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• W2895923242 abstract "Magnetic reconnection is a well-known source of electron and ion bulk heating, as well as energetic particles, in the solar system. Several authors have suggested that reconnection occurs at the heliopause. The paper's primary focus is to predict the amount of electron and ion bulk heating for heliopause reconnection, using the empirical relations of T. Phan and colleagues between the changes in electron and ion temperature and an Alfven speed VA,asym,r. This Alfven speed depends on the strengths of the reconnecting magnetic fields and includes asymmetries in the magnetic fields and densities on the two inflowing sides of the reconnection region. For the undisturbed interstellar flow the predicted VA,asym,r ≈ 25 km/s and the predicted changes in electron and ion temperature are ΔTe1000 K and ΔTi6000 K. These changes are relatively small and likely not important for dynamics at the heliopause. However, a plasma depletion layer (PDL) is predicted beyond the heliopause, analogous to the PDLs observed sunwards of the magnetopauses of Earth, Mercury, Jupiter, and Saturn. In the PDL, the interstellar (ISM) magnetic field lines drape over the heliopause. Plasma ions and electrons with relatively large parallel temperatures escape along the field, increasing the field strength, decreasing the plasma density, and increasing the Alfven speed. In the region of the PDL where these effects are strong, the expected field and density changes are a factor of 4 and 1/4, respectively, increasing VA,asym,r by a factor close to 3 and the temperature changes by almost a factor of 10. Thus, heliopause reconnection in a strong PDL is predicted to increase the electron and ion temperatures by up to 104 K and 8 × 104 K, respectively, corresponding to changes by factors of order 1.5 and 11 compared to the predicted ISM temperature of ≈ 7500 K. Thus, the effects of bulk heating in heliopause reconnection regions will be most important for plasma inside or magnetically connected to the strong region of the heliopauses PDL. As an aside, Coulomb collisions appear too slow to relax the ion temperature anisotropies in the PDL beyond the heliopause, different than for the electrons." @default.
• W2895923242 created "2018-10-26" @default.
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• W2895923242 date "2018-10-01" @default.
• W2895923242 modified "2023-10-18" @default.
• W2895923242 title "Electron and ion heating due to magnetic reconnection at the heliopause" @default.
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• W2895923242 doi "https://doi.org/10.1088/1742-6596/1100/1/012004" @default.
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