globular cluster M 4
Auteurs : S. Frandsen ; H. Bruntt ; F. Grundah ; G. Kopacki ; H. Kjeldsen ; T. Arentoft ; D. Stello ; T. R. Bedding ; A. P. Jacob ; R. L. Gilliland ; P. D. Edmonds ; E. Michel ; J. MatthiesenSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2007.
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Abstract
Context. To expand the range in the colour-magnitude diagram where asteroseismology can be applied, we organized a photometry campaign to find evidence for solar-like oscillations in giant stars in the globular cluster M 4. Aims. The aim was to detect the comb-like p-mode structure characteristic for solar-like oscillations in the amplitude spectra. The 24 main target stars are in the region of the bump stars and have luminosities in the range 50-140 L◦.. Methods. We collected 6160 CCD frames and light curves for about 14000 stars were extracted. The frames consist of exposures in the Johnson B, V and R bands and were obtained at three different telescopes. Three different software packages were applied to obtain the lowest possible photometric noise level. The resulting light curves have been analysed for signatures of oscillations using a variety of methods. Results. We obtain high quality light curves for the K giants, but no clear oscillation signal is detected. This is a surprise as the noise levels achieved in the amplitude spectra should permit oscillations to be seen at the levels predicted by extrapolating from stars at lower luminosities. In particular, when we search for the signature of oscillations in a large number of stars we might expect to see common features in the power spectra, but even here we fall short of having clear evidence of oscillations. Conclusions. High precision differential photometry is possible even in very crowded regions like the core of M4. Solar-like oscillations are probably present in K giants, but the amplitudes are lower than classical scaling laws predict. The reasons may be that the lifetime of the modes are short or the driving mechanism is relatively inefficient in giant stars.
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| NO : | PASCAL 07-0537931 INIST |
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| ET : | A search for solar-like oscillations in K giants in the globular cluster M 4 |
| AU : | FRANDSEN (S.); BRUNTT (H.); GRUNDAH (F.); KOPACKI (G.); KJELDSEN (H.); ARENTOFT (T.); STELLO (D.); BEDDING (T. R.); JACOB (A. P.); GILLILAND (R. L.); EDMONDS (P. D.); MICHEL (E.); MATTHIESEN (J.) |
| AF : | Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520/8000 Aarhus/Danemark (1 aut., 2 aut., 3 aut., 5 aut., 6 aut., 13 aut.); School of Physics A28, University of Sydney/2006 NSW/Australie (2 aut., 7 aut., 8 aut., 9 aut.); Danish AsteroSeismology Center (DASC), University of Aarhus/8000 Aarhus/Danemark (3 aut., 5 aut., 6 aut.); Institute of Astronomy, University of Wroclaw/Pologne (4 aut.); Space Telescope Science Institute/Baltimore/Etats-Unis (10 aut.); Center for Astrophysics/Cambridge, MA/Etats-Unis (11 aut.); Observatoire de Paris/Meudon/France (12 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2007; Vol. 475; No. 3; Pp. 991-1002; Bibl. 1/2 p. |
| LA : | Anglais |
| EA : | Context. To expand the range in the colour-magnitude diagram where asteroseismology can be applied, we organized a photometry campaign to find evidence for solar-like oscillations in giant stars in the globular cluster M 4. Aims. The aim was to detect the comb-like p-mode structure characteristic for solar-like oscillations in the amplitude spectra. The 24 main target stars are in the region of the bump stars and have luminosities in the range 50-140 L◦.. Methods. We collected 6160 CCD frames and light curves for about 14000 stars were extracted. The frames consist of exposures in the Johnson B, V and R bands and were obtained at three different telescopes. Three different software packages were applied to obtain the lowest possible photometric noise level. The resulting light curves have been analysed for signatures of oscillations using a variety of methods. Results. We obtain high quality light curves for the K giants, but no clear oscillation signal is detected. This is a surprise as the noise levels achieved in the amplitude spectra should permit oscillations to be seen at the levels predicted by extrapolating from stars at lower luminosities. In particular, when we search for the signature of oscillations in a large number of stars we might expect to see common features in the power spectra, but even here we fall short of having clear evidence of oscillations. Conclusions. High precision differential photometry is possible even in very crowded regions like the core of M4. Solar-like oscillations are probably present in K giants, but the amplitudes are lower than classical scaling laws predict. The reasons may be that the lifetime of the modes are short or the driving mechanism is relatively inefficient in giant stars. |
| CC : | 001E03 |
| FD : | Amas globulaire; Diagramme magnitude couleur; Astéroséismologie; Photométrie; Etoile géante; Mode p; Spectre amplitude; Luminosité; Courbe lumière; Spectre puissance; Loi échelle; Durée vie; Activité stellaire; Evolution stellaire; Amas stellaire |
| ED : | Globular clusters; Color-magnitude diagrams; Astroseismology; Photometry; Giant stars; p mode; Amplitude spectrum; Luminosity; Light curves; Power spectra; Scaling laws; Lifetime; Stellar activity; Stellar evolution; Star clusters |
