Travel grant for observing with SST, La Palma- Dynamic events in the chromosphere of coronal holes: RBE's and Swirls

用于观察拉帕尔马海表温度的旅行补助金 - 日冕洞色球层的动态事件：RBE 和漩涡

• 批准号: ST/K003143/1
• 负责人: Robert Von Fay-Siebenburgen
• 金额: $ 0.29万
• 依托单位: University of Sheffield
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2012
• 资助国家: 英国
• 起止时间: 2012 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FK003143%2F1
• 关键词: Travel; grant; observing; SST; La

One of the most intriguing problems of modern plasma-astrophysics is the rapid rise of temperature in the magnetised solar atmosphere. It is now clear that part of the vast mechanical energy of sub-photospheric granular motions is channelled into the solar atmosphere (see e.g. our Nature paper, Wedemeyer-Bhom et al. 2012 on how this energy transport takes space in solar tornadoes), where it is dissipated leading to the enormous heating of ambient plasma to millions of K. The details of this energy transport is not yet fully understood. Since the solar atmosphere has a large variety of features, from spicules, fibrils, pores, sunspot, coronal loops, coronal holes, etc. the energisation may be different in each of them. Cardinal questions are: do magnetohydrodynamic (MHD) waves play a key role, or is it the build-up and rapid release of magnetic stresses? Magnetic field is very central in shaping the solar atmosphere because: it (i) not only outlines the MHD waveguides that act as channels for the energy to propagate but, it also (ii) determines connectivity topology; and (iii) stores energy relevant to plasma heating. A viable scenario of this energy channelling is that the both coherent and random (sub)photospheric motions excite MHD waves that sail through the magnetised solar atmosphere, while carrying and damping the necessary of non-thermal energy relevant in the magnetic structures of the solar atmosphere. It is not anymore a question whether MHD waves are there. Instead, focus is now on how the necessary wave flux needed towards plasma heating is present in the magnetised plasma structures and what type of MHD waves are the major players in the energy transport process(es). Here we propose (i) observing and comprehensive tracking MHD waves from photosphere to chromosphere in localised highly dynamic magnetic waveguides with emphases on the magnetic signatures of these waves; (ii) Next, we will determine the actual identity and nature of the detected MHD waves (slow, fast, Alfven; kink, sausage; surface, body; etc.); (iii) We will investigate how these waves are present in a range of structures (e.g. a) spicules at limb; b) swirls in coronal holes)(iv) We will build up statistics of these structures and the waves present therein

现代等离子体天体物理学最有趣的问题之一是磁化太阳大气中温度的快速上升。现在很清楚，亚光球粒状运动的巨大机械能的一部分被引导到太阳大气中（例如，参见我们的《自然》论文，Wedemeyer-Bhom等人，2012年，关于这种能量传输如何在太阳龙卷风中占据空间），在那里它被消散，导致周围等离子体的巨大加热到数百万K。这种能量传输的细节尚未完全了解。由于太阳大气具有多种特征，从骨针、原纤维、孔隙、太阳黑子、日冕环、日冕洞等，它们各自的能量可能不同。主要问题是：磁流体动力（MHD）波是否起着关键作用，或者它是磁应力的积累和快速释放？磁场对于塑造太阳大气至关重要，因为：它 (i) 不仅勾画出充当能量传播通道的 MHD 波导，而且 (ii) 决定了连接拓扑； (iii) 储存与等离子体加热相关的能量。这种能量通道的一个可行方案是，相干和随机（亚）光球运动都会激发穿过磁化太阳大气的 MHD 波，同时携带和阻尼与太阳大气磁结构相关的非热能。 MHD 波是否存在已不再是问题。相反，现在的重点是等离子体加热所需的波通量如何存在于磁化等离子体结构中，以及什么类型的 MHD 波是能量传输过程中的主要参与者。在这里，我们建议（i）在局部高动态磁波导中观察和全面跟踪从光球层到色球层的 MHD 波，重点关注这些波的磁特征； (ii) 接下来，我们将确定检测到的 MHD 波的实际身份和性质（慢波、快波、阿尔文波、扭结波、香肠波、表面波、身体波等）； (iii) 我们将研究这些波如何存在于一系列结构中（例如，a）肢体的骨针； b）冕洞中的漩涡）（iv）我们将建立这些结构和其中存在的波的统计数据

项目成果

THE DETECTION OF UPWARDLY PROPAGATING WAVES CHANNELING ENERGY FROM THE CHROMOSPHERE TO THE LOW CORONA

• DOI: 10.1088/0004-637x/791/1/61
• 发表时间: 2014-07
• 期刊: The Astrophysical Journal
• 作者: N. Freij;E. Scullion;E. Scullion;C. J. Nelson;C. J. Nelson;Stuart Mumford;S. Wedemeyer;R. Erdélyi

Statistical Analysis of Small Ellerman Bomb Events

• DOI: 10.1007/s11207-012-0222-3
• 发表时间: 2013-01
• 期刊: Solar Physics
• 影响因子: 2.8
• 作者: C. Nelson;J. Doyle;R. Erdélyi;Z. Huang;M. Madjarska;M. Mathioudakis;S. Mumford;K. Reardon

Observations and mode identification of sausage waves in a magnetic pore

• DOI: 10.1051/0004-6361/201425096
• 发表时间: 2015-07
• 期刊: Astronomy and Astrophysics
• 影响因子: 6.5
• 作者: M. Moreels;N. Freij;R. Erdélyi;T. Doorsselaere;G. Verth

ON THE PROPERTIES OF SLOW MHD SAUSAGE WAVES WITHIN SMALL-SCALE PHOTOSPHERIC MAGNETIC STRUCTURES

• DOI: 10.3847/0004-637x/817/1/44
• 发表时间: 2015-09
• 期刊: The Astrophysical Journal
• 作者: N. Freij;I. Dorotovic;R. Morton;M. Ruderman;M. Ruderman;V. Karlovský;R. Erdélyi;R. Erdélyi