Simulated temporal evolution of plasma properties during the formation and disappearance of MBP2. Top left: normalised G-band intensity. Top right: evolution of total pressure (solid), gas pressure (dotted), magnetic pressure (dashed) and mass density (dash-dotted) at log(τ_{500 nm}) = 0. Bottom left: evolution of modulus of the magnetic field (solid) and line-of-sight velocity (dashed) at log(τ_{500 nm}) = 0, where downward (red-shifted) velocity is positive. Bottom right: plasma temperature evolution at log(τ_{500 nm}) = 0 (solid), log(τ_{500 nm}) = −1 (dashed) and log(τ_{500 nm}) = −2 (dotted). Markers along the x-axis indicate times at which images and profiles were taken for Fig. A.2.

First row: sequence of simulated G-band images over time. The green box encloses the area where MBP2 is seen to appear and disappear. Second row: sequence of simulated Stokes-I profiles from the centre of MBP2 (solid) and these degraded to the SOT spatial resolution (dotted). Third row: sequence of Stokes-V profiles (solid) with these degraded to the SOT spatial resolution (dotted). Fourth row: sequence of Stokes profiles (solid) with these degraded to the SOT spatial resolution (dotted). All profiles are normalised to the average continuum intensity, Ic.

Left: the Stokes-V amplitude asymmetries emanating from the central pixel of MBP2 (solid) for the 6 profiles of Fig. A.2. Right: the corresponding Stokes-V area asymmetries. The asymmetries of the degraded profiles are also shown (dashed).

Top row: simulations of the normalised G-band intensity slices for three snapshots of the MBP before, during and after its peak intensity. Middle row: line-of-sight velocity maps of the solar surface with the centre of the MBP located at approximately (375, 375) km. Redshifted velocity is positive. The horizontal dashed line represents the cut at which the G-band intensity plots are taken for the top row graphs. Bottom row: vertical velocity maps perpendicular to the solar surface, taking into account vertical and horizontal velocities with arrows representing the direction and magnitude of velocities. The solid white line is used to show the location of optical depth unity.

Simulated temporal evolution of plasma properties during the formation and disappearance of MBP3. Top left: normalised G-band intensity. Top right: evolution of total pressure (solid), gas pressure (dotted), magnetic pressure (dashed) and mass density (dash-dotted) at log(τ_{500 nm}) = 0. Bottom left: evolution of modulus of the magnetic field (solid) and line-of-sight velocity (dashed) at log(τ_{500 nm}) = 0, where downward (red-shifted) velocity is positive. Bottom right: plasma temperature evolution at log(τ_{500 nm}) = 0 (solid), log(τ_{500 nm}) = −1 (dashed) and log(τ_{500 nm}) = −2 (dotted). Markers along the x-axis indicate times at which images and profiles were taken for Fig. A.6.

First row: sequence of simulated G-band images over time. The green box encloses the area where MBP3 is seen to appear and disappear. Second row: sequence of simulated Stokes-I profiles from the centre of MBP3 (solid) and these degraded to the SOT spatial resolution (dotted). Third row: sequence of Stokes-V profiles (solid) with these degraded to the SOT spatial resolution (dotted). Fourth row: sequence of Stokes profiles (solid) with these degraded to the SOT spatial resolution (dotted). All profiles are normalised to the average continuum intensity, Ic.

Left: the Stokes-V amplitude asymmetries emanating from the central pixel of MBP3 (solid) for the 6 profiles of Fig. A.6. Right: the corresponding Stokes-V area asymmetries. The asymmetries of the degraded profiles are also shown (dashed).

Top row: simulations of the normalised G-band intensity slices for three snapshots of the MBP before, during and after its peak intensity. Middle row: line-of-sight velocity maps of the solar surface with the centre of the MBP located at approximately (375, 375) km. Redshifted velocity is positive. The horizontal dashed line represents the cut at which the G-band intensity plots are taken for the top row graphs. Bottom row: vertical velocity maps perpendicular to the solar surface, taking into account vertical and horizontal velocities with arrows representing the direction and magnitude of velocities. The solid white line is used to show the location of optical depth unity.