Helioseismology at Birmingham and Queen Mary

太阳是恒星天体物理学的试金石。它是研究其他恒星的内部物理、结构和动力学的支柱。了解是什么推动了观测到的恒星活动和排放的变化，不仅对日地关系至关重要，而且对于研究其他恒星对其当地环境的影响也具有更广泛的意义，这对探测到的系外行星的宜居性具有明显的影响。在最近的太阳研究中，最突出的是对目前较弱的第24个太阳周期的研究，该周期显示出低水平的活动，这在现代望远镜和卫星观测时代是前所未有的。随着我们迈向24/25最低周期和进入新周期，日震学不仅在了解这些变化的内部驱动因素，而且在了解它们可能持续的时间方面发挥着重要作用。我们将利用伯明翰太阳振荡网络(BISON)，通过当前弱活动周期的下降来跟踪太阳的地震行为，进入下一个太阳极小值。我们将从其他地面和空间日震仪器中挖掘这些数据和数据，以分离和提取内部结构和动态变化的特征。利用我们的野牛数据，我们还将首次有机会对一个完整的22年Hale周期与另一个进行地震比较。我们还将利用卫星和地面贡网的太阳分辨率数据，监测进入第25个周期时近地表流动模式的发展，并研究太阳包层的内部自转和组成。我们的另一个主要焦点涉及现在已经很成熟的太阳丰度或太阳模拟问题，即利用最新的化学丰度测定所建立的模型与太阳(由日震学确定)的结构持续存在分歧。我们将对太阳深部的物理学提出新的限制，特别是在天体物理不透明和非标准物理学可能有助于解决问题的程度上，利用我们联盟在模拟恒星内部方面的领先专业知识。这是太阳研究的一个例子，对恒星天体物理学的更广泛领域具有重要影响。

The Sun is a touchstone for stellar astrophysics. It is an anchor for studies of the internal physics, structure and dynamics of other stars. Understanding what drives the observed changes to its activity and emissions is not only of crucial importance to solar-terrestrial relations, but also has wider relevance to studies of the influence that other stars have on their local environments, with the obvious implications for habitability of detected exoplanets. Prominent among recent solar research have been studies of the current, weak Solar Cycle 24, which has shown low levels of activity that are unprecedented in the era of modern telescope and satellite observations. As we move towards the Cycle 24/25 minimum and into the new cycle, helioseismology has an important role to play in understanding not only the internal drivers for these changes, but also how long-lasting they might be. We will track the seismic behaviour of the Sun through the decline of the current, weak activity cycle into the next solar minimum, using the Birmingham Solar-Oscillations Network (BiSON). We will mine these data and data from other ground-based and space-borne helioseismic instruments, to isolate and extract signatures of structural and dynamic changes in interior. Using our BiSON data we will also have the first ever opportunity to conduct a seismic comparison of one full 22-year Hale cycle with another. We will also utilize resolved-Sun data from satellites and the ground-based GONG network to monitor the development of near-surface flow patterns as we head into Cycle 25, and to study the internal rotation and composition of the solar envelope.Our other major focus relates to the now well established solar-abundance or solar modelling problem, i.e., the continuing disagreement of the structures of models constructed using updated chemical abundance determinations with the Sun (as determined by helioseismology). We will provide new constraints on the physics of the deep solar interior, in particular on the extent to which astrophysical opacities and non-standard physics might help to resolve the problem, exploiting the leading expertise of our consortium in modelling stellar interiors. This is an example of solar research that has important implications for the wider domain of stellar astrophysics.