Unresolved Rossby and gravity modes in 214 A and F stars showing rotational modulation
Article
Henriksen, Andreea I., Antoci, Victoria, Saio, Hideyuki, Grundahl, Frank, Kjeldsen, Hans, Van Reeth, Timothy, Bowman, Dominic M., Papics, Peter I., De Cat, Peter, Kruger, Joachim, Andersen, M. Fredslund and Palle, P. L.. 2023. "Unresolved Rossby and gravity modes in 214 A and F stars showing rotational modulation." Monthly Notices of the Royal Astronomical Society. 524 (3), pp. 4196-4211.
Article Title | Unresolved Rossby and gravity modes in 214 A and F stars showing rotational modulation |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Henriksen, Andreea I., Antoci, Victoria, Saio, Hideyuki, Grundahl, Frank, Kjeldsen, Hans, Van Reeth, Timothy, Bowman, Dominic M., Papics, Peter I., De Cat, Peter, Kruger, Joachim, Andersen, M. Fredslund and Palle, P. L. |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 524 (3), pp. 4196-4211 |
Number of Pages | 16 |
Year | 2023 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Web Address (URL) | https://academic.oup.com/mnras/article-abstract/524/3/4196/7210543 |
Abstract | Here, we report an ensemble study of 214 A- and F-type stars observed by Kepler, exhibiting the so-called hump and spike periodic signal, explained by Rossby modes (r modes) – the hump – and magnetic stellar spots or overstable convective (OsC) modes – the spike, respectively. We determine the power confined in the non-resolved hump features and find additional gravity-mode (g-mode) humps always occurring at higher frequencies than the spike. Furthermore, we derive projected rotational velocities from FIES, SONG, and HERMES spectra for 28 stars and the stellar inclination angle for 89 stars. We find a strong correlation between the spike amplitude and the power in the r and g modes, which suggests that both types of oscillations are mechanically excited by either stellar spots or OsC modes. Our analysis suggests that stars with a higher power in m = 1 r-mode humps are more likely to also exhibit humps at higher azimuthal orders (m = 2, 3, or 4). Interestingly, all stars that show g-mode humps are hotter and more luminous than the observed red edge of the δ Scuti instability strip, suggesting that either magnetic fields or convection in the outer layers could play an important role. |
Keywords | stars: early-type |
ANZSRC Field of Research 2020 | 5101. Astronomical sciences |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2023 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | Technical University of Denmark, Denmark |
Tohoku University, Japan | |
Aarhus University, Denmark | |
Institute of Astronomy, Belgium | |
Royal Observatory of Belgium | |
Adam Mickiewicz University, Poland | |
Centre for Astrophysics | |
Institute of Astrophysics of the Canary Islands, Spain | |
University of La Laguna, Spain |
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