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The macroscopic MHD equation for the dynamic balance of the flowing plasma in the Jovian magnetodisc region has been solved for the aligned rotator model where the magnetic field rotates with the symmetrical configuration with respect to the magnetic equator that coincides with the perpendicular direction to the rotation axis. The equatorial region of the magnetodisc studied here is restricted in a limited azimuthal extent called “flow region”. The results indicate that the plasma is flowing out due to the centrifugal force forming the disc wind that blows outward with super magnetosonic velocity when the plasma approaches a critical region. The expansion of the disc current is also made as a result of the outflow of the plasma with slight differences of electron and proton velocity. In the region of the disc plasma, the magnetic field is frozen in the flowing plasma; there is a transient region, therefore, called here the internal magnetopause that separates the magnetic lobe of the Jovian magnetosphere from the flowing disc plasma. The plasma flow is interrupted at the inner boundary of the magnetopause forming the balance of the dynamic pressure between the solar wind and the disc wind. This inner boundary is sandwitching the intrinsic Jovian magnetic field with the outer boundary which is formed due to the solar wind interaction with the Jovian magnetic field.When the solar wind pressure increases, the position of the magnetopause is compressed with heating up effects on the disc plasma. The plasma flow can not, then, exceed the magnetosonic velocity and no disc wind is formed. The balance feature of the disc wind and the solar wind, thus, controls the location of the Jovian magnetopause so called spongy nature after the observation by the field and particle instruments onboard Pioneer 10, 11, Voyager 1 and 2.

Theoretical study on plasma wind and convection in Jovian magnetodisc.