太阳径向p模的速度强度不对称反转
Velocity-intensity asymmetry reversal of solar radial p-modes
摘要：
空间飞行任务的发展大大提高了类太阳振荡器测量光谱的质量。它们的$p$模式谱线轮廓现在可以被解析，并且可以推断出太阳以外的各种恒星的不对称性。然而，它已经知道了很长一段时间，太阳$p$ -模式的不对称性之间的速度和强度谱反转。了解这种反转的起源是必要的，以便使用不对称作为地震诊断的工具。对于恒星以外的太阳，只有强度功率谱是足够的解决，以允许模式不对称的估计。我们最近开发了一种方法，旨在模拟和预测这些不对称性的速度功率谱的太阳，并成功地将它们与它们的观测派生的同行。在本文中，我们扩展了我们的模型，并预测强度功率谱中的不对称性。我们发现，强度的模线轮廓的形状在很大程度上取决于如何处理的振荡引起的辐射通量的变化，它的建模现实是至关重要的理解不对称反转。扰动太阳校准的灰色大气模型，并采用准绝热框架作为第一步，我们再现了在太阳强度谱中观察到的低频模式的不对称性。我们的结论是，不像以前认为的，它是没有必要调用一个额外的机制（例如，非绝热效应，相干非共振背景信号）来解释不对称反转。然而，这种额外的机制是必要的，以解释高阶模式的不对称反转。
英文摘要：
The development of space-borne missions has significantly improved the quality of the measured spectra of solar-like oscillators. Their $p$-mode line profiles can now be resolved, and the asymmetries inferred for a variety of stars other than the Sun. However, it has been known for a long time that the asymmetries of solar $p$-modes are reversed between the velocity and the intensity spectra. Understanding the origin of this reversal is necessary in order to use asymmetries as a tool for seismic diagnosis. For stars other than the Sun, only the intensity power spectrum is sufficiently resolved to allow for an estimation of mode asymmetries. We recently developed an approach designed to model and predict these asymmetries in the velocity power spectrum of the Sun and to successfully compare them to their observationally derived counterparts. In this paper we expand our model and predict the asymmetries featured in the intensity power spectrum. We find that the shape of the mode line profiles in intensity is largely dependent on how the oscillation-induced variations of the radiative flux are treated, and that modelling it realistically is crucial to understanding asymmetry reversal. Perturbing a solar-calibrated grey atmosphere model, and adopting the quasi-adiabatic framework as a first step, we reproduce the asymmetries observed in the solar intensity spectrum for low-frequency modes. We conclude that, unlike previously thought, it is not necessary to invoke an additional mechanism (e.g. non-adiabatic effects, coherent non-resonant background signal) to explain asymmetry reversal. This additional mechanism is necessary, however, to explain asymmetry reversal for higher-order modes.
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。
