Effects of ion magnetization on the Farley-Buneman instability in the solar chromosphere
Fletcher, Alex C.
Dimant, Yakov S.
Oppenheim, Meers M.
Fontenla, Juan M.
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Citation (published version)Alex C Fletcher, Yakov S Dimant, Meers M Oppenheim, Juan M Fontenla. 2018. "Effects of Ion Magnetization on the Farley-Buneman Instability in the Solar Chromosphere." ASTROPHYSICAL JOURNAL, Volume 857, Issue 2, 9 pp. https://doi.org/10.3847/1538-4357/aab71a
Intense heating in the quiet-Sun chromosphere raises the temperature from 4000 to 6500 K but, despite decades of study, the underlying mechanism remains a mystery. This study continues to explore the possibility that the Farley–Buneman instability contributes to chromospheric heating. This instability occurs in weakly ionized collisional plasmas in which electrons are magnetized, but ions are not. A mixture of metal ions generate the plasma density in the coolest parts of the chromosphere; while some ions are weakly magnetized, others are demagnetized by neutral collisions. This paper incorporates the effects of multiple, arbitrarily magnetized species of ions to the theory of the Farley–Buneman instability and examines the ramifications on instability in the chromosphere. The inclusion of magnetized ions introduces new restrictions on the regions in which the instability can occur in the chromosphere—in fact, it confines the instability to the regions in which heating is observed. For a magnetic field of 30 G, the minimum ambient electric field capable of driving the instability is 13.5 V/m at the temperature minimum.
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