Electron bulk heating in magnetic reconnection at Earth's magnetopause: Dependence on the inflow Alfvén speed and magnetic shear. Issue 17 (11th September 2013)

• Record Type: Journal Article
• Authors: Phan, T. D.; Shay, M. A.; Gosling, J. T.; Fujimoto, M.; Drake, J. F.; Paschmann, G.; Oieroset, M.; Eastwood, J. P.; Angelopoulos, V.
• Is Part Of: Geophysical research letters. Volume 40:Issue 17(2013:Sep.)
• Page Start: 4475
• Page End: 4480
• Publication Date: 2013-09-11
• Subjects: Geophysics -- Periodicals; Planets -- Periodicals; Lunar geology -- Periodicals; 550
• DOI: 10.1002/grl.50917
• Languages: English
• ISSNs: 0094-8276

Abstract

<abstract abstract-type="main"> <title>Abstract</title> <p id="grl50917-para-0001">[1] We surveyed 79 magnetopause reconnection exhausts detected by the THEMIS spacecraft to investigate how the amount and anisotropy of electron bulk heating produced by reconnection depend on the inflow boundary conditions. We find that the amount of heating, ΔT_e, is correlated with the asymmetric Alfvén speed, V_{AL, asym}, based on the reconnecting magnetic field and the plasma density measured in both the high‐density magnetosheath and low‐density magnetospheric inflow regions. Best fit to the data produces the empirical relation ΔT_e = 0.017 m_iV_{AL, asym}², indicating that the amount of heating is proportional to the inflowing magnetic energy per proton‐electron pair, with ~1.7% of the energy being converted into electron heating. This finding, generalized to symmetric reconnection, could account for the lack of electron heating in typical solar wind exhausts at 1 AU, as well as strong heating to keV energies common in magnetotail exhausts. We also find that the guide field suppresses perpendicular heating.</p> </abstract>