Статья

HYBRID γ DORADUS-δ SCUTI PULSATORS: NEW INSIGHTS INTO THE PHYSICS OF THE OSCILLATIONS FROM <i>KEPLER</i> OBSERVATIONS

A. GrigahcèneCentro de Astrofísica, Faculdade de Ciências, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, PortugalV AntociL. A. BalonaSouth African Astronomical Observatory, P.O. Box 9, Observatory 7935, South AfricaG. CatanzaroINAF-Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, ItalyJ. Daszyńska‐DaszkiewiczInstytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622 Wrocław, PolandJoyce Ann GuzikLos Alamos National Laboratory, X-2 MS T-086, Los Alamos, NM 87545-2345, USAG. HandlerG. HoudekD. W. KurtzJeremiah Horrocks Institute of Astrophysics, University of Central Lancashire, Preston PR1 2HE, UKM. MarconiINAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Naples, ItalyM. J. P. F. G. MonteiroCentro de Astrofísica, Faculdade de Ciências, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, PortugalA. MoyaLaboratorio de Astrofísica Estelar y Exoplanetas, LAEX-CAB (INTA-CSIC), P.O. Box 78, 28691 Villanueva de la Cañada, Madrid, SpainV. RipepiINAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Naples, ItalyJ. C. SuárezInstituto de Astrofísica de Andalucía (CSIC), CP3004, Granada, SpainK. UytterhoevenLaboratoire AIM, CEA/DSM CNRS-Université Paris Diderot, IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette Cedex, FranceW. J. BoruckiNASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USAT. M. BrownLas Cumbres Observatory Global Telescope, Goleta, CA 93117, USAJ. Christensen‐DalsgaardDepartment of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C, DenmarkRonald L. GillilandSpace Telescope Science Institute, Baltimore, MD 21218, USAJon M. JenkinsSETI Institute/NASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USAH. KjeldsenDepartment of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C, DenmarkDavid KochNASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USAS. BernabeiINAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, ItalyPaul A. BradleyLos Alamos National Laboratory, X-4 MS T-087, Los Alamos, NM 87545-2345, USAM. BregerM. Di CriscienzoINAF-Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone, Rome, ItalyM. A. DupretInstitut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17-B 4000 Liège, BelgiumR. A. GarcíaLaboratoire AIM, CEA/DSM CNRS-Université Paris Diderot, IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette Cedex, FranceAntonio García HernándezInstituto de Astrofísica de Andalucía (CSIC), CP3004, Granada, SpainJason JackiewiczDepartment of Astronomy, New Mexico State University, Las Cruces, NM 88001, USAAndreas KaiserH. LehmannThueringer Landessternwarte, 07778 Tautenburg, GermanyS. Martín‐RuizInstituto de Astrofísica de Andalucía (CSIC), CP3004, Granada, SpainP. MathiasDépartement Fizeau, UMR 6525 Observatoire de la Cöte d'Azur/CNRS, BP 4229, F06304 Nice Cedex 4, FranceJ. Molenda‐ŻakowiczInstytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622 Wrocław, PolandJ. M. NemecDepartment of Physics and Astronomy, Camosun College, Victoria, British Columbia, CanadaJ. NusplKonkoly Observatory of the Hungarian Academy of Sciences, P.O. Box 67, H-1525 Budapest, HungaryM. PaparóKonkoly Observatory of the Hungarian Academy of Sciences, P.O. Box 67, H-1525 Budapest, HungaryM. RothKiepenheuer Institut für Sonnenphysik, Schöneckstr. 6, 79104, Freiburg, GermanyR. SzabóKonkoly Observatory of the Hungarian Academy of Sciences, P.O. Box 67, H-1525 Budapest, HungaryM. D. SuranAstronomical Institute of the Romanian Academy, Str. Cutitul de Argint 5, RO 40557, Bucharest, RomeniaR. VenturaINAF-Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy

2010en

ABI

Аннотация

Observations of the pulsations of stars can be used to infer their interior structure and test theoretical models.<br/>The main-sequence γ Doradus (Dor) and δ Scuti (Sct) stars with masses 1.2–2.5 M are particularly useful for these studies. The γ Dor stars pulsate in high-order g-modes with periods of order 1 day, driven by convective blocking at the base of their envelope convection zone. The δ Sct stars pulsate in low-order g- and p-modes with periods of order 2 hr, driven by the κ mechanism operating in the He ii ionization zone. Theory predicts an overlap region in the Hertzsprung–Russell diagram between instability regions, where “hybrid” stars pulsating in both types of modes should exist. The two types of modes with properties governed by different portions of the stellar interior provide complementary model constraints. Among the known γ Dor and δ Sct stars, only four have been confirmed as hybrids. Now, analysis of combined Quarter 0 and Quarter 1 Kepler data for hundreds of variable stars shows that the frequency spectra are so rich that there are practically no pure δ Sct or γ Dor pulsators, i.e., essentially all of the stars show frequencies in both the δ Sct and the γ Dor frequency range. A new observational classification scheme is proposed that takes into account the amplitude as well as the frequency and is applied to categorize 234 stars as δ Sct, γ Dor, δ Sct/γ Dor or γ Dor/δ Sct hybrids.<br/>

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Идентификаторы

DOI: 10.1088/2041-8205/713/2/l192

Цитирования и источники

Цитирований: 4Использованных источников: 0

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