scholarly journals Heliolatitudinal and time variations of the solar wind mass flux: Inferences from the backscattered solar Lyman-alpha intensity maps

2013 ◽  
Vol 118 (6) ◽  
pp. 2800-2808 ◽  
Author(s):  
O. A. Katushkina ◽  
V. V. Izmodenov ◽  
E. Quemerais ◽  
J. M. Sokół
Keyword(s):  
Solar Wind ◽  
Mass Flux ◽  
Lyman Alpha ◽  
Time Variations

Saturn's E, G and F rings: modulated by the plasma sheet

1984 ◽  
Vol 75 ◽  
pp. 597
Author(s):  
E. Grün ◽  
G.E. Morfill ◽  
T.V. Johnson ◽  
G.H. Schwehm
Keyword(s):  
Solar Wind ◽  
Direct Contact ◽  
Transport Processes ◽  
Time Variable ◽  
Dust Particles ◽  
Spatial Diffusion ◽  
Drag Forces ◽  
Orbit Perturbation ◽  
Time Variations ◽  
F Ring

ABSTRACTSaturn's broad E ring, the narrow G ring and the structured and apparently time variable F ring(s), contain many micron and sub-micron sized particles, which make up the “visible” component. These rings (or ring systems) are in direct contact with magnetospheric plasma. Fluctuations in the plasma density and/or mean energy, due to magnetospheric and solar wind processes, may induce stochastic charge variations on the dust particles, which in turn lead to an orbit perturbation and spatial diffusion. It is suggested that the extent of the E ring and the braided, kinky structure of certain portions of the F rings as well as possible time variations are a result of plasma induced electromagnetic perturbations and drag forces. The G ring, in this scenario, requires some form of shepherding and should be akin to the F ring in structure. Sputtering of micron-sized dust particles in the E ring by magnetospheric ions yields lifetimes of 102to 104years. This effect as well as the plasma induced transport processes require an active source for the E ring, probably Enceladus.

Observations of a sky Lyman α groove related to enhanced solar wind mass flux in the neutral sheet

1996 ◽  
Vol 23 (25) ◽  
pp. 3675-3678 ◽  
Author(s):  
Jean-Loup Bertaux ◽  
Eric Quémerais ◽  
Rosine Lallement
Keyword(s):  
Solar Wind ◽  
Mass Flux ◽  
Neutral Sheet

SWAN: A study of Solar Wind Anisotropies on SOHO with Lyman alpha sky mapping

Solar Physics ◽  
1995 ◽  
Vol 162 (1-2) ◽  
pp. 403-439 ◽  
Author(s):  
J. L. Bertaux ◽  
E. Kyr�l� ◽  
E. Qu�merais ◽  
R. Pellinen ◽  
R. Lallement ◽  
...  
Keyword(s):  
Solar Wind ◽  
Lyman Alpha

scholarly journals The contribution of X-ray polar blowout jets to the solar wind mass and energy

2013 ◽  
Vol 8 (S300) ◽  
pp. 239-242 ◽  
Author(s):  
Giannina Poletto ◽  
Alphonse C. Sterling ◽  
Stefano Pucci ◽  
Marco Romoli
Keyword(s):  
Solar Wind ◽  
Kinetic Energy ◽  
Energy Budget ◽  
Coronal Mass Ejections ◽  
Mass Flux ◽  
Large Scale ◽  
Coronal Holes ◽  
Magnetic Loop ◽  
Small Scale ◽  
X Ray

AbstractBlowout jets constitute about 50% of the total number of X-ray jets observed in polar coronal holes. In these events, the base magnetic loop is supposed to blow open in what is a scaled-down representation of two-ribbon flares that accompany major coronal mass ejections (CMEs): indeed, miniature CMEs resulting from blowout jets have been observed. This raises the question of the possible contribution of this class of events to the solar wind mass and energy flux. Here we make a first crude evaluation of the mass contributed to the wind and of the energy budget of the jets and related miniature CMEs, under the assumption that small-scale events behave as their large-scale analogs. This hypothesis allows us to adopt the same relationship between jets and miniature-CME parameters that have been shown to hold in the larger-scale events, thus inferring the values of the mass and kinetic energy of the miniature CMEs, currently not available from observations. We conclude our work estimating the mass flux and the energy budget of a blowout jet, and giving a crude evaluation of the role possibly played by these events in supplying the mass and energy that feeds the solar wind.

scholarly journals Study of the solar wind coupling to the time difference horizontal geomagnetic field

2005 ◽  
Vol 23 (5) ◽  
pp. 1949-1957 ◽  
Author(s):  
P. Wintoft
Keyword(s):  
Solar Wind ◽  
Standard Deviation ◽  
Geomagnetic Field ◽  
Network Models ◽  
Number Density ◽  
Neural Network Models ◽  
Proton Number ