发表机构
Institute of Science and Technology Austria (ISTA); Instituto de Astrofísica de Canarias; Departamento de Astrofísica, Universidad de La Laguna; Université Paris Cité; Université Paris-Saclay; CEA; CNRS（奥地利科学技术研究所; 加那利群岛天体物理研究所; 拉帕尔马大学天体物理学系; 巴黎西岱大学; 巴黎萨克雷大学; 法国原子能和替代能源委员会; 法国国家科学研究中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过构建质量增加模型，发现并合历史可显著改变红巨星内部磁场强度的星震学估计，并降低抑制混合模式的临界场强。
AI 中文摘要
红巨星辐射区内部磁场强度的星震学估计强烈依赖于由模型导出的内部恒星结构。由于红巨星分支并合产物已被证明可能拥有与同质量单星不同的核心结构，我们研究了质量增加历史如何影响我们对内部磁场强度的估计。我们构建了在红巨星分支演化阶段开始后经历或不经历质量增加事件的恒星模型，其质量范围为$1.1\\,M_\odot \le M \le 2\\,M_\odot$。首先，通过假设弱磁场，我们研究了质量增加事件对振荡频率对磁场全局敏感性的影响。我们发现，在质量高于$1.6\\,M_\odot$时，质量增加模型对磁场的敏感性可能比相同总质量的单星模型高出数倍。因此，考虑并合候选体的质量增加演化历史可以对磁场强度进行显著修正。在存在强磁场的情况下，我们还表明，如果发生了质量增加事件（对于质量$M\gtrsim1.6\\,M_\odot$的恒星），抑制混合偶极模式所需的临界场强显著降低。因此，被抑制恒星分布的大质量端强烈倾向于并合起源。我们得出结论，当旨在从星震学观测中约束内部场强估计时，正确约束恒星演化历史至关重要。
英文摘要
Asteroseismic estimates of the magnetic field strength in the radiative interior of red giant stars depend strongly on the internal stellar structure derived from models. Since red giant branch merger products have been shown to be able to possess a different core structure than single stars of the same mass, we investigate how a mass-gain history influences our estimates of an internal magnetic field strength. We construct stellar models with and without a mass-gain event after the onset of the RGB evolutionary phase with masses of $1.1\,M_\odot \le M \le 2\,M_\odot$. First, by assuming a weak magnetic field, we investigate the influence of a mass-gain event on the global sensitivity of the oscillation frequencies to the magnetic field. We find that mass-gain models can be several times more sensitive to the field than single-star models of identical total mass at masses above $1.6\,M_\odot$. Therefore, considering a mass-gain evolutionary history for merger candidates allows a significant correction to the magnetic field strength. In the presence of strong magnetic fields, we also show that the critical field strength needed to suppress mixed dipole modes is significantly lower if a mass-gain event has occurred (for stars with masses $M\gtrsim1.6\,M_\odot$). The massive end of the suppressed stars' distribution is therefore strongly favored by a merger origin. We conclude that properly constraining the stellar evolutionary history is essential when aiming to constrain internal field strength estimates from asteroseismic observations.
Comments15 pages, 11 Figures, 2 Tables, accepted for publication in A&A
