Solar eruptions, such as solar flares, filament/prominence eruptions, jets, and coronal mass ejections, are violent explosions that occur frequently in the Sun’s corona. A major solar eruption can launch over billons of tons of magnetized plasma at high speeds into the heliosphere and could drive adverse space weather events that severely impact human activities in modern society. Research on solar eruptions has a long history of more than a century, and now it has been well-recognized that they are manifestations of a sudden release of free energy stored in the coronal magnetic fields which otherwise undergo a quasi-static evolution as driven by photospheric motions. However, the realistic eruptions as witnessed in recent observations are much more complex than previously thought and challenges theoretical and idealized models, especially on the questions such as how they are initiated, driven and evolve.
This Research Topic provides an opportunity for solar physicists to publish Original Research and Review articles on the theme of “Comprehensive understanding of solar eruptions by combining state-of-the-art observations and modelling”. With this Research Topic, we aim to better understand and characterize the whole life of solar eruptions, including the process of its energy building up, the initiation, and the subsequent evolution and propagation in solar wind. We solicit publications focused on the study of solar eruptions with cutting edge observational data, data-constrained modelling, and data-driven simulation. In particular, we encourage submissions utilizing jointly observations and numerical simulations together to answer/clarify fundamental but focused issues of solar eruptions.
The Research Topic welcomes articles focused on answering the following key questions,
1. What is the structure of the pre-eruptive magnetic field and how does it form?
2. What is the trigger of solar eruption and how is the CME accelerated impulsively?
3. What is the specific role played by ideal MHD instability and magnetic reconnection, respectively, in solar eruptions?
4. What are the key factors that determine a flare to be eruptive or confined?
5. Is there a threshold of magnetic free energy, relative helicity or other indicator of nonpotentiality of coronal magnetic field that determines the condition of the eruption?
6. How does the eruptive structure evolve and interplay with the background field, both locally and globally?
Solar eruptions, such as solar flares, filament/prominence eruptions, jets, and coronal mass ejections, are violent explosions that occur frequently in the Sun’s corona. A major solar eruption can launch over billons of tons of magnetized plasma at high speeds into the heliosphere and could drive adverse space weather events that severely impact human activities in modern society. Research on solar eruptions has a long history of more than a century, and now it has been well-recognized that they are manifestations of a sudden release of free energy stored in the coronal magnetic fields which otherwise undergo a quasi-static evolution as driven by photospheric motions. However, the realistic eruptions as witnessed in recent observations are much more complex than previously thought and challenges theoretical and idealized models, especially on the questions such as how they are initiated, driven and evolve.
This Research Topic provides an opportunity for solar physicists to publish Original Research and Review articles on the theme of “Comprehensive understanding of solar eruptions by combining state-of-the-art observations and modelling”. With this Research Topic, we aim to better understand and characterize the whole life of solar eruptions, including the process of its energy building up, the initiation, and the subsequent evolution and propagation in solar wind. We solicit publications focused on the study of solar eruptions with cutting edge observational data, data-constrained modelling, and data-driven simulation. In particular, we encourage submissions utilizing jointly observations and numerical simulations together to answer/clarify fundamental but focused issues of solar eruptions.
The Research Topic welcomes articles focused on answering the following key questions,
1. What is the structure of the pre-eruptive magnetic field and how does it form?
2. What is the trigger of solar eruption and how is the CME accelerated impulsively?
3. What is the specific role played by ideal MHD instability and magnetic reconnection, respectively, in solar eruptions?
4. What are the key factors that determine a flare to be eruptive or confined?
5. Is there a threshold of magnetic free energy, relative helicity or other indicator of nonpotentiality of coronal magnetic field that determines the condition of the eruption?
6. How does the eruptive structure evolve and interplay with the background field, both locally and globally?
