Kepler observations of the variability in B-type stars

被引：122

作者：

Balona, L. A. ^{[1
]}

Pigulski, A. ^{[2
]}

De Cat, P. ^{[3
]}

Handler, G. ^{[4
]}

Gutierrez-Soto, J. ^{[5
,6
]}

Engelbrecht, C. A. ^{[7
]}

Frescura, F. ^{[8
]}

Briquet, M. ^{[9
]}

Cuypers, J. ^{[3
]}

Daszynska-Daszkiewicz, J. ^{[2
]}

Degroote, P. ^{[9
]}

Dukes, R. J. ^{[10
]}

Garcia, R. A. ^{[11
]}

Green, E. M. ^{[12
]}

Heber, U. ^{[13
]}

Kawaler, S. D. ^{[14
]}

Lehmann, H. ^{[15
]}

Leroy, B. ^{[6
]}

Molenda-Zakowicz, J. ^{[2
]}

Neiner, C. ^{[6
]}

Noels, A. ^{[16
]}

Nuspl, J. ^{[23
]}

Ostensen, R.

Pricopi, D. ^{[17
]}

Roxburgh, I. ^{[23
]}

Salmon, S. ^{[16
]}

Smith, M. A. ^{[18
]}

Suarez, J. C.

Suran, M.

Szabo, R. ^{[19
]}

Uytterhoeven, K. ^{[11
]}

Christensen-Dalsgaard ^{[20
]}

Kjeldsen, H. ^{[20
]}

Caldwell, D. A. ^{[21
]}

Girouard, F. R. ^{[22
]}

Sanderfer, D. T.

机构：

[1] S African Astron Observ, ZA-7935 Cape Town, South Africa

[2] Uniwersytet Wroclawski, Inst Astron, PL-51622 Wroclaw, Poland

[3] Koninklijke Sterrenwacht Belgie, B-1180 Brussels, Belgium

[4] Univ Vienna, Inst Astron, A-1180 Vienna, Austria

[5] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[6] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France

[7] Univ Johannesburg, Dept Phys, Johannesburg, South Africa

[8] Univ Witwatersrand, Sch Phys, Johannesburg, South Africa

[9] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium

[10] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA

[11] CEA DSM CNRS Univ Paris Diderot, IRFU SAp, Ctr Saclay, Lab AIM, F-91191 Gif Sur Yvette, France

[12] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[13] FAU Erlangen Nuremberg, Astron Inst, Dr Karl Remeis Observ ECAP, D-96049 Bamberg, Germany

[14] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA

[15] Thuringer Landessternwarte, Tautenburg, Germany

[16] Univ Liege, Inst Astron & Geophys, Liege, Belgium

[17] Romanian Acad, Astron Inst, Bucharest, Romania

[18] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[19] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary

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

[21] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA

[22] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA

[23] Queen Mary Univ London, London E1 4NS, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2011年 / 413卷 / 04期

关键词：

stars: early-type; stars: oscillations; SOLAR-LIKE OSCILLATIONS; ALPHA EMISSION STARS; BETA-CEPHEI STARS; DETECTS G-MODES; OPACITY MECHANISM; INITIAL CHARACTERISTICS; ROTATIONAL VELOCITIES; SPECTRAL-ANALYSIS; ASAS-3; DATA; NU-ERIDANI;

D O I：

10.1111/j.1365-2966.2011.18311.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The analysis of the light curves of 48 B-type stars observed by Kepler is presented. Among these are 15 pulsating stars, all of which show low frequencies, characteristic of slowly pulsating B (SPB) stars. Seven of these stars also show a few weak, isolated high frequencies and they could be considered as SPB/beta Cephei (beta Cep) hybrids. In all cases, the frequency spectra are quite different from what is seen from ground-based observations. We suggest that this is because most of the low frequencies are modes of high degree which are predicted to be unstable in models of mid-B stars. We find that there are non-pulsating stars within the beta Cep and SPB instability strips. Apart from the pulsating stars, we can identify stars with frequency groupings similar to what is seen in Be stars but which are not Be stars. The origin of the groupings is not clear, but may be related to rotation. We find periodic variations in other stars which we attribute to proximity effects in binary systems or possibly rotational modulation. We find no evidence for pulsating stars between the cool edge of the SPB and the hot edge of the delta Sct instability strips. None of the stars shows the broad features which can be attributed to stochastically excited modes as recently proposed. Among our sample of B stars are two chemically peculiar stars, one of which is a HgMn star showing rotational modulation in the light curve.

引用

页码：2403 / 2420

页数：18

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