Speaker
Description
Jupiter possesses the most hazardous radiation belt in the solar system which is responsible of trapping ultra-relativistic protons (~ 100 GeV), electrons (~ 100 MeV) and heavy ions like $O^+$, $O^{++}$, $S^+$, $S^{++}$, $S^{+++}$ (~100 MeV). Depending on the energy of the charged particles and the strength of Jupiter's magnetic field, these particles are either lost or trapped as they enter Jupiter's magnetic field. Once trapped in radiation belts, these particles gyrate along the magnetic field lines, bounce along the mirror points, and drift around the Jupiter. Since charged particles found in Jupiter's radiation belt are highly energetic, it is yet unknown whether they exhibit adiabatic or non-adiabatic behaviour. Several theoretical models exist to track the position of the particle, but they are all based on the gyro-centre approximation and are only applicable to charged particles that behave adiabatically. However, we do find charged particles with MeV-GeV ranges in Jupiter's radiation belts where the gyro-center approach may fail due to their larger gyro radius. In this context, we have developed a three-dimensional relativistic model using test particle simulation including all the three motions by incorporating Jupiter's magnetic field (intrinsic + current source) to examine the behaviour of these energetic charged particles. Furthermore, we found a proxy that involves perpendicular velocity and ambient magnetic field, to predict the adiabatic or non-adiabatic behaviour of the charged particles trapped in Jupiter's radiation belts.
