期刊
ASTRONOMY & ASTROPHYSICS
卷 618, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201832718
关键词
asteroseismology; methods: data analysis; stars: fundamental parameters; stars: variables: general; stars: oscillations; stars: rotation
资金
- Research Foundation Flanders (FWO, Belgium) [G.0B69.13, V4.272.17N]
- European Research Council (ERC) under the European Union [670519: MAMSIE, 647383: SPIRE]
- National Science Foundation of the United States [NSF PHY-1748958]
- Belgian Science Policy Office (Belspo) under ESA/PRODEX grant PLATO mission development
- Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO) [G0H5416N]
- PLATO CNES grant at CEA-Saclay
- Australian Research Council
- Danish National Research Foundation [DNRF106]
- MINECO/FEDER [ESP2015-65712-C5-5-R]
- Spanish MINECO [RYC-2012-09913]
- Fundacao para a Ciencia e a Tecnologia (FCT, Portugal) [SFRH/BPD/80619/2011]
- European Council Project SPACEINN [FP7-SPACE-2012-312844]
- National Science Foundation [AST 1716436, ACI 1663696]
- NASA's Science Mission Directorate
- Fundação para a Ciência e a Tecnologia [SFRH/BPD/80619/2011] Funding Source: FCT
Context. While rotation has a major impact on stellar structure and evolution, its effects are not well understood. Thanks to high-quality and long-time base photometric observations obtained with recent space missions, we are now able to study stellar rotation more precisely. Aims. We aim to constrain radial differential rotation profiles in gamma Doradus (gamma Dor) stars, and to develop new theoretical seismic diagnosis for such stars with rapid and potentially non-uniform rotation. Methods. We have derived a new asymptotic description which accounts for the impact of weak differential near-core rotation on gravity-mode period spacings. The theoretical predictions are illustrated from pulsation computations with the code GYRE and compared with observations of gamma Dor stars. When possible, we also derived the surface rotation rates in these stars by detecting and analysing signatures of rotational modulation, and computed the core-to-surface rotation ratios. Results. Stellar rotation must be strongly differential before its effects on period spacing patterns can be detected, unless multiple period spacing patterns can be compared. Six stars in our sample exhibit a single unexplained period spacing pattern of retrograde modes. We hypothesise that these are Yanai modes. Finally, we find signatures of rotational spot modulation in the photometric data of eight targets. Conclusions. If only one period spacing pattern is detected and analysed for a star, it is difficult to detect differential rotation. A rigidly rotating model will often provide the best solution. Differential rotation can only be detected when multiple period spacing patterns have been found for a single star or its surface rotation rate is known as well. This is the case for eight of the stars in our sample, revealing surface-to-core rotation ratios between 0.95 and 1.05.
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