Oscillations in Procyon A First results from a multi-site campaign

被引：2

作者：

Hekker, S. ^{[1
]}

Arentoft, T. ^{[2
]}

Kjeldsen, H. ^{[2
]}

Bedding, T. R. ^{[3
]}

Christensen-Dalsgaard, J. ^{[2
]}

Reffert, S. ^{[4
]}

Bruntt, H. ^{[3
]}

Butler, R. P. ^{[5
]}

Kiss, L. L. ^{[3
]}

O'Toole, S. J. ^{[3
]}

Kambe, E. ^{[6
]}

Ando, H. ^{[7
]}

Izumiura, H. ^{[6
]}

Sato, B. ^{[8
]}

Hartmann, M. ^{[9
]}

Hatzes, A. P. ^{[9
]}

Appourchaux, T. ^{[10
]}

Barban, C. ^{[11
]}

Berthomieu, G. ^{[12
]}

Bouchy, F. ^{[13
]}

Garcia, R. A. ^{[14
]}

Lebrun, J-C ^{[15
]}

Martic, M. ^{[15
]}

Michel, E. ^{[11
]}

Mosser, B.

Nghiem, P. A. P. ^{[14
]}

Provost, J. ^{[12
]}

Samadi, R. ^{[11
]}

Thevenin, F. ^{[12
]}

Turck-Chieze, S. ^{[14
]}

Bonanno, S. A. ^{[16
]}

Benatti, S. ^{[17
]}

Claudi, R. U. ^{[17
]}

Cosentino, R. ^{[18
]}

Leccia, S. ^{[19
]}

Frandsen, S. ^{[2
]}

Brogaard, K. ^{[2
]}

Grundahl, F. ^{[2
]}

Stempels, H. C. ^{[20
]}

Bazot, M. ^{[2
]}

Dall, T. H. ^{[21
]}

Karoff, C. ^{[2
]}

Carrier, F. ^{[22
]}

Eggenberger, P. ^{[23
]}

Sosnowska, D. ^{[24
]}

Wittenmyer, R. A. ^{[25
]}

Endl, M. ^{[26
]}

Metcalfe, T. S. ^{[27
]}

机构：

[1] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[2] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark

[3] Univ Sydney, Sch Phys A28, Sydney, NSW 2006, Australia

[4] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany

[5] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA

[6] Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan

[7] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[8] Tokyo Inst Technol, Tokyo 1528550, Japan

[9] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany

[10] Univ Paris XI CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France

[11] Univ Paris 06, Univ Denis Diderot, Observ Paris, CNRS,LESIA, F-92195 Meudon, France

[12] Observ Cote Azur, UMT CNRS 6202, Lab Cassiopee, F-06304 Nice, France

[13] Inst Astrophys, CNRS, F-75014 Paris, France

[14] CEA Saclay, DAPNIA DSM Serv Astrophys, F-91191 Gif Sur Yvette, France

[15] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France

[16] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy

[17] Osserv Astron Padova, INAF, I-35122 Padua, Italy

[18] Telescopio Nazl Galileo, INAF, Santa Cruz de La Palma 38700, Spain

[19] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy

[20] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

[21] Gemini Observ, Hilo, HI 96720 USA

[22] Katholieke Univ Leuven, Inst Sterrekunde, B-3001 Heverlee, Belgium

[23] Univ Liege, Inst Astrophys & Geophys, B-4000 Cointe Ougree, Belgium

[24] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland

[25] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[26] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA

[27] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA

来源：

PROCEEDINGS OF THE SECOND HELAS INTERNATIONAL CONFERENCE: HELIOSEISMOLOGY, ASTEROSEISMOLOGY AND MHD CONNECTIONS | 2008年 / 118卷

关键词：

D O I：

10.1088/1742-6596/118/1/012059

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Procyon A is a bright F5IV star in a binary system. Although the distance, mass and angular diameter of this star are all known with high precision, the exact evolutionary state is still unclear. Evolutionary tracks with different ages and different mass fractions of hydrogen in the core pass, within the errors, through the observed position of Procyon A in the Hertzsprung-Russell diagram. For more than 15 years several different groups have studied the solar-like oscillations in Procyon A to determine its evolutionary state. Although several studies independently detected power excess in the periodogram, there is no agreement on the actual oscillation frequencies yet. This is probably due to either insufficient high-quality data (i.e., aliasing) or due to intrinsic properties of the star (i.e., short mode lifetimes). Now a spectroscopic multi-site campaign using 10 telescopes world-wide (minimizing aliasing effects) with a total time span of nearly 4 weeks (increase the frequency resolution) is performed to identify frequencies in this star and finally determine its properties and evolutionary state.

引用

页数：7

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