| SD : | Modo p; Espectro amplitud |
| LO : | INIST-14176.354000174235840230 |
| ID : | 07-0537931 |
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Arentoft</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="03"><s1>Danish AsteroSeismology Center (DASC), University of Aarhus</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation><inist:fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name><affiliation><inist:fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jacob, A P" sort="Jacob, A P" uniqKey="Jacob A" first="A. P." last="Jacob">A. P. Jacob</name><affiliation><inist:fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilliland, R L" sort="Gilliland, R L" uniqKey="Gilliland R" first="R. L." last="Gilliland">R. L. Gilliland</name><affiliation><inist:fA14 i1="05"><s1>Space Telescope Science Institute</s1><s2>Baltimore</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Edmonds, P D" sort="Edmonds, P D" uniqKey="Edmonds P" first="P. D." last="Edmonds">P. D. Edmonds</name><affiliation><inist:fA14 i1="06"><s1>Center for Astrophysics</s1><s2>Cambridge, MA</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Michel, E" sort="Michel, E" uniqKey="Michel E" first="E." last="Michel">E. Michel</name><affiliation><inist:fA14 i1="07"><s1>Observatoire de Paris</s1><s2>Meudon</s2><s3>FRA</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Matthiesen, J" sort="Matthiesen, J" uniqKey="Matthiesen J" first="J." last="Matthiesen">J. Matthiesen</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">07-0537931</idno><date when="2007">2007</date><idno type="stanalyst">PASCAL 07-0537931 INIST</idno><idno type="RBID">Pascal:07-0537931</idno><idno type="wicri:Area/PascalFrancis/Corpus">003882</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">A search for solar-like oscillations in K giants in the globular cluster M 4</title><author><name sortKey="Frandsen, S" sort="Frandsen, S" uniqKey="Frandsen S" first="S." last="Frandsen">S. Frandsen</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bruntt, H" sort="Bruntt, H" uniqKey="Bruntt H" first="H." last="Bruntt">H. Bruntt</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Grundah, F" sort="Grundah, F" uniqKey="Grundah F" first="F." last="Grundah">F. Grundah</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="03"><s1>Danish AsteroSeismology Center (DASC), University of Aarhus</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kopacki, G" sort="Kopacki, G" uniqKey="Kopacki G" first="G." last="Kopacki">G. Kopacki</name><affiliation><inist:fA14 i1="04"><s1>Institute of Astronomy, University of Wroclaw</s1><s3>POL</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="03"><s1>Danish AsteroSeismology Center (DASC), University of Aarhus</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Arentoft, T" sort="Arentoft, T" uniqKey="Arentoft T" first="T." last="Arentoft">T. Arentoft</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="03"><s1>Danish AsteroSeismology Center (DASC), University of Aarhus</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation><inist:fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name><affiliation><inist:fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jacob, A P" sort="Jacob, A P" uniqKey="Jacob A" first="A. P." last="Jacob">A. P. Jacob</name><affiliation><inist:fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilliland, R L" sort="Gilliland, R L" uniqKey="Gilliland R" first="R. L." last="Gilliland">R. L. Gilliland</name><affiliation><inist:fA14 i1="05"><s1>Space Telescope Science Institute</s1><s2>Baltimore</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Edmonds, P D" sort="Edmonds, P D" uniqKey="Edmonds P" first="P. D." last="Edmonds">P. D. Edmonds</name><affiliation><inist:fA14 i1="06"><s1>Center for Astrophysics</s1><s2>Cambridge, MA</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Michel, E" sort="Michel, E" uniqKey="Michel E" first="E." last="Michel">E. Michel</name><affiliation><inist:fA14 i1="07"><s1>Observatoire de Paris</s1><s2>Meudon</s2><s3>FRA</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Matthiesen, J" sort="Matthiesen, J" uniqKey="Matthiesen J" first="J." last="Matthiesen">J. Matthiesen</name><affiliation><inist:fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2007">2007</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Amplitude spectrum</term><term>Astroseismology</term><term>Color-magnitude diagrams</term><term>Giant stars</term><term>Globular clusters</term><term>Lifetime</term><term>Light curves</term><term>Luminosity</term><term>Photometry</term><term>Power spectra</term><term>Scaling laws</term><term>Star clusters</term><term>Stellar activity</term><term>Stellar evolution</term><term>p mode</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Amas globulaire</term><term>Diagramme magnitude couleur</term><term>Astéroséismologie</term><term>Photométrie</term><term>Etoile géante</term><term>Mode p</term><term>Spectre amplitude</term><term>Luminosité</term><term>Courbe lumière</term><term>Spectre puissance</term><term>Loi échelle</term><term>Durée vie</term><term>Activité stellaire</term><term>Evolution stellaire</term><term>Amas stellaire</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. To expand the range in the colour-magnitude diagram where asteroseismology can be applied, we organized a photometry campaign to find evidence for solar-like oscillations in giant stars in the globular cluster M 4. Aims. The aim was to detect the comb-like p-mode structure characteristic for solar-like oscillations in the amplitude spectra. The 24 main target stars are in the region of the bump stars and have luminosities in the range 50-140 L<sub>◦.