Two following flaring loops during their evolution. The figure shows the distribution of density (upper panels), pressure (middle panels), and temperature (lower panels) in a slice in the [ r,θ ] plane passing through the middle of the loops. In the upper panels white lines represent magnetic field lines projected in the [ r,θ ] plane, while the black line shows the β = 1 surface. The slice encompasses an angular sector going from the rotation axis to the disk equatorial plane. The first flare occurs in a β> 1 region, surrounded with β< 1 region, and produces a magnetically confined loop linking star and disk. The second flare is also released in a β> 1 region, but at a larger distance from the star and at approximately the same angle φ, compared with the first flare. It appears a bit later in time, at time t = 93 s, and becomes bright at t = 155 s. Differently from the first flare, the hot plasma of the second flare is not magnetically confined (run F4f1.00a).