中国科大地空学院“瀚海问天”日地空间物理前沿论坛讲座第35期-Maria Madjarska

报告人简介：      

Dr. Maria Madjarska is a Senior Researcher at the Max Planck Institute for Solar System Research, with expertise in solar and heliospheric physics. Her research focuses on small-scale magnetic structures, coronal heating, and the origin of the solar wind, using coordinated multi-satellite and ground-based observations. Since August 2024, she has served on the Steering Committee of IAU Division E: Sun and Heliosphere. She holds multiple editorial roles, including Associate Editor for Astronomy & Astrophysics, Editor for the A&A Web of Conferences, and previously Associate Editor for Solar Physics. Her work advances research on solar atmospheric dynamics and Sun-heliosphere coupling.

摘要：

Loops are the fundamental structures that shape the magnetic skeleton of the solar atmosphere. This is captured by the emission recorded in images taken in the extreme ultraviolet (EUV) and X-ray wavelength ranges, as many of these loops confine plasma heated to a million degrees. The corona of the QS is filled with numerous loops (also coronal holes, though reduced in number), which were first named X-ray bright points (XBPs). After their counterpart was identified in extreme-ultraviolet emission, the more general term Coronal Bright Points (CBPs) was adopted. The fainter emission surrounding CBPs, both in EUV and X-rays, is possibly caused by the cumulative effect of many fainter and hard-to-distinguish loops. What makes the observational investigation and modelling of these small-scale loops very important is that they are a clear representation of one of the many faces of the coronal heating problem, namely the heating of plasma confined in magnetic loops. Also, the evolution of these small-scale loops has often been related to dynamic transient solar phenomena observed throughout the entire solar atmosphere, the extended corona, and possibly the solar wind. This implies that these loop systems may also have a significant impact on the mass and energy transfer in the solar atmosphere. During my seminar, I will review the morphology and the plasma and magnetic properties of small-scale bright and faint loop systems. I will report on the state-of-the-art modelling of these fundamental structures. I will give an overview of the dynamic transients that originate from these loop systems. My review talk will conclude with a discussion on the possible role of small-scale loops and associated transient phenomena in heating the solar atmosphere and wind.