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  Small-scale dynamo in cool stars. I. Changes in stratification and near-surface convection for main-sequence spectral types

Bhatia, T. S., Cameron, R. H., Solanki, S. K., Peter, H., Przybylski, D., Witzke, V., & Shapiro, A. (2022). Small-scale dynamo in cool stars. I. Changes in stratification and near-surface convection for main-sequence spectral types. Astronomy and Astrophysics, 663, A166. doi:10.1051/0004-6361/202243607.

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アイテムのパーマリンク: https://hdl.handle.net/21.11116/0000-000C-9376-9 版のパーマリンク: https://hdl.handle.net/21.11116/0000-000D-B292-4
資料種別: 学術論文

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URL:
https://ui.adsabs.harvard.edu/abs/2022A&A...663A.166B (全文テキスト(全般))
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作成者

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 作成者:
Bhatia, Tanayveer S.1, 著者           
Cameron, Robert H.2, 著者           
Solanki, Sami K.1, 3, 著者           
Peter, Hardi1, 著者           
Przybylski, Damien, 著者
Witzke, Veronika, 著者
Shapiro, Alexander4, 著者           
所属:
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              
2Department Solar and Stellar Interiors, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832287              
3MPI for Aeronomy, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832291              
4Max Planck Research Group in Solar Variability and Climate, Max Planck Institute for Solar System Research, Max Planck Society, ou_2265637              

内容説明

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キーワード: stars: interiors; stars: late-type; stars: magnetic field; convection; dynamo; Astrophysics - Solar and Stellar Astrophysics
 要旨: Context. Some of the small-scale solar magnetic flux can be attributed to a small-scale dynamo (SSD) operating in the near-surface convection. The SSD fields have consequences for solar granular convection, basal flux, and chromospheric heating. A similar SSD mechanism is expected to be active in the near-surface convection of other cool main-sequence stars, but this has not been investigated thus far.
Aims: We aim to investigate changes in stratification and convection due to inclusion of SSD fields for F3V, G2V, K0V, and M0V spectral types in the near-surface convection.
Methods: We studied 3D magnetohydrodynamic (MHD) models of the four stellar boxes, covering the subsurface convection zone up to the lower photosphere in a small Cartesian box, based on the MURaM radiative-MHD simulation code. We compared the SSD runs against reference hydrodynamic runs.
Results: The SSD is found to efficiently produce magnetic field with energies ranging between 5% to 80% of the plasma kinetic energy at different depths. This ratio tends to be larger for larger Teff. The relative change in density and gas pressure stratification for the deeper convective layers due to SSD magnetic fields is negligible, except for the F-star. For the F-star, there is a substantial reduction in convective velocities due to Lorentz force feedback from magnetic fields, which, in turn, reduces the turbulent pressure.
Conclusions: The SSD in near-surface convection for cool main-sequence stars introduces small but significant changes in thermodynamic stratification (especially for the F-star) due to a reduction in the convective velocities.

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 日付: 2022
 出版の状態: 出版
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 識別子(DOI, ISBNなど): DOI: 10.1051/0004-6361/202243607
ISSN: 0004-6361
 学位: -

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出版物 1

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出版物名: Astronomy and Astrophysics
種別: 学術雑誌
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ページ: - 巻号: 663 通巻号: - 開始・終了ページ: A166 識別子(ISBN, ISSN, DOIなど): -