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An analysis of the data from the Wind and IMP-8 spacecraft revealed that a slow solar wind, flowing in the heliospheric plasma sheet, represents a set of magnetic tubes with plasma of increased density (N > 10cm-3 at the Earth’s orbit). They have a fine structure at several spatial scales (fractality), from 2°-3°(at the Earth’s orbit, it is equivalent to 3.6-5.4h, or (5.4-8.0)×106km) to the minimum about 0.025°, i.e. the angular size of the nested tubes is changed nearly by two orders of magnitude. The magnetic tubes at each observed spatial scale are diamagnetic, i.e. their surface sustains a flow of diamagnetic (or drift) current that decreases the magnetic field within the tube itself and increases it outside the tube. Furthermore, the value of β= 8π[N(Te + Tp)]/B2 within the tube exceeds the value of βoutside the tube. In many cases total pressure P = N(Te + Tp) + B2/8πis almost constant within and outside the tubes at any one of the aforementioned scales.
An analysis of the data from the Wind and IMP-8 spacecraft revealed that a slow solar wind, flowing in the heliospheric plasma sheet, represents a set of magnetic tubes with plasma of increased density (N> 10 cm-3 at the Earth’s orbit). They have a fine structure at several spatial scales (fractality), from 2 ° -3 ° (at the Earth’s orbit, it is equivalent to 3.6-5.4 h, or (5.4-8.0) × 106 km) to the minimum about 0.025 °, ie the angular size of the nested tubes is shifted nearly by two orders of magnitude. The magnetic tubes at shifted every spatial axis are the magnetic field within the tube itself In addition, the value of β = 8π [N (Te + Tp)] / B2 within the tube exceeds the value of βoutside the tube. In many cases total pressure P = N (Te + Tp) + B2 / 8πis almost constant within and outside the tubes at any one of the scales scales.