Why Do Active Regions Erupt? Modeling of Active Region from Pre-Eruptive to Eruptive Processes
为什么活跃区域会爆发?
基本信息
- 批准号:1650854
- 负责人:
- 金额:$ 38.59万
- 依托单位:
- 依托单位国家:美国
- 项目类别:Standard Grant
- 财政年份:2017
- 资助国家:美国
- 起止时间:2017-08-01 至 2021-07-31
- 项目状态:已结题
- 来源:
- 关键词:
项目摘要
Solar eruptions have significant impact on the near-Earth environment due to the enhanced flux of energetic particles bombarding the Earth and the embedded magnetic structures impacting the Earth's magnetosphere. This has serious consequences for our technological assets both in space and on the ground, including interruption of tele-communication, compromising the safety of astronauts, and damaging satellites and electric power grids. Therefore, focused investigations of solar eruptions and the associated magnetic field evolution of the solar corona have the potential to reveal the underlying physical mechanism(s) of the drivers of space weather at the Sun. This 3-year project is aimed at investigating the physical origins of solar eruptions at the Sun by means of data-driven, three-dimensional (3-D) numerical simulations. The project also has a strong educational component as it provides partial support for a Ph.D. student and a junior scientist at the University of Alabama in Huntsville. Thus, the research and EPO agenda of this project supports the Strategic Goals of the AGS Division in discovery, learning, diversity, and interdisciplinary research.This 3-year project is aimed at answering some of the fundamental questions concerning the physical origin and evolution of solar eruptions, which will expand the frontier of existing knowledge on the energy release during solar flares and Coronal Mass Ejections (CMEs) on the Sun and the associated reconfiguration of the solar corona. The underlying research objectives are: (i) understanding the fundamental active region (AR) eruptive physics; and, (ii) providing a practical tool as an initiation model for the development of a physics-based data-driven space weather prediction code. The research plan is to use the MHD-DARE model developed by the project team, together with observational data from the HMI and AIA instruments onboard the Solar Dynamics Observatory (SDO), to address the following science questions: (i) what are the basic characteristics of magnetic field configuration before a solar eruption?; (ii) how do photospheric surface motions, including shear, convergence and flux cancellation bring the initial emerged fields to such an unstable configuration?; (iii) what are the specific roles played by magnetic flux rope and magnetic reconnection in triggering solar eruptions?; (iv) can we understand the complexity of various flare/eruption process from topology and evolution of the magnetic field?; and, (v) how do solar eruptions leave imprints on the photospheric fields? These aspects of the AR development will be connected to the evolution of the coronal field long before and during a solar eruption, for which the project team will use the MHD-DARE model to carry out numerical simulations driven by the time-dependent vector magnetograms. Then, the simulation results will be analyzed to yield the evolution of the magnetic topology, electric currents, plasma flows, and Lorentz force to determine the primary triggering mechanisms of the solar eruption, and they will be compared with relevant solar observations. In addition, the project team plans to further improve the current model by including a realistic energy equation and a plasma configuration directly from the photosphere into the solar corona.
太阳爆发对近地环境有重大影响,这是由于轰击地球的高能粒子通量增加以及嵌入的磁性结构影响地球磁层。 这对我们在太空和地面的技术资产造成严重后果,包括中断远程通信,危及宇航员的安全,破坏卫星和电网。 因此,对太阳爆发和日冕相关磁场演变的重点调查有可能揭示太阳空间天气驱动因素的潜在物理机制。 这个为期三年的项目旨在通过数据驱动的三维数值模拟研究太阳爆发的物理起源。 该项目还具有很强的教育成分,因为它为博士学位提供部分支持。他是亨茨维尔市亚拉巴马大学的一名学生和初级科学家。 因此,该项目的研究和EPO议程支持AGS部门在发现,学习,多样性和跨学科研究方面的战略目标。这个为期3年的项目旨在回答有关太阳爆发的物理起源和演变的一些基本问题,这将扩大太阳耀斑和日冕物质抛射(CME)期间能量释放的现有知识的前沿太阳和太阳日冕的相关重新配置。 基本研究目标是:了解基本的活动区喷发物理学;提供一个实用工具,作为开发基于物理学的数据驱动空间气象预测代码的初始模型。 研究计划是利用项目小组开发的MHD-DARE模型,以及太阳动力学观测台(SDO)上HMI和AIA仪器的观测数据,解决以下科学问题:(i)太阳爆发前磁场结构的基本特征是什么?(ii)光球表面的运动,包括切变、会聚和通量抵消,是如何使最初出现的场变成如此不稳定的结构的?(iii)磁通绳和磁场重联在引发太阳爆发中扮演什么样的具体角色?(iv)我们能否从磁场的拓扑结构和演化来理解各种耀斑/喷发过程的复杂性?以及,(v)太阳爆发如何在光球场上留下印记? AR开发的这些方面将与太阳爆发之前和期间日冕场的演变有关,为此,项目团队将使用MHD-DARE模型进行由随时间变化的矢量磁图驱动的数值模拟。 然后,将分析模拟结果,以产生磁拓扑结构,电流,等离子体流和洛伦兹力的演变,以确定太阳爆发的主要触发机制,并将它们与相关的太阳观测进行比较。 此外,项目小组计划进一步改进目前的模型,包括一个现实的能量方程和直接从光球层进入日冕的等离子体配置。
项目成果
期刊论文数量(7)
专著数量(0)
科研奖励数量(0)
会议论文数量(0)
专利数量(0)
Comparison of the Hall Magnetohydrodynamics and Magnetohydrodynamics Evolution of a Flaring Solar Active Region
- DOI:10.3847/1538-4357/ac3bce
- 发表时间:2021-12
- 期刊:
- 影响因子:0
- 作者:K. Bora;R. Bhattacharyya;A. Prasad;B. Joshi;Q. Hu
- 通讯作者:K. Bora;R. Bhattacharyya;A. Prasad;B. Joshi;Q. Hu
Magnetohydrodynamic Simulation of Magnetic Null-point Reconnections and Coronal Dimmings during the X2.1 Flare in NOAA AR 11283
- DOI:10.3847/1538-4357/abb8d2
- 发表时间:2020-09
- 期刊:
- 影响因子:0
- 作者:A. Prasad;K. Dissauer;Q. Hu;R. Bhattacharyya;A. Veronig;Sanjay Kumar;B. Joshi
- 通讯作者:A. Prasad;K. Dissauer;Q. Hu;R. Bhattacharyya;A. Veronig;Sanjay Kumar;B. Joshi
Effects of Cowling Resistivity in the Weakly Ionized Chromosphere
弱电离色球层罩电阻率的影响
- DOI:10.3847/2041-8213/aba69a
- 发表时间:2020
- 期刊:
- 影响因子:0
- 作者:Yalim, M. S.;Prasad, A.;Pogorelov, N. V.;Zank, G. P.;Hu, Q.
