发表机构
Max-Planck-Institut für Sonnensystemforschung; Institut für Astrophysik und Geophysik, Georg-August-Universität Göttingen; Center for Space Science, NYUAD Institute, New York University Abu Dhabi; School of Physics and Astronomy, University of Birmingham（马克斯·普朗克太阳系研究所; 哥廷根大学天体物理与地球物理研究所; 纽约大学阿布扎比分院空间科学中心; 伯明翰大学物理与天文学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究提出一种增强的互相关技术，通过设计滤波器分离不同ℓ的p模频率变化，经太阳数据验证，可应用于类太阳恒星KIC 8006161的频率位移测定。
AI 中文摘要
太阳和类太阳恒星的声学模式频率会因磁活动发生变化，其时间尺度远大于恒星自转周期，远小于恒星演化周期。鉴于观测到的恒星p模的信噪比（S/N）较低，测量单个模式频率的变化颇具挑战性。通常，人们会对不同时间序列片段的功率谱进行互相关以估算平均p模频率变化，最终会对各个模式的贡献取平均。我们旨在通过引入一种新颖且计算成本低廉的方法来增强互相关方法，从而能够解耦不同球谐次数ℓ对应的p模频率变化。假设倾角和自转速率已被测量，我们设计了滤波器，该滤波器可分离给定ℓ对应的模式频率变化δωℓ，同时防止相邻模式引入偏差。我们开展了蒙特卡洛模拟以量化δωℓ估算的不确定性。我们针对研究充分的太阳数据（SOHO/VIRGO和BiSON）验证了该方法，并证明其适用于类太阳开普勒（Kepler）恒星KIC 8006161。
英文摘要
Acoustic mode frequencies in the Sun and Sun-like stars change due to magnetic activity, on time-scales much larger than the star's rotation and much smaller than its evolution. Given the poor S/N of the observed stellar p-modes, it is challenging to measure the changes of individual mode frequencies. Typically, power spectra of different time series segments are cross-correlated to estimate a mean p-mode frequency change, which ends up averaging over the individual mode contributions. We seek to enhance the cross-correlation method, by introducing a novel and computationally cheap method, thus enabling us to disentangle p-mode frequency changes for different spherical harmonic degree $\ell$. Assuming that the inclination angle and rotation rate are already measured, filters are designed, which enable the isolation of $δω_\ell$, frequency changes of modes with a given $\ell$, while preventing bias creeping in from neighbouring modes. Monte-Carlo simulations are performed to quantify uncertainty in the estimation of $δω_\ell$. We validate our method against well-studied solar data (SOHO/VIRGO and BiSON) and demonstrate its applicability to the solar-like Kepler star KIC 8006161.
Comments7 pages, 9 figures, accepted A&A Letters
Journal refA&A, 713, L12 (2026)
DOI：10.1051/0004-6361/202661137
