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Our final conclusion involving the importance of the shape of the current sheet for the substorm dynamics calls for further investigation.
If we estimate the spatial scale of the four current sheets from V timH multiplied by the crossing times, we obtain the thicknesses of the current sheet for each event: (1) 1310 km, (2) 710 km, (3) 140, and (4) 170 km. Figure 4a h shows magnetic field and plasma data from the low-energy particle instrument (LEP) (Mukai et al. 1994) from Geotail observations between 09 50 and 10 30 UT.
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with the calculated magnetic field structures and with the actual position of the heliospheric current sheet (as derived for the source surface at r = 2.5R⊙) is evident.
Using data on cosmic ray modulation parameter since 1951, we have estimated the evolution of the heliospheric current sheet tilt angle for the period 1951 1975, i.e., 25 years before regular observations of the tilt angle.
Rev. Letters, 83,4768, 1999) the author showed that current sheets in a low β plasma will be kinetically unstable with respect to Alfvén wave emission if the current sheet becomes sufficiently thin for the field-aligned electron flow to become super-Alfvenic.
A dipole tilt and/or current sheet crossings are unlikely causes for such periodic perturbations.
In this paper we will review the history of and evidence for the Current Sheet Disruption model, especially with regard to recent evidence in favor of the NENL model.
CS stands for the current sheet, and PSBL the plasma sheet boundary layer.
However, the directions of ion drift and current sheet motion were both Earthward/equatorward for the subsequent events (3) and (4), as is the case for a dipolarization front of Earthward convecting plasmas.
The simulation domain is LZ × LX = 4200 × 2100 cells = 40di × 20di (di is the ion inertial skin depth on the high-density side) for an asymmetric current sheet with no guide magnetic field.
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