A mechanism for heating electrons in the magnetopause current layer and adjacent regions
- 1LPP-CNRS, UMR7648, Ecole Polytechnique, route de Saclay, 91128 Palaiseau cedex, France
- 2IGPP/ESS University of California, Los Angeles, CA, 90095-1567, USA
- 3Institut fur Geophysik und extraterrestrische Physik der Technischen University at Braunschweig, Mendelssohnstrasse 3, 38106 Braunschweig, Germany
- 4Space Sciences Laboratory, University of California, Berkeley, 7 Gauss Way, Berkeley, CA, 94720-7450, USA
- 5Department of Physics, Umeå University, Umeå, Sweden
- 6Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA
Abstract. Taking advantage of the string-of-pearls configuration of the five THEMIS spacecraft during the early phase of their mission, we analyze observations taken simultaneously in the magnetosheath, the magnetopause current layer and the magnetosphere. We find that electron heating coincides with ultra low frequency waves. It seems unlikely that electrons are heated by these waves because the electron thermal velocity is much larger than the Alfvén velocity (Va). In the short transverse scale (k⊥ρi >> 1) regime, however, short scale Alfvén waves (SSAWs) have parallel phase velocities much larger than Va and are shown to interact, via Landau damping, with electrons thereby heating them. The origin of these waves is also addressed. THEMIS data give evidence for sharp spatial gradients in the magnetopause current layer where the highest amplitude waves have a large component δB perpendicular to the magnetopause and k azimuthal. We suggest that SSAWs are drift waves generated by temperature gradients in a high beta, large Ti/Te magnetopause current layer. Therefore these waves are called SSDAWs, where D stands for drift. SSDAWs have large k⊥ and therefore a large Doppler shift that can exceed their frequencies in the plasma frame. Because they have a small but finite parallel electric field and a magnetic component perpendicular to the magnetopause, they could play a key role at reconnecting magnetic field lines. The growth rate depends strongly on the scale of the gradients; it becomes very large when the scale of the electron temperature gradient gets below 400 km. Therefore SSDAW's are expected to limit the sharpness of the gradients, which might explain why Berchem and Russell (1982) found that the average magnetopause current sheet thickness to be ~400–1000 km (~500 km in the near equatorial region).