Sea of Bubbles at Edge of Solar System
This animation summarizes the new heliospheric scenario and the formation of the "sea" of bubbles in the heliosheath. The Sun’s magnetic field points toward the Sun in the Northern hemisphere and away from the Sun in the Southern (shown in red and blue). These oppositely pointing magnetic fields are separated by a layer of current called the heliospheric current sheet. Due to the tilt of the magnetic axis in relation to the axis of rotation of the Sun, the heliospheric current sheet flaps like a flag in the wind. The flapping current sheet separates regions of oppositely pointing magnetic field, called sectors. As the solar wind speed decreases past the termination shock, the sectors squeeze together, bringing regions of opposite magnetic field closer to each other. When the separation of sectors becomes very small, the sectored magnetic field breaks up into a sea of nested "magnetic bubbles" in a phenomenon called magnetic reconnection.
