Exploring the multi-scaled nature of solar vortices with DKIST
与 DKIST 一起探索太阳涡旋的多尺度性质
基本信息
- 批准号:2878221
- 负责人:
- 金额:--
- 依托单位:
- 依托单位国家:英国
- 项目类别:Studentship
- 财政年份:2023
- 资助国家:英国
- 起止时间:2023 至 无数据
- 项目状态:未结题
- 来源:
- 关键词:
项目摘要
Braiding and twisting of magnetic field structures, rooted within the surface of the Sun, has been considered important for understanding the origins of solar atmospheric heating, one of the longest unsolved puzzles in all of astrophysics. Persistent counter-streaming flows at the solar surface layer (known as the photosphere) provides the perfect conditions facilitating magnetic twist, brought about by vortex formation due to turbulent convection. Multi-layer numerical MagnetoHydroDynamics (MHD) of 3D vortex tubes have shown that they are more than adequate to supply enough Poynting flux to heat the solar corona. However, it is not yet known how frequently vortices appear from observations, how correlated they are between the atmospheric layers and how magnetic fields respond to vortices. With the advent of the Daniel K Inouye 4-m Solar Telescope (DKIST) observations, we now have the opportunity to understand the collective nature of solar vortices statistically, at unprecedented spatial and temporal resolution, and to finally confirm the collective contribution of vortices to solar atmospheric heating.Despite recent advancements in the statistical account of small-scale vortex motions in the solar photosphere, their magnetic fields and heating impacts in the layers above remain unconfirmed. Vortex motion is expected to dictate much of the physics in other twisting phenomena that appear to dominate the chromosphere, including spicules Photospheric vortex flow fields are often inferred from motions of magnetic bright points at intergranular lanes. With the application of a novel fully-automated photospheric vortex identification algorithms, inter-granular photospheric intensity vortices have been detected in large numbers for the first time, with the Swedish 1-m Solar Telescope. At the resolution of 100km, it was proposed that at any time there could be ~1.4x106 photospheric vortices covering about 2.8% of the solar surface. However, in the chromosphere above the photosphere the manifestation of vortices is much more difficult to detect and so far most studies are limited to a handful of events detected "by eye". In this project, we will develop new approaches to the automated detection of vortices in multiple atmospheric layers with DKIST, in order to understand the 3D nature of vortex tubes channelling energy from the photosphere to the corona. The project aims to exploit new ground-based observations from DKIST in order to accurately quantify:a) how many vortices in the photosphere appear as chromospheric vortices (and vice versa)?b) how twisted are magnetic fields within vortex tubes in the chromosphere?c) how much MHD wave power is excited in chromospheric swirls for basal heating of the corona?To address the three questions we outline the following three project objectives:Detect, track, characterize and correlate simultaneous vortex flows in both the photosphere and chromosphere, using DKIST observations. Demonstrate the coupling of vorticity between atmospheric layers and understand its importance for energy transfer.Measure changes in the vector magnetic field in the photosphere and chromosphere from DKIST observations in VISP, VBI and VTF. Find evidence of magnetic twist in swirls, for the first time, which is an important feature of numerical models of magnetic tornadoes in delivering Poynting flux.Identify and characterize wave properties, correlations with heating signatures and non-potentiality of magnetic field in a large-scale swirl, co-observed with DKIST and Interface Region Imaging Spectrometer (IRIS).
磁场结构的编织和扭曲,植根于太阳表面,被认为是理解太阳大气加热起源的重要因素,这是所有天体物理学中最长的未解决的难题之一。太阳表面层(称为光球层)持续的逆流流动提供了促进磁扭曲的完美条件,这是由湍流对流形成的涡旋所带来的。三维涡流管的多层数值磁流体动力学(MHD)已经表明,它们足以提供足够的坡印亭通量来加热日冕。然而,目前还不知道涡旋在观测中出现的频率,它们在大气层之间的相关性以及磁场对涡旋的反应。随着丹尼尔K井上4米太阳望远镜(DKIST)观测的出现,我们现在有机会以前所未有的空间和时间分辨率从统计上了解太阳涡旋的集体性质,并最终确认涡旋对太阳大气加热的集体贡献。尽管最近在太阳光球层中小尺度涡旋运动的统计解释方面取得了进展,它们的磁场和对上层的加热影响仍然没有得到证实。预计涡旋运动将决定其他似乎主导色球层的扭曲现象(包括针状体)的大部分物理特性,光球涡旋流场通常根据粒间通道磁亮点的运动来推断。随着一种新的全自动光球涡旋识别算法的应用,瑞典1米太阳望远镜首次大量探测到了颗粒间光球强度涡旋。在100公里的分辨率下,任何时候都可能有约1.4 × 106个光球涡旋覆盖约2.8%的太阳表面。然而,在光球层上方的色球层中,涡旋的出现要困难得多,到目前为止,大多数研究仅限于“肉眼”检测到的少数事件。在这个项目中,我们将开发新的方法来自动检测多个大气层中的涡旋与DKIST,以了解涡流管的3D性质从光球引导能量到日冕。该项目旨在利用DKIST新的地面观测数据,以便准确地量化:a)光球中有多少涡旋出现在色球涡旋中(反之亦然)?B)色球层中涡流管内的磁场有多扭曲?c)在色球涡旋中激发了多少MHD波功率用于日冕的基底加热?为了解决这三个问题,我们概述了以下三个项目的目标:检测,跟踪,表征和相关的光球和色球层的同时涡流,使用DKIST观测。演示大气层之间涡度的耦合并理解其对能量传输的重要性。通过VISP、VBI和VTF中的DKIST观测测量光球层和色球层中矢量磁场的变化。首次发现涡旋中存在磁扭曲的证据,这是磁龙卷风数值模型在传递坡印亭通量方面的一个重要特征。通过DKIST和界面区域成像光谱仪(IRIS)共同观测,确定并表征大尺度涡旋中的波特性、与加热特征的相关性以及磁场的非势性。
项目成果
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其他文献
吉治仁志 他: "トランスジェニックマウスによるTIMP-1の線維化促進機序"最新医学. 55. 1781-1787 (2000)
Hitoshi Yoshiji 等:“转基因小鼠中 TIMP-1 的促纤维化机制”现代医学 55. 1781-1787 (2000)。
- DOI:
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LiDAR Implementations for Autonomous Vehicle Applications
- DOI:
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2021 - 期刊:
- 影响因子:0
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吉治仁志 他: "イラスト医学&サイエンスシリーズ血管の分子医学"羊土社(渋谷正史編). 125 (2000)
Hitoshi Yoshiji 等人:“血管医学与科学系列分子医学图解”Yodosha(涉谷正志编辑)125(2000)。
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Effect of manidipine hydrochloride,a calcium antagonist,on isoproterenol-induced left ventricular hypertrophy: "Yoshiyama,M.,Takeuchi,K.,Kim,S.,Hanatani,A.,Omura,T.,Toda,I.,Akioka,K.,Teragaki,M.,Iwao,H.and Yoshikawa,J." Jpn Circ J. 62(1). 47-52 (1998)
钙拮抗剂盐酸马尼地平对异丙肾上腺素引起的左心室肥厚的影响:“Yoshiyama,M.,Takeuchi,K.,Kim,S.,Hanatani,A.,Omura,T.,Toda,I.,Akioka,
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