Particle-In-Cell Simulations of Sunward and Anti-sunward Whistler Waves in the Solar Wind
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2023
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866910285858603008 |
|---|---|
| author | Kuzichev, Ilya V. Vasko, Ivan Y. Artemyev, Anton V. Bale, Stuart D. Mozer, Forrest S. |
| author_facet | Kuzichev, Ilya V. Vasko, Ivan Y. Artemyev, Anton V. Bale, Stuart D. Mozer, Forrest S. |
| contents | Spacecraft observations showed that electron heat conduction in the solar wind is probably regulated by whistler waves, whose origin and efficiency in electron heat flux suppression is actively investigated. In this paper, we present Particle-In-Cell simulations of a combined whistler heat flux and temperature anisotropy instability that can operate in the solar wind. The simulations are performed in a uniform plasma and initialized with core and halo electron populations typical of the solar wind. We demonstrate that the instability produces whistler waves propagating both along (anti-sunward) and opposite (sunward) to the electron heat flux. The saturated amplitudes of both sunward and anti-sunward whistler waves are strongly correlated with their {\it initial} linear growth rates, $B_{w}/B_0\sim (γ/ω_{ce})^ν$, where for typical electron betas we have $0.6\lesssim ν\lesssim 0.9$. The correlations of whistler wave amplitudes and spectral widths with plasma parameters (electron beta and temperature anisotropy) revealed in the simulations are consistent with those observed in the solar wind. The efficiency of electron heat flux suppression is positively correlated with the saturated amplitude of sunward whistler waves. The electron heat flux can be suppressed by 10--60% provided that the saturated amplitude of sunward whistler waves exceeds about 1% of background magnetic field. Other experimental applications of the presented results are discussed. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2303_18214 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Particle-In-Cell Simulations of Sunward and Anti-sunward Whistler Waves in the Solar Wind Kuzichev, Ilya V. Vasko, Ivan Y. Artemyev, Anton V. Bale, Stuart D. Mozer, Forrest S. Space Physics Solar and Stellar Astrophysics Plasma Physics Spacecraft observations showed that electron heat conduction in the solar wind is probably regulated by whistler waves, whose origin and efficiency in electron heat flux suppression is actively investigated. In this paper, we present Particle-In-Cell simulations of a combined whistler heat flux and temperature anisotropy instability that can operate in the solar wind. The simulations are performed in a uniform plasma and initialized with core and halo electron populations typical of the solar wind. We demonstrate that the instability produces whistler waves propagating both along (anti-sunward) and opposite (sunward) to the electron heat flux. The saturated amplitudes of both sunward and anti-sunward whistler waves are strongly correlated with their {\it initial} linear growth rates, $B_{w}/B_0\sim (γ/ω_{ce})^ν$, where for typical electron betas we have $0.6\lesssim ν\lesssim 0.9$. The correlations of whistler wave amplitudes and spectral widths with plasma parameters (electron beta and temperature anisotropy) revealed in the simulations are consistent with those observed in the solar wind. The efficiency of electron heat flux suppression is positively correlated with the saturated amplitude of sunward whistler waves. The electron heat flux can be suppressed by 10--60% provided that the saturated amplitude of sunward whistler waves exceeds about 1% of background magnetic field. Other experimental applications of the presented results are discussed. |
| title | Particle-In-Cell Simulations of Sunward and Anti-sunward Whistler Waves in the Solar Wind |
| topic | Space Physics Solar and Stellar Astrophysics Plasma Physics |
| url | https://arxiv.org/abs/2303.18214 |