Abstract
The interaction (oblique collision) of two ion acoustic solitons (IASs) in a magnetized relativistic degenerate plasma with relativistic degenerate electrons and non-degenerate cold ions is studied. The extended Poincaré–Lighthill–Kuo (PLK) method is used to obtain two Korteweg deVries (KdV) wave equations that describe the interacting IASs, then the phase shifts due to interaction are calculated. We studied influence of the fluid number density on the interaction process, interacting solitons phase shifts and also phase velocities. The introduced model is valid for astrophysical objects with high density matter such as white dwarfs, neutron stars, degenerate electrons gas in metals and laboratory degenerate plasma. An inverse proportionality between the phase shifts, phase velocity and the equilibrium electron fluid number density n_{eo} was established in the range 10^{35},{text {m}}^{-3}>n_{eo}>10^{38},{text {m}}^{-3}. We found that the soliton waves get sharper (narrower) and higher with increasing the electrons fluid number density n_{eo}, and hence less spacial occupying. The phase shifts and the phase velocity remain approximately unchanged in the range of 10^{35},{text {m}}^{-3}<n_{eo}<10^{38},{text {m}}^{-3}. The impact of the obliqueness angle theta on the soliton interaction process is also studied.
Highlights
The interaction of two ion acoustic solitons (IASs) in a magnetized relativistic degenerate plasma with relativistic degenerate electrons and non-degenerate cold ions is studied
In order to get the phase shifts resulting from the oblique collision process, we suppose that the two solitons S1 and S2 are at the initial time (t = −∞ ) asymptotically far from each other such that soliton S1 is at ξ = 0 and η = −∞ while soliton S2 is at η = 0 and ξ = +∞
The impact of equilibrium electrons fluid number density neo on the phase velocity is introduced in Fig. 7, in which it is found that an inverse proportionality between the phase velocity and neo which is similar to the range that was presented in Fig. 5 which is between neo ≈ 1035 m−3 to 1038 m−3, on the other hand for the range 1035 m−3 > neo > 1038 m−3 the phase velocity tends to be nearly unchanged against neo specially for higher values of obliqueness angle θ
Summary
In the existence of a static external magnetic field B = Bozalong z direction with the unit vector zsuch that Bo is the magnetic field strength, considering the movement of ion acoustic (IA) excitations in a relativistic degenerate plasma. We consider a two component degenerate relativistic plasma composed of ions and electrons. Introducing the normalized set of governing equations that were adopted from[34] as follows:. This system has been declared with ni and ne represent the fluid number density for ions and electrons, respectively, ui and ue are their fluids velocity. Me and e denote the electron mass and charge respectively, mi is the ion mass, c is the speed of light and γj =
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
