Radial and latitudinal dependencies of discontinuities in the solar wind between 0.3 and 19 AU and -80° and +10°

Details Radial and latitudinal dependencies of discontinuities in the solar wind between 0.3 and 19 AU and -80° and +10° Radial and latitudinal dependencies of discontinuities in the solar wind between 0.3 and 19 AU and -80° and +10°

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001angeo..19..681s&link_type=abstract

Annales Geophysicae, vol. 19, Issue 7, pp.681-686

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Directional discontinuities (DD) from 5 missions at 7 different locations between 0.3 and 19 AU and - 80° and + 10° in the 3D heliosphere are investigated during minimum solar activity. The data are surveyed using the identification criteria of Burlaga (1969) (B) and Tsurutani and Smith (1979) (TS). The rate of occurrence depends linearly on the solar wind velocity caused by the geometric effect of investigating a larger plasma volume if the solar wind velocity vsw increases. The radial dependence is proportional to r - 0.78 (TS criterion) and r - 1.28 (B criterion), respectively. This dependence is not only due to an increasing miss rate with increasing distance. The DDs must be unstable or some other physical effect must exist. After normalization of the daily rates to 400 km/s and 1 AU, no dependence on heliographic latitude or on solar wind structures is observable. This means that the DDs are uniformly distributed on a spherical shell. Normalized 64 DD per day are identified with both criteria. But large variations of the daily rate still occur, indicating that other influences must exist. The ratio of the rates of rotational (RDs) and tangential discontinuities (TDs) depends on the solar wind structures. In high speed streams, relatively more RDs exist than in low speed streams. In the inner heliosphere (r < 10 AU), no radial or latitudinal dependence of the portions of the DD types occur. 55% clear RDs, 10% clear TDs and 33% EDs (either discontinuities) are observed, but the portions differ with regard to the criteria used. In the middle heliosphere (10 AU< r < 40 AU), the DD types are more uniformly distributed. The distribution of the directional change over the transition evolves to an increase of smaller with increasing distance from the sun. The evolution is yielded by the anisotropic RDs with small . The spatial thickness dkm in kilometers increases with distance. The thickness drg normalized to the proton gyro radius decreases by a factor of 50 between 0.3 and 19 AU, from 201.3 rg down to 4.3 rg . In the middle heliosphere, the orientation of the normals relative to the local magnetic field is essentially uniform except for the parallel direction where no DDs occur. This indicates that RDs propagating parallel to B play a special role. In addition, in only a few cases is [ ] parallel to [ B/ ] , which is required by the MHD theory for RDs. The DDs have strongly enhanced values of proton gyro radius rg for ~ 90°. In contrast, in the inner heliosphere, only a small increase in rg with

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