asteroseismology; stars: oscillations; stars: early-type; stars: fundamental parameters; open clusters and associations: individual: NGC 6910; Astrophysics - Solar and Stellar Astrophysics
Abstract :
[en] Asteroseismology offers the possibility of probing stellar interiors and testing evolutionary and seismic models. Precise photometry and spectroscopy obtained during multi-site campaigns on young open clusters allows discovering rich samples of pulsating stars and using them in a simultaneous seismic modelling called ensemble asteroseismology. The aim of this study is to obtain the age of the open cluster NGC 6910 by means of ensemble asteroseismology of the early-type pulsating members, to derive their stellar parameters, and to classify the excited modes. We used time-series analysis, performed photometric and spectroscopic mode identification, and calculated grids of evolutionary and seismic models to apply the procedure of ensemble asteroseismology for nine pulsating members of NGC 6910. With two iterations of the procedure of ensemble asteroseismology applied to nine pulsating stars we derived an age of 10.6[SUB]-0.8[/SUB][SUP]+0.9[/SUP] Myr for NGC 6910. We also identified the degree l for 8 of 37 modes detected in these stars and classified all modes in terms of p, g, and mixed-mode pulsations. Of the nine pulsating stars examined in the paper, eight are β Cep stars, including three that are hybrid β Cep and slowly pulsating B-type (SPB) pulsators, and one is an SPB star. Interestingly, the least massive β Cep star, NGC 6910-38, has a mass of about 5.6 M[SUB]☉[/SUB]. The present theory does not predict unstable p modes in B-type stars with such a low mass. The g modes with relatively high frequencies (> 3.5 d[SUP]-1[/SUP]), observed in three members of the cluster, are also stable according to seismic modelling. Both findings pose a challenge for theoretical calculations and prompt a revision of the opacities. The procedure of ensemble asteroseismology was found to be successful for NGC 6910 and χ Per on the basis of pulsating B-type stars and can therefore be applied to other young open clusters that are rich in such stars. <P />The photometry presented in Sect. 3 is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/cat/J/A+A/632/A95">http://cdsarc.u-strasbg.fr/viz- bin/cat/J/A+A/632/A95</A>
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Moździerski, D.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Pigulski, A.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Kołaczkowski, Z.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland ; Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716, Warszawa, Poland
Michalska, G.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Kopacki, G.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Carrier, F.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Walczak, P.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Narwid, A.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Stęślicki, M.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland ; Space Research Centre, Polish Academy of Sciences, Kopernika 11, 51-622, Wrocław, Poland
Fu, J.-N.; Department of Astronomy, Beijing Normal University, 100875, Beijing, PR China
Jiang, X.-J.; National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, 100012, Beijing, PR China
Zhang, Ch; Department of Astronomy, Beijing Normal University, 100875, Beijing, PR China
Jackiewicz, J.; Department of Astronomy, New Mexico State University, Las Cruces, NM, 88003, USA
Telting, J.; Nordic Optical Telescope, Rambla José Ana Fernández Pérez 7, 38711, San Antonio, Breña Baja, Santa Cruz de Tenerife, Spain
Morel, Thierry ; Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique stellaire théorique et astérosismologie
Saesen, S.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium ; Département d'Astronomie, Université de Genève, Chemin des Maillettes 51, 1290, Versoix, Switzerland
Zahajkiewicz, E.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Bruś, P.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Śródka, P.; Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622, Wrocław, Poland
Vučković, M.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium ; Instituto de Física y Astronomía, Universidad de Valparaíso, Casilla, 5030, Valparaíso, Chile
Verhoelst, T.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium ; Royal Belgian Institute for Space Aeronomy, Ringlaan 3, 1180, Brussels, Belgium
Van Helshoecht, V.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Lefever, K.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium ; Royal Belgian Institute for Space Aeronomy, Ringlaan 3, 1180, Brussels, Belgium
Gielen, C.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Decin, L.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Vanautgaerden, J.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Aerts, C.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium ; Department of Astrophysics, IMAPP, Radboud University Nijmegen, 6500 GL, Nijmegen, The Netherlands)
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