![]() Magnetized planets have an area above their ionospheres which traps energetic particles and plasma along magnetic fields, referred to as magnetospheres. Planetary Graphic of the magnetosphere of Jupiter with a flux tube connecting Jupiter and Io shown in yellow. Solar prominences are modeled using twisted magnetic flux tubes known as flux ropes. The result of emerging twisted flux tubes from the interior of the sun cause twisted magnetic structures in the corona, which then lead to solar prominences. The confined magnetic field strength varies from 0.1 to 10 G with diameters ranging from 200 to 300 km. These flux tubes confine plasma and are characterized as isolated. These coronal loops get their characteristic high luminosity and ranges of shapes from the behavior of the magnetic flux tube. The plasma inside the loop has a higher temperature than the surroundings causing the pressure and density of the plasma to increase. Plasma that is trapped within magnetic flux tubes that are attached to the photosphere, referred to as footpoints, create a loop-like structure known as a coronal loop. If there is a significant difference in the temperatures in the flux tube and the surroundings, there is a decrease in plasma pressure as well as a decrease in the plasma density causing some of the magnetic field to escape the plasma. The magnetic field causes the plasma pressure in the flux tube to decrease, known as the plasma density depletion region. These flux tubes are concentrated strong magnetic fields that are found between solar granules. ![]() Tube-like region of space with constant magnet flux along its length Diagram of a flux tube showing the magnetic field lines B Wb. ![]()
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