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The new computer simulations are based on a magnetic field structure that is often associated with prominences: the magnetic field lines in the corona form a double arc with a small dip in the middle. As the calculations show, the flame-like prominence forms in this dip and remains trapped there. All relevant layers of the Sun were taken into account, from the corona, the Sun’s outer atmosphere, to parts of the convection zone below the Sun’s surface. Image Credit: © MPS |
Scientific Frontline: Extended "At a Glance" Summary: Solar Prominence Supply Mechanisms
The Core Concept: Solar prominences are massive, densely packed structures of relatively cool plasma that extend for thousands of kilometers into the Sun's exceptionally hot outer atmosphere, the corona.
Key Distinction/Mechanism: Unlike the surrounding corona, which burns at over one million degrees, prominences consist of plasma cooled to approximately 10,000 degrees. They remain suspended and stable for weeks due to a delicate supply balance: turbulent magnetic forces in the cooler, lower layer of the Sun (the chromosphere) eject bursts of cool plasma upward, while hot coronal plasma simultaneously flows into magnetic dips and condenses, offsetting material that "rains" back down.
Major Frameworks/Components:
- Double-Arc Magnetic Architecture: Magnetic field lines in the corona frequently form a double arch resembling two adjacent mountains; the cool prominence material forms and becomes trapped within the central dip.
- Chromospheric Injection: Turbulent, small-scale magnetic field movements beneath the corona forcefully eject cool plasma upward to feed the prominence.
- Coronal Condensation: Secondary supply logistics occur when hot plasma travels along magnetic field lines into the central dip, where it cools and condenses.
- Multi-Layered Simulation Models: The research framework accounts for all relevant solar layers concurrently, linking turbulent plasma flows below the visible surface, the cooler chromosphere, and the extremely hot corona.