Consolidated Solar and Astrophysics Research at UCLan

这项综合拨款提案汇集了中央兰开夏大学（UCLan）耶利米霍罗克斯研究所（JHI）在太阳物理学，恒星天体物理学，银河天体物理学和银河系外天体物理学的关键研究领域的研究。在所有这些领域，我们将在天体物理学研究的前沿解决关键的科学问题。在太阳物理学领域，我们将研究一些问题，例如在我们理解日冕、光球层和色球层之间的界面时包括精确的建模，以便对日冕加热问题提供定量的了解。我们将模拟太阳高能粒子（SEP）在日光层中的运动，以研究SEP从太阳到地球的传输。这将与太阳爆发事件和SEP传输之间关系的研究相联系，这反过来将使我们能够更准确地预测空间天气对地球的影响。我们还将研究太阳黑子的旋转，并了解是什么导致它们旋转，以发现旋转的耀斑和太阳黑子在多大程度上导致太阳爆发。在另一项研究中，我们将发现太阳系中的行星对黄道带云的形成有什么影响。在恒星天体物理学领域，我们将解决星星形成中目前尚未解决的一些关键问题，特别是围绕星前核的形成、结构和演化的问题。这一点很重要，因为人们相信核心质量函数和恒星初始质量函数（IMF）之间存在联系。这将使我们对国际货币基金组织本身的起源有一个真正的物理理解。作为这项研究的一部分，我们将研究湍流和磁场在星星形成中的作用。我们还将研究原恒星周围圆盘的演化和双星对行星形成的影响，并模拟原恒星周围圆盘中巨行星的迁移，以了解这是如何受到恒星光度和圆盘性质的影响。我们还将利用开普勒的数据来探索和理解燃烧氢的主序星的内部角动量传输。在银河系和银河系外天体物理学领域，我们计划测量星系中恒星种群的年龄和丰度模式，以了解恒星形成的时间和地点。我们将模拟星系盘内恒星形成系统的物理过程，以便对银河系盘中的恒星迁移进行定量预测。这一领域的总体目标之一是推断银河系的质量组装，从而了解整个银河系的形成和演化。在外部星系中，我们将开发银河系外喷流中的准直冲击模拟，以包括额外的物理和现实条件，以便更好地理解这些高能现象。我们将解决类星体中的FeII问题，最后我们将研究明显超过均匀尺度极限的超大型类星体群，以便开始了解最大尺度上的宇宙。

This consolidated grant proposal brings together research within the Jeremiah Horrocks Institute (JHI) of the University of Central Lancashire (UCLan) in the key research areas of solar physics, stellar astrophysics, Galactic astrophysics, and extra-Galactic astrophysics. In all of these areas, we will be addressing key science questions at the cutting edge of astrophysical research. Some examples of these are given here.In the area of solar physics we will look at issues such as including accurate modelling in our understanding of the interface between the solar corona, photosphere and chromosphere, in order to provide quantitative insight into the solar coronal heating problem. We will simulate the motions of solar energetic particles (SEPs) in the heliosphere in order to study SEP transport from the Sun to the Earth. This will link into a study of the relation between solar eruptive events and SEP transport, which in turn will allow us to make more accurate predictions of space weather effects on the Earth. We will also study the rotation of sunspots and understand what causes them to rotate, in order to discover to what extent rotating flares and sunspots lead to solar eruptions. In another study we will discover what effect planets in our solar system have in shaping the zodiacal cloud.In the area of stellar astrophysics, we will solve some of the currently unanswered key questions in star formation, particularly those surrounding the formation, structure and evolution of prestellar cores. This is important, because there is believed to be a link between the core mass function and the stellar Initial Mass Function (IMF). It is planned that this will lead us to a true physical understanding of the origin of the IMF itself. As part of this study we will look at the roles of turbulence and magnetic fields in star formation. We will also study the evolution of discs around protostars and the effects of binarity on planet formation, and model the migration of giant planets in discs around protostars to see how this is affected by stellar luminosity and the properties of the disc. We will also use Kepler data to explore and understand internal angular momentum transport in hydrogen-burning, main-sequence stars.In the areas of Galactic and extra-Galactic astrophysics we plan to measure the ages and abundance patterns of stellar populations in galaxies, to understand when and where the stars formed. We will model physical processes in star-forming systems within the disc of a galaxy in order to develop quantitative predictions for stellar migration in the Milky Way disc. One of the overall goals in this area is to infer the mass assembly of the Milky Way, and hence to understand the formation and evolution of the Milky Way as a whole. In external galaxies we will develop recollimation shock simulations in extra-galactic jets to include additional physics and realistic conditions, in order to better understand these highly energetic phenomena. We will resolve the FeII problem in quasars, and finally we will study ultra-large quasar groups that apparently exceed the homogeneity scale limit, to begin to understand the Universe on its largest scales.