Reading Solar System Science 2020

在阅读太阳系科学，我们提出了五个独立的项目，以获得进一步的洞察力和了解太阳和日光层物理，磁层等离子体过程和行星大气。我们的研究将解决一些重要问题，如太阳的运行方式、太阳的变化对太阳系的影响、空间天气学以及其他行星上的生命存在等。太阳风是太阳外层大气的一个术语，它在太阳系中不断扩张，像风一样吹过行星。我们将使用基于物理学的模型和数据同化，对几十年来太阳风的结构进行首次重建。然后，我们就可以对这一重建过程进行探索，以发现更多关于太阳风产生的信息。太阳风将磁场从我们的星星深处带到太阳系。该场形成闭合环（两端都在太阳处）和“开放”线程，其中只有一端起源于太阳。对于日光层中有多少“开放”磁场存在，不同的独立测量方法提供了不同的开放磁场（称为“开放太阳通量”）存在量的估计;我们将使用大量新的和旧的现场航天器测量来试图解释差异。太阳周期性地向太阳风中发射大气泡等离子体，称为日冕物质抛射（CME）。这些气泡流过太阳风，与太阳风相互作用，改变形状和速度。我们将使用成像数据，其中一些已经由公民科学家处理，沿着基于物理的模型来推断CME在不同太阳风场景中传播时的变化。我们将采用一种新的技术来探测CME的密度如何在运输中变化。在离地球更近的地方，环绕地球的辐射带中的高能电子部分受到与各种电磁波相互作用的控制。我们对这些波粒相互作用的强度有一个有用的理论描述，但它只适用于随时间变化不大的波。现实世界的观测表明，波和等离子体条件是高度可变的，因此我们希望运行基于物理的数值实验，以确定我们应该如何使用波粒相互作用的知识来更好地模拟辐射带的行为。我们将在实验室中建立火星大气的模拟物，以便更好地了解火星大气中带电尘埃粒子和尘卷风的行为。气氛火星的干旱环境支持尘暴的形成，这些尘暴比地球上的尘暴大得多，也更强，我们建议在实验室中重现它们的形成条件，以便更好地了解这些大气现象如何影响甲烷的分布。重要的是，甲烷可以提供地球上生命存在的线索之一。

In Reading Solar System Science, we propose five independent projects to gain further insight and understanding in solar and heliospheric physics, magnetospheric plasma processes and planetary atmospheres. Our research will address questions important to how our Sun works, how its variability affects the solar system, the science of space weather, and the existence of life on other planetary bodies.The solar wind is the term given to the outer atmosphere of the Sun, which is constantly expanding through the solar system and blowing across the planets like a wind. We will use physics-based models and data assimilation to make the first reconstruction of the structure of the solar wind over many decades. This reconstruction can then be probed to discover more about the generation of the solar wind.The solar wind carries the magnetic field from deep within our star out into the solar system. This field forms closed loops (with both ends at the Sun) and "open" threads, where only one end originates at the Sun. Different independent measures of how much "open" magnetic field exists in the heliosphere provide different estimates of the amount of open field (known as "open solar flux") that exists; we will use a large number of new and old in-situ spacecraft measurements to attempt to explain the discrepancy.Periodically, the Sun emits large bubbles of plasma into the solar wind, known as coronal mass ejections (CMEs). These bubbles flow through the solar wind, interacting with it and changing shape and speed. We will use imaging data, some of which has been processed by citizen scientists, along with physics-based models to infer the changes in CMEs as they propagate through different solar wind scenarios. We will employ a novel technique to probe how the density of CMEs changes in transit too. Closer to the Earth, the energetic electrons in the radiation belts that surround the Earth are controlled in part by interactions with a wide range of electromagnetic waves. We have a useful theoretical description of the strength of these wave-particle interactions, but it was only designed for waves that do not vary much in time. Real-world observations indicate that the waves and plasma conditions are highly variable and so we look to run physics-based numerical experiments to identify how we should use our knowledge of wave-particle interactions to better model the behaviour of the radiation belt.Finally, we will build analogues of the Martian atmosphere in the laboratory in order to better understand the behaviour of charged dust particles and dust devils in the Martian atmosphere. The arid environment of Mars supports the formation of dust devils that are much larger and stronger than those found on Earth, and we propose to recreate conditions for their formation in the lab, in order to better understand how these atmospheric phenomena affect the distribution of methane. Importantly, methane could provide one of the clues to the existence of life on the planet.