Electron-scale Kelvin-Helmholtz Instability In Magnetized Shear Flows

Electron-scale Kelvin-Helmholtz instabilities (ESKHI) are present in several astrophysical situations. Naturally ESKHI is topic to a background magnetic area, however an analytical dispersion relation and an correct growth charge of ESKHI below this circumstance are lengthy absent, as former MHD derivations aren't applicable within the relativistic regime. We current a generalized dispersion relation of ESKHI in relativistic magnetized shear flows, with few assumptions. ESKHI linear growth rates in certain circumstances are numerically calculated. We conclude that the presence of an exterior magnetic area decreases the maximum instability development charge usually, but can barely increase it when the shear velocity is sufficiently high. Also, the exterior magnetic discipline ends in a larger cutoff wavenumber of the unstable band and will increase the wavenumber of probably the most unstable mode. PIC simulations are carried out to confirm our conclusions, where we additionally observe the suppressing of kinetic DC magnetic discipline generation, ensuing from electron gyration induced by the external magnetic area. Electron-scale Kelvin-Helmholtz instability (ESKHI) is a shear instability that takes place at the shear boundary where a gradient in velocity is present.



Despite the significance of shear instabilities, ESKHI was solely recognized recently (Gruzinov, 2008) and remains to be largely unknown in physics. KHI is stable below a such condition (Mandelker et al., 2016). These make ESKHI a promising candidate to generate magnetic fields in the relativistic jets. ESKHI was first proposed by Gruzinov (2008) in the limit of a chilly and collisionless plasma, the place he also derived the analytical dispersion relation of ESKHI progress price for symmetrical shear flows. PIC simulations later confirmed the existence of ESKHI (Alves et al., 2012), finding the generation of typical electron vortexes and magnetic subject. It is noteworthy that PIC simulations additionally found the generation of a DC magnetic area (whose common along the streaming route will not be zero) in firm with the AC magnetic field induced by ESKHI, while the previous shouldn't be predicted by Gruzinov. The technology of DC magnetic fields is due to electron thermal diffusion or mixing induced by ESKHI throughout the shear interface (Grismayer et al., 2013), which is a kinetic phenomenon inevitable in the settings of ESKHI.



A transverse instability labelled mushroom instability (MI) was also discovered in PIC simulations regarding the dynamics in the plane transverse to the velocity shear (Liang et al., 2013a; Alves et al., 2015; Yao et al., 2020). Shear flows consisting of electrons and positrons are also investigated (Liang et al., 2013a, b, 2017). Alves et al. ESKHI and numerically derived the dispersion relation within the presence of density contrasts or clean velocity Wood Ranger Power Shears website (Alves et al., 2014), which are both found to stabilize ESKHI. Miller & Rogers (2016) prolonged the idea of ESKHI to finite-temperature regimes by contemplating the stress of electrons and derived a dispersion relation encompassing each ESKHI and MI. In pure situations, ESKHI is commonly subject to an exterior magnetic discipline (Niu et al., 2025; Jiang et al., 2025). However, works mentioned above were all carried out in the absence of an exterior magnetic discipline. While the speculation of fluid KHI has been prolonged to magnetized flows a long time in the past (Chandrasekhar, Wood Ranger Power Shears website 1961; D’Angelo, 1965), the habits of ESKHI in magnetized shear flows has been slightly unclear.



To date, the only theoretical concerns concerning this downside are introduced by Che & Zank (2023) and Tsiklauri (2024). Both works are restricted to incompressible plasmas and some sort of MHD assumptions, that are solely valid for small shear velocities. 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Wood Ranger Power Shears order now] electric power shears Shears USA their conclusions cannot be instantly applied in the relativistic regime, where ESKHI is expected to play a big function (Alves et al., 2014). Simulations had reported clear discrepancies from their idea (Tsiklauri, cordless electric power shears shears 2024). As Tsiklauri highlighted, a derivation of the dispersion relation without excessive assumptions is critical. This varieties a part of the motivation behind our work. In this paper, we will consider ESKHI under an external magnetic subject by instantly extending the works of Gruzinov (2008) and Alves et al. 2014). Because of this our work is carried out in the limit of chilly and collisionless plasma. We undertake the relativistic two-fluid equations and keep away from any form of MHD assumptions. The paper is organized as follows. In Sec. 1, we current a quick introduction to the background and topic of ESKHI.