Results 151 to 160 of about 205 (182)

The solar origins of solar wind interstream flows: Near‐equatorial coronal streamers

Journal of Geophysical Research: Space Physics, 1981
Vela heavy ion and IMP solar wind data are used to identify the coronal origins of the interstream, low‐speed solar wind as well as to understand the causes of the long‐term trends in solar wind densities and electron temperatures observed at 1 AU. Several lines of evidence suggest a strong association between interstream flows and the extensions of ...
W. C. Feldman, J. R. Asbridge, S. J. Bame, E. E. Fenimore, J. T. Gosling   +4 more
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Model of solar wind flow near an equatorial coronal streamer

AIP Conference Proceedings, 1999
In a previous work (1) we developed a semiempirical axisymmetric and magnetostatic model of the minimum activity corona, accounting for the gas pressure gradient effects on the magnetic structure. The model is able to reproduce the streamer belt closed region and the streamer surrounding open field lines, predicting high plasma β values (>1) in the ...
A. M. Vásquez, A. A. van Ballegooijen, J. C. Raymond   +2 more
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Analysis of an elongated narrow coronal streamer observed at the 1973 solar eclipse

Solar Physics, 1986
A detailed photometric analysis has been made of a narrow elongated coronal streamer observed at the 1973 total eclipse. After deriving real intensity distributions, the electron density has been deduced under the assumption that the distribution is axially symmetric and that the decrease in density from the central axis follows the gaussian law.
Hugo E. Trigoso, Tokio Tsubaki
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The origin of the slow solar wind in coronal streamers

Advances in Space Research, 2004
Abstract The highly variable slow solar wind has been associated with low-latitude regions of the heliosphere most clearly by the Ulysses spacecraft. Although, it is evident today that the slow solar wind originates in coronal helmet streamers, the mechanism of the slow solar wind acceleration, and the origin of the variability are still being ...
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Solar coronal streamers observed at 169 MHz with the Nan�ay East-West radioheliograph

Solar Physics, 1971
The slowly varying component of the Sun at 169 MHz for the period August 1962 to March 1966 has been studied, using daily data from the East West radioheliograph at Nancay.
F. Axisa, Y. Avignon, M. J. Martres, M. Pick, P. Simon   +4 more
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Non-radial coronal streamers in the course of the solar cycle

Astronomy Reports, 2009
Equatorward deviations of coronal streamers at solar minima and poleward deviations at solar maxima are interpreted as the effects of changes in the general topology of the global solar magnetic field. The streamer axis is located on the neutral surface of the radial magnetic field Br = 0, and the neutral surfaces deviate toward the field null points ...
openaire   +1 more source

STRUCTURE OF SOLAR CORONAL STREAMERS

1992
ABSTRACT We present here a new numerical method for solving generalized potential problems. The method is a direct method, effectively a shooting method, working outwards from an O-point, under the assumption that flux surfaces exist. The standard difficulties encountered in calculating equilibria with vanishing flux gradients, such as neutral sheets
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An estimate of solar wind velocity profiles in a coronal hole and a coronal streamer area (6–40 R[sub ☉])

AIP Conference Proceedings, 1996
Using the total electron content data obtained by the Ulysses Solar Corona Experiment during the first solar conjunction in summer 1991 (Bird et al., 1994), an estimate is presented of solar wind velocity profiles in a coronal hole and a coronal streamer area in the range between 6 and 40 solar radii.
M. Pätzold, B. T. Tsurutani, M. K. Bird   +2 more
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Numerical MHD modeling of the solar driver for the destabilization of a coronal helmet streamer

Advances in Space Research, 1997
Abstract We investigate the forms of the solar driver which cause the destabilization of helmet streamers. Two forms of solar drivers are considered; (i) emergence of a flux-rope from sub-photospheric levels and (ii) application of a photospheric shear motion to a streamer-flux rope system.
S.T. Wu, W.P. Guo
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Connections between the slow solar wind, CMES, and the helmet streamer belt inferred from coronal field models

AIP Conference Proceedings, 1999
The source region of the slow solar wind is complicated by the fact that it is apparently located at the boundary between the helmet streamer belt arcade and adjacent polar coronal holes. This location implies that it should occupy the same region of heliospheric space as transients associated with CMEs, and may in fact consist partly of slow ...
J. G. Luhmann, D. Larson, J. T. Hoeksema, X-P. Zhao, N. Arge, O. C. St. Cyr   +5 more
openaire   +1 more source