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 - 胃物理学最有趣的问题之一是磁化太阳大气中温度的迅速升高。 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.由于太阳大气层具有各种特征，因此从香料，原纤维，孔，黑子，冠状环，冠状孔等。基本问题是：磁水动力学（MHD）波是否起关键作用，还是磁应力的积累和快速释放？磁场在塑造太阳气氛方面非常中心，因为它不仅概述了能量传播能量的通道的MHD波导，而且（ii）决定了连接性拓扑； （iii）存储与血浆加热相关的能量。这种能量通道的可行场景是，相干和随机（子）光电运动激发了穿过磁性太阳能气氛的MHD波，同时承载和抑制了与太阳能大气层磁性结构相关的非热能的必要条件。是否有MHD波是否存在问题。取而代之的是，现在的焦点是如何在磁性的等离子体结构中存在对等离子体加热所需的必要波通量以及哪种类型的MHD波是能量传输过程（ES）的主要参与者。在这里，我们提出（i）观察和全面的跟踪MHD波从光球到色球，在局部高度动态的磁性波导中，重点是这些波的磁特征； （ii）接下来，我们将确定检测到的MHD波的实际身份和性质（慢速，快速，Alfven；扭结，香肠；表面，身体；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spicules； b）冠状孔中的旋流）（iv）我们将建立这些结构的统计数据和其中存在的波浪

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