The two-stream instability generation around Moon: Effect of Interplanetary Magnetic Field during Solar Wind - Lunar Plasma Interaction
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| Format: | Preprint |
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2026
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| _version_ | 1866910247758594048 |
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| author | Yadav, Vipin K. Singh, Abhinav Kumar, Rajneesh |
| author_facet | Yadav, Vipin K. Singh, Abhinav Kumar, Rajneesh |
| contents | The relative motion of two interpenetrating streams of charged particles usually leads to the generation of two stream instability (TSI) and eventually result in the onset of non-linear plasma processes such as the turbulence or the plasma waves. A natural example of such an event is the solar wind interaction with the lunar electron plasma where the interplanetary magnetic field (IMF) is embedded within the solar wind. The inclusion of IMF in the solar wind lunar plasma interaction modifies the dispersion relation of the TSI and an angular cyclotron frequency term appears in the denominator of the leading term and hence leads to the change in the parameters such as the instability growth rate as now it depends on the solar wind electron velocity, solar wind and the lunar electron plasma density, and the IMF magnitude. It is observed that the growth rate increases fast with the increase in the magnetic field initially but the increase slows down on further increasing the magnetic field thereby smoothening the top. From the particle in cell (PIC) simulations, it is observed that during the solar wind IMF interaction with lunar plasma, the non-energetic background electrons make a shield around the solar wind electrons in the vortices formed. It is further observed that those lunar electrons which are not participating either in the vortices formation or in the shielding of solar wind electrons, start moving in the direction of the incoming solar wind. These observations indicate this interaction is capable in getting converted into a non-linear physical process in the lunar plasma environment. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2605_23511 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | The two-stream instability generation around Moon: Effect of Interplanetary Magnetic Field during Solar Wind - Lunar Plasma Interaction Yadav, Vipin K. Singh, Abhinav Kumar, Rajneesh Plasma Physics The relative motion of two interpenetrating streams of charged particles usually leads to the generation of two stream instability (TSI) and eventually result in the onset of non-linear plasma processes such as the turbulence or the plasma waves. A natural example of such an event is the solar wind interaction with the lunar electron plasma where the interplanetary magnetic field (IMF) is embedded within the solar wind. The inclusion of IMF in the solar wind lunar plasma interaction modifies the dispersion relation of the TSI and an angular cyclotron frequency term appears in the denominator of the leading term and hence leads to the change in the parameters such as the instability growth rate as now it depends on the solar wind electron velocity, solar wind and the lunar electron plasma density, and the IMF magnitude. It is observed that the growth rate increases fast with the increase in the magnetic field initially but the increase slows down on further increasing the magnetic field thereby smoothening the top. From the particle in cell (PIC) simulations, it is observed that during the solar wind IMF interaction with lunar plasma, the non-energetic background electrons make a shield around the solar wind electrons in the vortices formed. It is further observed that those lunar electrons which are not participating either in the vortices formation or in the shielding of solar wind electrons, start moving in the direction of the incoming solar wind. These observations indicate this interaction is capable in getting converted into a non-linear physical process in the lunar plasma environment. |
| title | The two-stream instability generation around Moon: Effect of Interplanetary Magnetic Field during Solar Wind - Lunar Plasma Interaction |
| topic | Plasma Physics |
| url | https://arxiv.org/abs/2605.23511 |