Synoptic maps of solar wind parameters from in situ spacecraft observations

Details Synoptic maps of solar wind parameters from in situ spacecraft observations Synoptic maps of solar wind parameters from in situ spacecraft observations

Publishing date

Mar 1995

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...100.3383g&link_type=abstract

Journals

Journal of Geophysical Research (ISSN 0148-0227), vol. 100, no. A3, p. 3383-3393

Science

Physics

Additional info 2

6

Additional info 3

Current Sheets, Evolution (Development), In Situ Measurement, Interplanetary Magnetic Fields, Solar Wind, Solar Wind Velocity, Temporal Distribution, Data Reduction, Dynamic Pressure, Explorer 50 Satellite, Kinetic Energy, Observation, Pioneer Venus Spacecraft, Plasma Temperature

Type

Scientific paper

Abstract

Solar wind observations from the Interplanetary Monitoring Platform-8 (IMP-8) and Pioneer Venus Orbiter (PVO) spacecraft from 1982 until 1988 are combined to construct synoptic maps of solar wind parameters near 1 AU. Each map consists of 6 months of hourly averaged solar wind data, binned by heliographic latitude and Carrington longitude and projected back to the Sun. These maps show the structure and time evolution of solar wind streams near 1 AU in the heliographic latitudes of +/- 7.25 deg and provide and explicit picture of several phenomena, such as gradients, changes in the inclination of the heliospheric current sheet, and the relative positions of various structures in the inner heliosphere, that is difficult to obtain from single-spacecraft observations. The stream structure varied significantly during the last solar cycle. Between 1982 and early 1985, solar wind parameters did not depend strongly on heliographic latitude. During the last solar minimum, the solar wind developed significant latitudinal structure, and high-speed streams were excluded from the vicinity of the solar equator. The interplanetary magnetic field was strongly correlated with the coronal field, and the current sheet tended to coincide with the coronal neutral line. The solar wind speed showed the expected correlations with temperature, interplanetary magnetic field, and distance from the current sheet. The solar wind speed was anticorrelated with density, but the regions of highest density occurred east of the heliospheric current sheet and the regions of lowest solar wind speed. This is consistent with compression at the leading edge of high-speed streams.

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