Obliquely nonlinear solitary waves in magnetized electron–positron–ion plasma

This study focused on nonlinear ion-acoustic solitary structures (IASS) in a magnetized plasma system that is kappa distributed comprising electrons, positrons, and ions (e–p–i) using a fluid theory approach. A novel nonlinear inverse dispersion relation peculiar to this complex plasma environment was derived. The dispersive properties of ion-acoustic waves in magnetized e–p–i plasma environment were investigated considering the influence of various superthermal of electrons and positrons \((\kappa _{e}~\textrm{and} ~\kappa _{p})\) $({\kappa }_e\text{and}{\kappa }_p)$ , unperturbed positron to ion density ratio, p, electron to ion density ratio, \((\delta )\) $(\delta )$ , ion to electron temperature ratio, \((\sigma )\) $(\sigma )$ . By numerically analyzing the impact of plasma properties, particularly the nonlinear dispersion characteristics in a magnetized e–p–i plasma. The influence of the external magnetic field (obliqueness) angle, \(\theta\) $\theta$ , which alters the frequency value of \((\omega ^{2})\) $({\omega }^2)$ . It was found that the values of \(\delta\) $\delta$ , the frequency \(\omega ^{2}\) ${\omega }^2$ of IASS waves decreases with increasing \(\delta\) $\delta$ . This result has significant implications for understanding the dynamics of various astrophysical settings, such as the solar wind. However, when \(\delta > 0\) $\delta >0$ , the curves become more nonlinear, indicating the waves become more dispersive. Further, it is discovered that as the value of \(\theta\) $\theta$ for \(+~\omega ^{2}\) $+{\omega }^2$ solution increases, the shape of the dispersion curve does not significantly change. In contrast, it is observed from the \(-~\omega ^{2}\) $-{\omega }^2$ solution that for all values of angle \(\theta\) $\theta$ , frequency decreases with increasing angle \(\theta\) $\theta$ . This is because the ion-acoustic mode is strong at the propagation angle at \(\theta = 0^{\circ }\) $\theta =0^{\circ }$ and weakens as the propagation angle increases, eventually disappearing at \(\theta = 90^{\circ }\) $\theta ={90}^{\circ }$ . Thus, these findings provide an appreciable understanding of the dispersion characteristics of obliquely propagating IASS modes in a magnetized e–p–i plasma. In conclusion, our results provide important and new information on the interaction of plasma parameters in complex astronomical (natural) and laboratory (artificial) settings.