A detailed examination of a X-line region in the distant tail: ISEE-3 observations of jet flow and B(sub z) reversals and a pair of slow shocks

Details A detailed examination of a X-line region in the distant tail: ISEE-3 observations of jet flow and B(sub z) reversals and a pair of slow shocks A detailed examination of a X-line region in the distant tail: ISEE-3 observations of jet flow and B(sub z) reversals and a pair of slow shocks

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994georl..21.3031h&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 21, no. 25, p. 3031-3034

Other

16

Flow Velocity, Geomagnetic Tail, Interplanetary Magnetic Fields, Magnetic Field Reconnection, Magnetic Signatures, Magnetohydrodynamic Flow, Plasma Jets, Satellite Observation, Shock Waves, Space Plasmas, Electron Density (Concentration), Electron Energy, International Sun Earth Explorer 3, Magnetic Measurement, Magnetic Storms, Mathematical Models, Rankine-Hugoniot Relation, Two Dimensional Flow

Scientific paper

We report an observation of Petschek-type magnetic reconnection at a distant neutral line (X = -230 R(sub e)) with a full set of signatures of the magnetic merging process. These features include a reversal of plasma flows from earthward to tailward, a pair of slow shocks and the magnetic field X-type line. These two slow shocks are shown to satisfy the shock criteria used by Feldman et al. (1987). The spacecraft first crosses a slow shock to enter the earthward flowing plasmasheet with velocity of about 440 km/s. The embedded magnetic field has a positive B(sub z) component. The spacecraft next enters a region of tailward plasma flow with speed approximately 670 km/s and an embedded negative B(sub z), indicating entry into the plasmasheet tailward of the X-line. These observed velocities are comparable to calculated velocities based on Rankine-Hugoniot conservation relationships. The spacecraft subsequently returns into the south tail lobe by crossing another slow shock. Coplanarity analyses shows that the two slow shocks have orientations consistent with that predicted by the Petschek reconnection model. We note that this event occurs during northward interplanetary magnetic fields. Thus, a magnetic stress built-up in the distant tail may be responsible for this reconnection process.

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