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| Titel |
Radial and latitudinal dependencies of discontinuities in the solar wind between 0.3 and 19 AU and -80° and +10° |
| VerfasserIn |
A. Söding, F. M. Neubauer, B. T. Tsurutani, N. F. Ness, R. P. Lepping |
| Medientyp |
Artikel
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| Sprache |
Englisch
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| ISSN |
0992-7689
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| Digitales Dokument |
URL |
| Erschienen |
In: Annales Geophysicae ; 19, no. 7 ; Nr. 19, no. 7, S.667-680 |
| Datensatznummer |
250014279
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| Publikation (Nr.) |
 copernicus.org/angeo-19-667-2001.pdf |
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| Zusammenfassung |
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 νsw
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 ω over the transition evolves to an increase of
smaller ω with increasing distance from the sun. The evolution is
yielded by the anisotropic RDs with small ω. 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 [υ] parallel to [B / ρ], which is required by the MHD theory for RDs. The DDs have strongly enhanced
values of proton gyro radius rg for ω ~ 90°. In
contrast, in the inner heliosphere, only a small increase in rg with
ω is observed.
Key words. Interplanetary physics
(discontinuities; interplanetary magnetic fields) – Space plasma physics
(discontinuities) |
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