Reading Solar System Science 2020

阅读太阳系科学 2020

• 批准号: ST/V000497/1
• 负责人: Mathew Owens
• 金额: $ 104.09万
• 依托单位: University of Reading
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2021
• 资助国家: 英国
• 起止时间: 2021 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FV000497%2F1
• 关键词: Reading; Solar; System; Science; 2020

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.

在阅读太阳系科学时，我们提出了五个独立的项目，以进一步了解太阳能和地球物理学，磁层等离子体过程和行星气氛。我们的研究将解决对我们的太阳工作原理的重要问题，其可变性如何影响太阳系，太空天气科学以及其他行星体内生命的存在。太阳风是赋予太阳外部气氛的术语，该术语在太阳的外部气氛中不断扩展，该术语在太阳系中不断扩展，并像风一样吹过星球。我们将使用基于物理学的模型和数据同化来对太阳风结构进行数十年的首次重建。然后可以探究这种重建，以发现有关太阳风的产生的更多信息。太阳风将磁场从我们的恒星内的深处带入太阳系。该磁场形成闭环（两端在太阳下）和“开放”线，其中只有一端起源于太阳。在Heliosphere中存在多少“开放”磁场的不同独立测量，提供了存在存在的开放场量（称为“开放太阳通量”）的不同估计值；我们将使用大量新的和旧的原位航天器测量值来试图解释差异。末端，太阳在太阳风中散发出很大的血浆气泡，称为冠状质量弹出（CMES）。这些气泡流过太阳风，与它相互作用并改变形状和速度。我们将使用成像数据，其中一些是由公民科学家处理的，以及基于物理学的模型来推断CME通过不同的太阳风场传播时的变化。我们将采用一种新颖的技术来探测CME的密度也如何变化。靠近地球，围绕地球的辐射带中的能量电子部分通过与各种电磁波相互作用来控制。我们对这些波颗粒相互作用的强度有一个有用的理论描述，但仅针对时间不大的波设计。现实世界的观察表明，波浪和血浆条件是高度可变的，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利用对波颗粒相互作用的知识，以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层的类似物，以更好地理解带电的尘埃和尘埃的行为。火星的干旱环境支持比地球上发现的尘埃魔鬼的形成更大，更强，我们建议为它们在实验室中形成的条件重新创建条件，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，甲烷可以为地球上生命的存在提供一个线索。

项目成果

Observational Evidence of S-web Source of the Slow Solar Wind

• DOI: 10.3847/1538-4357/acc653
• 发表时间: 2023-03
• 期刊: The Astrophysical Journal
• 作者: D. Baker;P. Démoulin;S. Yardley;T. Mihailescu;L. Driel-Gesztelyi;R. D’Amicis;D. Long;A. To;C. Owen;T. Horbury;D. Brooks;D. Perrone;R. French;A. James;M. Janvier;S. Matthews;M. Stangalini;G. Valori;P. Smith;R. A. Cuadrado;H. Peter;U. Schuehle;L. Harra;Krzysztof Barczynski;D. Berghmans;A. Zhukov;L. Rodriguez;C. Verbeeck

SIR-HUXt -- a particle filter data assimilation scheme for assimilating CME time-elongation profiles

SIR-HUXt——用于同化 CME 时间伸长剖面的粒子滤波器数据同化方案

• DOI: 10.48550/arxiv.2210.02122
• 发表时间: 2022
• 作者: Barnard L

Assessing the potential of heliospheric imager data assimilation to improve CME modelling.

评估日光层成像仪数据同化改进 CME 建模的潜力。

• DOI: 10.5194/egusphere-egu22-5613
• 发表时间: 2022
• 作者: Barnard L

HUXt -- An open source, computationally efficient reduced-physics solar wind model, written in Python

HUXt——一种开源、计算高效的简化物理太阳风模型，用 Python 编写

• DOI: 10.48550/arxiv.2210.00455
• 发表时间: 2022
• 作者: Barnard L

Improving CME modelling with data assimilation of Heliospheric Imager observations into the HUXt solar wind numerical model.

通过将日光层成像仪观测数据同化到 HUXt 太阳风数值模型中，改进 CME 建模。

• DOI: 10.5194/egusphere-egu21-192
• 发表时间: 2021
• 作者: Barnard L