Figure A5 is consistent with the conventional picture of the current density evolution during the substorm growth phase. The assumptions of the pressure balance and the Harris current sheet profile are avoided.
We want to hear from you. Know plasma, know 99.999% of the Universe (No plasma, no Universe). The use of the third criterion meant that we only applied equation 1 when the central plane of the current sheet and the magnetic equator were approximately parallel to the Z = 0 plane of the SM coordinates.
Our calculations show that the net MF is maximum in the near-edge region and in the between is weaker than other areas. The current density was sampled every 10 min to halve the number of observations to reduce any overlaps. For both observational and theoretical reasons, the potential causes of a bifurcated current sheet in the near‐Earth tail, where a typical plasma/current sheet is considerably thicker (say, a half thickness of 1 to 4 RE), seem to be absent. [2002] have proposed an idea of plasma sheet “aging,” where bifurcation appears during the late stage of current sheet thinning. The Cluster observations in the midtail also indicated the presence of a bifurcated current sheet during a flapping motion [e.g., Runov et al., 2003; Sergeev et al., 2003], while Tang et al. To examine their association with substorms, we referred to the THEMIS data of field, particle, and ground‐based auroral global images (http://themis.ssl.berkeley/edu/summary) and the time series data of geomagnetic indices from a substorm swift search (http://s‐cubed).
Equation 1 was used with this criterion to avoid a large error.
When I am taking log j (current density), I will not get any results as log (-) current can't be evaluated. Learn more.
A total of 3838 current density observations were obtained to study the vertical profile. Note that the plasma pressure is constant along the magnetic field lines because the pressure balance along the magnetic field line may be easily and quickly achieved owing to the high temperature. The exchange current density can be obtained from Tafel plot (log I vs. V, then extrapolate current to V = 0). We have supposed a washer (with the inner and outer radii a and b) carrying sub-critical currents subject to an applied magnetic field.
Figure 7 shows the average property of the near‐Earth current sheet for a tail structure. A high current density in the near‐Earth tail means that the formation of a single thin current sheet for typical solar wind dynamic pressures is unlikely. Its radial component goes down to zero on the z axes at the origin.
A north‐south symmetry was assumed throughout the present analysis. THEMIS observations from 2007 to 2013 allowed us to study the distribution of the cross‐tail current density in the near‐Earth tail (−8 > X > −12 RE).
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