arXiv 2602.157352026-02astro-ph.SR

自转对太阳型恒星声学模振幅的影响：来自流体动力学模拟的见解

Impact of rotation on the amplitude of acoustic modes in solar-like stars: Insights from hydrodynamical simulations

Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、天体物理学与分子相互作用研究所）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University（西北大学跨学科天文探索与研究中心）

Arthur Le Saux, Leïla Bessila, Stéphane Mathis

备注：: Accepted for publication in MNRAS Letters

阅读 PDF

arXiv 页面 ↗HTML 原文 ↗

AI总结：

研究通过流体动力学模拟探讨自转如何影响太阳型恒星声学模振幅，发现自转增强导致振幅下降和模衰减率增加，揭示了自转对振荡特性的影响。

摘要：

在太阳型恒星中，声学模是探测其内部结构和动态的主要方式。尽管这些模在具有对流包层的恒星中预期普遍存在，但开普勒观测显示，显著比例的太阳型恒星表现出不可检测的声学模，特别是在快速自转和磁活动性强的恒星中。最近的理论工作提出，自转倾向于抑制对流运动，从而减少可用于随机激发低阶声学模的功率。在此，我们通过完全可压缩的流体动力学模拟测试这一预测，使用MUSIC代码进行一系列2.5D模拟，考虑纵向对称性，覆盖自转率从0到8Ω⊙。我们发现随着自转率的增加，声学模振幅呈现明显且系统的下降。在最快速自转模型中，模衰减率也增强。随着自转率的增加，激发的减少和衰减的增加提供了对快速自转太阳型恒星中模可检测性的减少的物理解释。我们的结果表明，自转可以显著改变振荡特性，并且在解释恒星震颤观测时必须加以考虑。

英文摘要：

In solar-like stars, acoustic modes provide the main way of probing their internal structure and dynamics. Although these modes are expected to be ubiquitous in stars with convective envelopes, Kepler observations reveal that a significant fraction of solar-like stars show no detectable acoustic modes, particularly among rapidly rotating and magnetically active stars. Recent theoretical work has proposed that rotation tends to inhibit convective motions, thereby reducing the power available for stochastic excitation of low degree acoustic modes. Here, we test this prediction using fully compressible hydrodynamical simulations of a solar-like star. We perform a series of 2.5D simulations, which consider longitudinal symmetry, using the MUSIC code spanning rotation rates from 0 to 8 $Ω_{\odot}$. We find a clear and systematic decline of acoustic mode amplitudes with increasing rotation rate. In the most rapidly rotating models, mode damping rates are also enhanced. The combined reduction in excitation and increase in damping with increasing rotation rate provide a physical explanation for the observed decrease in mode detectability in rapidly rotating solar-like stars. Our results demonstrate that rotation can significantly modify oscillation properties and must be accounted for when interpreting asteroseismic observations.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

AI总结：

摘要：

英文摘要：

相关论文