Pulsational amplitude growth of the star KIC 3429637 (HD 178875) in the context of Am and ρ Pup stars

被引：25

作者：

Murphy, Simon J. ^{[1
]}

Grigahcene, A. ^{[2
,3
,4
]}

Niemczura, E. ^{[5
]}

Kurtz, D. W. ^{[1
]}

Uytterhoeven, K. ^{[6
,7
]}

机构：

[1] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

[2] Univ Porto, Fac Ciencias, Ctr Astrofis, P-4150762 Oporto, Portugal

[3] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA

[4] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[5] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland

[6] IAC, Tenerife 38205, Spain

[7] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Spain

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 427卷 / 02期

基金：

美国国家科学基金会;

关键词：

stars: chemically peculiar; stars: individual: HD 178875; stars: oscillations; stars: variables: delta Scuti; F-TYPE STARS; DELTA-SCUTI; CHEMICAL-COMPOSITION; ABUNDANCE ANALYSIS; MAIN-SEQUENCE; OPEN CLUSTERS; NON-LTE; METALLICISM; VARIABILITY; ROTATION;

D O I：

10.1111/j.1365-2966.2012.22062.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

KIC 3429637 (HD 178875) is a delta Sct star whose light curve shows continuous pulsational amplitude growth in Kepler mission photometry. Analysis of the three largest amplitude peaks in the Fourier transform indicates different growth rates for all three. We have ruled out instrumental causes, and determine the amplitude growth to be intrinsic to the star. We calculate time-dependent convection models and compare them with the observations. We confirm earlier characterizations that KIC 3429637 is a marginal Am star through the analysis of new spectroscopic data. With the data presently available, a plausible cause of the amplitude growth is increasing pulsational driving as evolutionary changes shift the He II driving zone deeper in this rho Puppis star. If this model is correct, then we are watching real-time stellar evolutionary changes.

引用

页码：1418 / 1428

页数：11