تقرير
Magnetic field evolution and reconnection in low resistivity plasmas
| العنوان: | Magnetic field evolution and reconnection in low resistivity plasmas |
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| المؤلفون: | Boozer, Allen H. |
| سنة النشر: | 2022 |
| المجموعة: | Astrophysics Physics (Other) |
| مصطلحات موضوعية: | Physics - Plasma Physics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics |
| الوصف: | The mathematics and physics of each of the three aspects of magnetic field evolution -- topology, energy, and helicity -- is remarkably simple and clear. When the resistivity $\eta$ is small compared to an imposed evolution, $a/v$, timescale, which means $R_m\equiv\mu_0va/\eta>>1$, magnetic field line chaos dominates the evolution of field-line topology in three-dimensional systems. Chaos has no direct role in the dissipation of energy. A large current density, $j_\eta\equiv vB/\eta$, is required for energy dissipation to be on a comparable time scale to the topological evolution. Nevertheless, chaos plus Alfv\'en wave damping explain why both timescales tend to be approximately an order of magnitude longer than the evolution timescale $a/v$. Magnetic helicity is injected onto tubes of field lines when boundary flows have vorticity. Chaos can spread but not destroy magnetic helicity. Resistivity has a negligible effect on helicity accumulation when $R_m>>1$. Helicity accumulates within a tube of field lines until the tube erupts and moves far from its original location. Comment: arXiv admin note: text overlap with arXiv:2009.08779 by other authors |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.1063/5.0138805 |
| URL الوصول: | http://arxiv.org/abs/2212.07487 |
| رقم الأكسشن: | edsarx.2212.07487 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.1063/5.0138805 |
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