Quantifying when and where strong magnetic skew forms in a data-driven global non-potential model of the solar corona I: production and persistence of skew
Throughout the simulation, the angle of skew along polarity inversion lines, coloured to show dextral (reddish), sinistral (blueish), and very weak (green) skew.
Underneath, the normal component of the magnetic field is shown in white (positive) and black (negative).Throughout the simulation, the change, from the previous day to the current, in the angle of skew along polarity inversion lines, coloured to show increases (red) and decreases (blue).
Underneath, the normal component of the magnetic field is shown in white (positive) and black (negative).Throughout the simulation, skew in the corona, categorized to identify strong dextral (yellow), strong sinistral (blue), strengthening dextral (red), strengthening sinistral (purple), weakening dextral (green), and weakening sinistral (cyan) skew.
Underneath, the normal component of the magnetic field is shown in white (positive) and black (negative).
Linking computational models to follow the evolution of heated coronal plasma
Evolution of temperature, number density, thermal pressure, and field-aligned velocity along 1D thermodynamic model of a coronal strand, in response to an imposed heating function.
That heating function is derived from heating along a field line in a full 3D MHD simulation.
Coronal energy release by MHD avalanches: Heating mechanisms
Motion over time of the end points on the top plane of field lines traced from the bottom plane.
Seeds on the bottom plane are updated according to the imposed rotation on the boundary, such that 'the same' field lines are traced over time.
When the motion of end points deviates from the imposed boundary rotations, magnetic reconnection has occurred.Motion over time of field lines.
Field lines traced from the left-hand, central, and right-hand flux tubes are shown in yellow, blue, and magenta, respectively.
Field lines are traced from the bottom (slightly darker) and top (slightly lighter) boundary planes.
Seeds on each plane are updated according to the imposed rotation on the boundary, such that 'the same' field lines are traced over time.Axial current in the mid-plane.
Here, the component of current parallel (red) and anti-parallel (blue) to the initial magnetic field and axis of the flux tubes is plotted, evolving in time.