The elements that impact the dynamics and collaborations of waves and particles in the magnetosphere of planets have been considered here. Saturn’s internal magnetosphere is determined by substantiated instabilities and discovered to be an exceptional zone of wave activity. Interchanged instability is found to be one of the responsible events in view of temperature anisotropy and energization processes of magnetospheric species. The generated active ions alongside electrons that constitute the populations of highly magnetized planets like Saturn’s ring electron current are taken into consideration in the current framework. The previous and similar method of characteristics and the perturbed distribution function have been used to derive dispersion relation. In incorporating this investigation, the characteristics of electromagnetic ion cyclotron wave (EMIC) waves are determined by the composition of ions in plasmas through which the waves propagate. The effect of ring distribution illustrates non-monotonous description on growth rate (GR) depending upon plasma parameters picked out. Observations made by Cassini found appropriate for modern study, have been applied to the Kronian magnetosphere. Using Maxwellian ring distribution function of ions and detailed mathematical formulation, an expression for dispersion relation as well as GR and real frequency (RF) are evaluated. Analysis of plasma parameters shows that, proliferating EMIC waves are not developed much when propagation is parallelly aligned with magnetosphere as compared to waves propagating in oblique direction. GR for the oblique case, is influenced by temperature anisotropy as well as by alternating current (AC) frequency, whereas it is much affected only by AC frequency for parallel propagating waves.

1. INTRODUCTION
2. Ring distribution and Satellite’s flybys
3. EMPIRICAL DISPERSION MODEL
    3.1 Case I
    3.2 Case II
4. RESULTS AND DISCUSSION
    4.1 Important Magnetospheric Parameters
    4.2 Parallel and Oblique Propagation
5. CONCLUSION
ACKNOWLEDGMENTS
REFERENCES

• Kumari Neeta Shukla(Department of Applied Sciences, Manav Rachna International Institute of Research and Studies, Faridabad , Haryana, 121001, India)
• Jyoti Kumari(Department of Physics, Amity Institute of Applied Sciences, Amity University, Noida, Uttar Pradesh 201303, India)
• Rama Shankar Pandey(Department of Physics, Amity Institute of Applied Sciences, Amity University, Noida, Uttar Pradesh 201303, India) Corresponding author