Results 151 to 160 of about 2,675,738 (224)

Signature in the interplanetary medium for substorms

Journal of Geophysical Research, 1971
A detailed signature for individual substorms is sought in the interplanetary medium. Hourly values of interplanetary field and plasma parameters are correlated with hourly averages of the AE index. An interplanetary variable involving the southward component of the interplanetary field in the solar magnetospheric coordinate system is shown to be ...
R. Arnoldy
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The relationship between geomagnetic indices and the interplanetary medium parameters in magnetic storm main phases during CIR and ICME events

, 2020
This paper is a continuation of research (Boroyev and Vasiliev, 2018), in which the relationship of substorm indices both with the rate of storm development and electric field of the solar wind (SW) during the main phase of magnetic storms induced by CIR
R. N. Boroyev, M. Vasiliev, D. Baishev
semanticscholar   +1 more source

Slow shocks in the interplanetary medium

Journal of Geophysical Research, 1977
The production of MHD shock ensembles in the solar wind will, in general, result in slow forward and reverse shocks in addition to fast forward and reverse shocks and a contact discontinuity. As opposed to fast shocks, which last for an extended period of time, slow shocks disappear in two stages.
Philip Rosenau, S. T. Suess
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Ring current and interplanetary medium parameters

Studia Geophysica et Geodaetica, 1989
Based on hourly averaged data, the ring current decay parameter and the injection function associated with interplanetary medium parameters are analysed. The distinction among the decay parameter values during a magnetic storm has been carefully drawn, the dependence ofτ on the injection function during the main phase and on the DR variation during the
V. Yu. Pisarskij, Ya. I. Feldstein, N. M. Rudneva, A. Prigancová   +3 more
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H2 Enrichment of Interplanetary Medium

1982
Observational evidences show the presence in the solar system of interplanetary matter.A considerable contribution to the enrichment of dust and gas in the interplanetary medium is given through release by comets under the action of the solar radiation field and of its particle emission (solar wind,impulsive phenomena etc.).
PIRRONELLO, Valerio, Strazzulia G, Foti G.   +2 more
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Large-scale structure of the interplanetary medium

Solar Physics, 1973
We introduce a method for constructing large-scale (∼0.25 AU) interplanetary magnetic field lines using only solar wind velocity from well-separated appropriately located spacecraft. The technique is based on ‘labeling’ the field lines at each spacecraft with their coronal connection longitudes calculated in the EQRH (extrapolated quasi-radial ...
J. T. Nolte, E. C. Roelof
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Semiempirical Model of the Interplanetary Medium

Physical Review Letters, 1962
A model extending from the corona to about 5 astronomical units is presented. The interplanetary plasma expansion velocity run was inferred from comet-tail orientations in the cornet-orbit plane. The density run was computed from the continuity equation appropriate for spherical geometry. A relation between the velocity space anisotropy, mean expansion
John C. Brandt, Richard W. Michie
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Shock waves in the interplanetary medium

Planetary and Space Science, 1966
Shock waves in interplanetary medium caused by sudden expansion of solar corona following ...
M. Simon, W.I. Axford
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Sector boundary distortion in the interplanetary medium

Journal of Geophysical Research, 1977
We address the theoretical problem of the effect of a solar wind meridional velocity gradient on the orientation, or tipping, of a line embedded within the interplanetary plasma. We find that rotations of from 30degree to 75degree, between 1.5 solar radii and I AU, are produced when observed values for the solar wind velocity and its meridional ...
S. T. Suess, Joan Feynman
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Solar Wind and Interplanetary Medium

1977
Due to high temperature and more importantly a small temperature gradient with height the solar corona is not in hydrostatic equilibrium but is continuously expanding into interplanetary space. The resulting outflow of coronal plasma is known as the solar wind. Because of the very high electrical conductivity of the coronal plasma the magnetic field in
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