</sub>. Methods. We collected 6160 CCD frames and light curves for about 14000 stars were extracted. The frames consist of exposures in the Johnson B, V and R bands and were obtained at three different telescopes. Three different software packages were applied to obtain the lowest possible photometric noise level. The resulting light curves have been analysed for signatures of oscillations using a variety of methods. Results. We obtain high quality light curves for the K giants, but no clear oscillation signal is detected. This is a surprise as the noise levels achieved in the amplitude spectra should permit oscillations to be seen at the levels predicted by extrapolating from stars at lower luminosities. In particular, when we search for the signature of oscillations in a large number of stars we might expect to see common features in the power spectra, but even here we fall short of having clear evidence of oscillations. Conclusions. High precision differential photometry is possible even in very crowded regions like the core of M4. Solar-like oscillations are probably present in K giants, but the amplitudes are lower than classical scaling laws predict. The reasons may be that the lifetime of the modes are short or the driving mechanism is relatively inefficient in giant stars.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>475</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>A search for solar-like oscillations in K giants in the globular cluster M 4</s1></fA08><fA11 i1="01" i2="1"><s1>FRANDSEN (S.)</s1></fA11><fA11 i1="02" i2="1"><s1>BRUNTT (H.)</s1></fA11><fA11 i1="03" i2="1"><s1>GRUNDAH (F.)</s1></fA11><fA11 i1="04" i2="1"><s1>KOPACKI (G.)</s1></fA11><fA11 i1="05" i2="1"><s1>KJELDSEN (H.)</s1></fA11><fA11 i1="06" i2="1"><s1>ARENTOFT (T.)</s1></fA11><fA11 i1="07" i2="1"><s1>STELLO (D.)</s1></fA11><fA11 i1="08" i2="1"><s1>BEDDING (T. R.)</s1></fA11><fA11 i1="09" i2="1"><s1>JACOB (A. P.)</s1></fA11><fA11 i1="10" i2="1"><s1>GILLILAND (R. L.)</s1></fA11><fA11 i1="11" i2="1"><s1>EDMONDS (P. D.)</s1></fA11><fA11 i1="12" i2="1"><s1>MICHEL (E.)</s1></fA11><fA11 i1="13" i2="1"><s1>MATTHIESEN (J.)</s1></fA11><fA14 i1="01"><s1>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="02"><s1>School of Physics A28, University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="03"><s1>Danish AsteroSeismology Center (DASC), University of Aarhus</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></fA14><fA14 i1="04"><s1>Institute of Astronomy, University of Wroclaw</s1><s3>POL</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Space Telescope Science Institute</s1><s2>Baltimore</s2><s3>USA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="06"><s1>Center for Astrophysics</s1><s2>Cambridge, MA</s2><s3>USA</s3><sZ>11 aut.</sZ></fA14><fA14 i1="07"><s1>Observatoire de Paris</s1><s2>Meudon</s2><s3>FRA</s3><sZ>12 aut.</sZ></fA14><fA20><s1>991-1002</s1></fA20><fA21><s1>2007</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000174235840230</s5></fA43><fA44><s0>0000</s0><s1>© 2007 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>07-0537931</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>Context. To expand the range in the colour-magnitude diagram where asteroseismology can be applied, we organized a photometry campaign to find evidence for solar-like oscillations in giant stars in the globular cluster M 4. Aims. The aim was to detect the comb-like p-mode structure characteristic for solar-like oscillations in the amplitude spectra. The 24 main target stars are in the region of the bump stars and have luminosities in the range 50-140 L<sub>◦.</sub>. Methods. We collected 6160 CCD frames and light curves for about 14000 stars were extracted. The frames consist of exposures in the Johnson B, V and R bands and were obtained at three different telescopes. Three different software packages were applied to obtain the lowest possible photometric noise level. The resulting light curves have been analysed for signatures of oscillations using a variety of methods. Results. We obtain high quality light curves for the K giants, but no clear oscillation signal is detected. This is a surprise as the noise levels achieved in the amplitude spectra should permit oscillations to be seen at the levels predicted by extrapolating from stars at lower luminosities. In particular, when we search for the signature of oscillations in a large number of stars we might expect to see common features in the power spectra, but even here we fall short of having clear evidence of oscillations. Conclusions. High precision differential photometry is possible even in very crowded regions like the core of M4. Solar-like oscillations are probably present in K giants, but the amplitudes are lower than classical scaling laws predict. The reasons may be that the lifetime of the modes are short or the driving mechanism is relatively inefficient in giant stars.