- 通讯作者:Hu, Q.
Validation and Interpretation of a Three-dimensional Configuration of a Magnetic Cloud Flux Rope
- DOI:10.3847/1538-4357/ac7803
- 发表时间:2022-04
- 期刊:
- 影响因子:0
- 作者:Q. Hu;Chunming Zhu;W. He;J. Qiu;L. Jian;A. Prasad
- 通讯作者:Q. Hu;Chunming Zhu;W. He;J. Qiu;L. Jian;A. Prasad
A magnetic flux rope configuration derived by optimization of two-spacecraft In-situ measurements
- DOI:10.3389/fphy.2022.960315
- 发表时间:2022-06
- 期刊:
- 影响因子:0
- 作者:Q. Hu;W. He;Yu Chen
- 通讯作者:Q. Hu;W. He;Yu Chen
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Qiang Hu其他文献
Morphometric analysis of stem-group mollusks from the northern Yangtze Craton, China
中国扬子克拉通北部干群软体动物的形态分析
- DOI:
10.1017/jpa.2022.29 - 发表时间:
2022-05 - 期刊:
- 影响因子:1.4
- 作者:
Yanchun Pang;Michael Steiner;Ben Yang;Mingcai Hou;James G. Ogg;Wenhu Ji;Qiang Hu;Siyu Liang;Mengshao Zhang;Yangjian He;Li Lin - 通讯作者:
Li Lin
ドップラーセンサを用いた非接触型宅内行動認識システムの開発と評価
使用多普勒传感器的非接触式室内行为识别系统的开发和评估
- DOI:
- 发表时间:
2020 - 期刊:
- 影响因子:0
- 作者:
Qiang Hu;Yuejun Guo;Xiaofei Xie;Maxime Cordy;Lei Ma;Mike Papadakis;Yves Le Traon;三崎慎也,馬越圭介,松井智一,Hyuckjin Choi,藤本まなと,安本慶一 - 通讯作者:
三崎慎也,馬越圭介,松井智一,Hyuckjin Choi,藤本まなと,安本慶一
Online identification of a link function degradation model for solid oxide fuel cells under varying-load operation
变负载运行下固体氧化物燃料电池链路功能退化模型的在线辨识
- DOI:
10.1016/j.ijhydene.2021.10.177 - 发表时间:
2021-11 - 期刊:
- 影响因子:7.2
- 作者:
Yingtian Chi;Yiwei Qiu;Jin Lin;Yonghua Song;Qiang Hu;Wenying Li;Shujun Mu - 通讯作者:
Shujun Mu
Neyman-Pearson-Based Early Mode Decision for HEVC Encoding
基于 Neyman-Pearson 的 HEVC 编码早期模式决策
- DOI:
10.1109/tmm.2015.2512799 - 发表时间:
2016-03 - 期刊:
- 影响因子:7.3
- 作者:
Qiang Hu;Xiaoyun Zhang;Zhiru Shi;Zhiyong Gao - 通讯作者:
Zhiyong Gao
A comparison study of a solar active-region eruptive ?lament and a neighboring non-eruptive ?lament
太阳活动区喷发性哀伤与邻近非喷发性哀伤的比较研究
- DOI:
- 发表时间:
2016 - 期刊:
- 影响因子:0
- 作者:
Chaowei Jiang;S. T. Wu;Xueshang Feng;Qiang Hu - 通讯作者:
Qiang Hu
Qiang Hu的其他文献
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{{ truncateString('Qiang Hu', 18)}}的其他基金
Collaborative Research: DKIST Critical Science: Study of Flare Producing Active Regions with Highest Resolution Observations and Data-based Magnetohydrodynamics (MHD) Modeling
合作研究:DKIST 关键科学:利用最高分辨率观测和基于数据的磁流体动力学 (MHD) 建模研究耀斑产生的活动区域
- 批准号:
2204385 - 财政年份:2022
- 资助金额:
$ 38.59万 - 项目类别:
Standard Grant
Collaborative Research: Dynamic and Non-Force-Free Properties of Solar Active Regions and Subsequent Initiation of Flares
合作研究:太阳活动区域的动态和非无力特性以及随后耀斑的引发
- 批准号:
1954503 - 财政年份:2020
- 资助金额:
$ 38.59万 - 项目类别:
Standard Grant
SHINE: Analysis of Solar Active Region Energetics Based on Non-Force-Free Coronal Magnetic Field Extrapolation
SHINE:基于非无力日冕磁场外推的太阳活动区能量学分析
- 批准号:
1062050 - 财政年份:2011
- 资助金额:
$ 38.59万 - 项目类别:
Continuing Grant
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