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Title: Solar wind flow about the terrestrial planets 2. Comparison with gas dynamic theory and implications for solar-planetary interactions

Abstract

This study utilizes gas dynamic calculations in conjunction with observational bow shock models to investigate the solar wind flow patterns about the terrestrial planets. Average dayside bow shock position could be predicted for the earth by theory with an error of only approx.2%, given the observed shape and location of the magnetopause. Accordingly, our findings confirm the validity of the single-fluid gas dynamic approximation for describing this major aspect of solar wind flow past the earth. Modeled using gas dynamic theory, the solar wind interactions with Venus and Mars exhibit very significant differences. At Mars the mean inferred altitude of the solar wind-obstacle interface varies from 510 km at the stagnation point to almost 1000 km near the terminator. The effective magnetic moment required to produce a magnetosphere of this size for average solar wind dynamic pressures and terrestrial-type internal current systems is 1.4 +- 0.6 x 10/sup 22/ G cm/sup 3/. Gas dynamic modeling of the January 21, 1972, Mars 3 and July 20, 1976, Viking 1 lander particles and fields observations supports the conclusion that the Martian obstacle to the solar wind lies at altitudes too high for it to be associated with only an ionospheric or atmosphericmore » interaction. In contrast with Mars, our modeling of the Venus observations has found that the bow wave is closer to the planet than would be expected for a purely ionospheric obstacle. The subsolar width of the Venus ionosheath in the Venera and PVO measurements is only 60% and 90%, respectively, of that predicted by the gas dynamic model. This result is attributed to the presence of solar wind-neutral atmosphere interactions in the lower ionosheath that are not included in the gas dynamic code.« less

Authors:
; ; ; ;
Publication Date:
Research Org.:
NRC-NASA Resident Research Associate, Jet Propulsion Laboratory California Institute of Technology, Pasadena, California 91109
OSTI Identifier:
5909793
Resource Type:
Journal Article
Journal Name:
J. Geophys. Res.; (United States)
Additional Journal Information:
Journal Volume: 88:A1
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; MAGNETOPAUSE; SOLAR WIND; MARS PLANET; PLANETARY MAGNETOSPHERES; VENUS PLANET; MAGNETIC FIELD CONFIGURATIONS; PLANETARY IONOSPHERES; ATMOSPHERES; PLANETARY ATMOSPHERES; PLANETS; SOLAR ACTIVITY; 640107* - Astrophysics & Cosmology- Planetary Phenomena; 640203 - Atmospheric Physics- Magnetospheric Phenomena- (-1987)

Citation Formats

Slavin, J A, Holzer, R E, Spreiter, J R, Stahara, S S, and Chaussee, D S. Solar wind flow about the terrestrial planets 2. Comparison with gas dynamic theory and implications for solar-planetary interactions. United States: N. p., 1983. Web. doi:10.1029/JA088iA01p00019.
Slavin, J A, Holzer, R E, Spreiter, J R, Stahara, S S, & Chaussee, D S. Solar wind flow about the terrestrial planets 2. Comparison with gas dynamic theory and implications for solar-planetary interactions. United States. https://doi.org/10.1029/JA088iA01p00019
Slavin, J A, Holzer, R E, Spreiter, J R, Stahara, S S, and Chaussee, D S. 1983. "Solar wind flow about the terrestrial planets 2. Comparison with gas dynamic theory and implications for solar-planetary interactions". United States. https://doi.org/10.1029/JA088iA01p00019.
@article{osti_5909793,
title = {Solar wind flow about the terrestrial planets 2. Comparison with gas dynamic theory and implications for solar-planetary interactions},
author = {Slavin, J A and Holzer, R E and Spreiter, J R and Stahara, S S and Chaussee, D S},
abstractNote = {This study utilizes gas dynamic calculations in conjunction with observational bow shock models to investigate the solar wind flow patterns about the terrestrial planets. Average dayside bow shock position could be predicted for the earth by theory with an error of only approx.2%, given the observed shape and location of the magnetopause. Accordingly, our findings confirm the validity of the single-fluid gas dynamic approximation for describing this major aspect of solar wind flow past the earth. Modeled using gas dynamic theory, the solar wind interactions with Venus and Mars exhibit very significant differences. At Mars the mean inferred altitude of the solar wind-obstacle interface varies from 510 km at the stagnation point to almost 1000 km near the terminator. The effective magnetic moment required to produce a magnetosphere of this size for average solar wind dynamic pressures and terrestrial-type internal current systems is 1.4 +- 0.6 x 10/sup 22/ G cm/sup 3/. Gas dynamic modeling of the January 21, 1972, Mars 3 and July 20, 1976, Viking 1 lander particles and fields observations supports the conclusion that the Martian obstacle to the solar wind lies at altitudes too high for it to be associated with only an ionospheric or atmospheric interaction. In contrast with Mars, our modeling of the Venus observations has found that the bow wave is closer to the planet than would be expected for a purely ionospheric obstacle. The subsolar width of the Venus ionosheath in the Venera and PVO measurements is only 60% and 90%, respectively, of that predicted by the gas dynamic model. This result is attributed to the presence of solar wind-neutral atmosphere interactions in the lower ionosheath that are not included in the gas dynamic code.},
doi = {10.1029/JA088iA01p00019},
url = {https://www.osti.gov/biblio/5909793}, journal = {J. Geophys. Res.; (United States)},
number = ,
volume = 88:A1,
place = {United States},
year = {Sat Jan 01 00:00:00 EST 1983},
month = {Sat Jan 01 00:00:00 EST 1983}
}