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Amas globulaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Globular clusters</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Diagramme magnitude couleur</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Color-magnitude diagrams</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Astéroséismologie</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Astroseismology</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Photométrie</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Photometry</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Etoile géante</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Giant stars</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Mode p</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>p mode</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Modo p</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Spectre amplitude</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Amplitude spectrum</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Espectro amplitud</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Luminosité</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Luminosity</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Courbe lumière</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Light curves</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Spectre puissance</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Power spectra</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Loi échelle</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Scaling laws</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Durée vie</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Lifetime</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Activité stellaire</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Stellar activity</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Evolution stellaire</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Stellar evolution</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Amas stellaire</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Star clusters</s0><s5>40</s5></fC03><fN21><s1>344</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 07-0537931 INIST</NO><ET>A search for solar-like oscillations in K giants in the globular cluster M 4</ET><AU>FRANDSEN (S.); BRUNTT (H.); GRUNDAH (F.); KOPACKI (G.); KJELDSEN (H.); ARENTOFT (T.); STELLO (D.); BEDDING (T. R.); JACOB (A. P.); GILLILAND (R. L.); EDMONDS (P. D.); MICHEL (E.); MATTHIESEN (J.)</AU><AF>Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Bygn. 520/8000 Aarhus/Danemark (1 aut., 2 aut., 3 aut., 5 aut., 6 aut., 13 aut.); School of Physics A28, University of Sydney/2006 NSW/Australie (2 aut., 7 aut., 8 aut., 9 aut.); Danish AsteroSeismology Center (DASC), University of Aarhus/8000 Aarhus/Danemark (3 aut., 5 aut., 6 aut.); Institute of Astronomy, University of Wroclaw/Pologne (4 aut.); Space Telescope Science Institute/Baltimore/Etats-Unis (10 aut.); Center for Astrophysics/Cambridge, MA/Etats-Unis (11 aut.); Observatoire de Paris/Meudon/France (12 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2007; Vol. 475; No. 3; Pp. 991-1002; Bibl. 1/2 p.</SO><LA>Anglais</LA><EA>Context. To expand the range in the colour-magnitude diagram where asteroseismology can be applied, we organized a photometry campaign to find evidence for solar-like oscillations in giant stars in the globular cluster M 4. Aims. The aim was to detect the comb-like p-mode structure characteristic for solar-like oscillations in the amplitude spectra. The 24 main target stars are in the region of the bump stars and have luminosities in the range 50-140 L<sub>◦.</sub>. Methods. We collected 6160 CCD frames and light curves for about 14000 stars were extracted. The frames consist of exposures in the Johnson B, V and R bands and were obtained at three different telescopes. Three different software packages were applied to obtain the lowest possible photometric noise level. The resulting light curves have been analysed for signatures of oscillations using a variety of methods. Results. We obtain high quality light curves for the K giants, but no clear oscillation signal is detected. This is a surprise as the noise levels achieved in the amplitude spectra should permit oscillations to be seen at the levels predicted by extrapolating from stars at lower luminosities. In particular, when we search for the signature of oscillations in a large number of stars we might expect to see common features in the power spectra, but even here we fall short of having clear evidence of oscillations. Conclusions. High precision differential photometry is possible even in very crowded regions like the core of M4. Solar-like oscillations are probably present in K giants, but the amplitudes are lower than classical scaling laws predict. The reasons may be that the lifetime of the modes are short or the driving mechanism is relatively inefficient in giant stars.</EA><CC>001E03</CC><FD>Amas globulaire; Diagramme magnitude couleur; Astéroséismologie; Photométrie; Etoile géante; Mode p; Spectre amplitude; Luminosité; Courbe lumière; Spectre puissance; Loi échelle; Durée vie; Activité stellaire; Evolution stellaire; Amas stellaire</FD><ED>Globular clusters; Color-magnitude diagrams; Astroseismology; Photometry; Giant stars; p mode; Amplitude spectrum; Luminosity; Light curves; Power spectra; Scaling laws; Lifetime; Stellar activity; Stellar evolution; Star clusters</ED><SD>Modo p; Espectro amplitud</SD><LO>INIST-14176.354000174235840230</LO><ID>07-0537931</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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