Effect of Rotation on Wave Mixing in Intermediate-mass Stars

被引：3

作者：

Varghese, A. ^{[1
,2
]}

Ratnasingam, R. P. ^{[1
]}

Vanon, R. ^{[3
]}

Edelmann, P. V. F. ^{[4
]}

Mathis, S. ^{[2
]}

Rogers, T. M. ^{[1
,5
]}

机构：

[1] Newcastle Univ, Newcastle Upon Tyne, England

[2] Univ Paris Saclay, Univ Paris, Sorbonne Paris Cite, CEA,CNRS,IM, F-91191 Gif Sur Yvette, France

[3] Univ Leeds, Leeds, England

[4] Los Alamos Natl Lab, Los Alamos, NM USA

[5] Planetary Sci Inst, Tucson, AZ USA

来源：

ASTROPHYSICAL JOURNAL | 2024年 / 970卷 / 02期

基金：

欧洲研究理事会;

关键词：

INTERNAL GRAVITY-WAVES; ANGULAR-MOMENTUM TRANSPORT; GAMMA DORADUS STARS; STOCHASTIC EXCITATION; CONVECTIVE BOUNDARIES; INERTIAL WAVES; STELLAR; MODULES; MODES; FREQUENCY;

D O I：

10.3847/1538-4357/ad54b5

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Internal gravity waves are likely to cause mixing in stellar interiors. Studies show that the mixing by these waves changes drastically across age and mass. Here, we study the effect of rotation on this wave mixing by considering a 7 M circle dot model at zero-age main sequence and mid-main sequence. We compare the mixing profiles at a range of rotation rates (1 x 10-5, 2 x 10-5, 3 x 10-5, 4 x 10-5, and 1 x 10-4 rad s-1) and observe that the mixing decreases with decreasing Rossby number. This can be attributed to the effect of rotation on convection, which influences the amplitude with which the waves are excited near the convective-radiative interface.

引用

页数：10

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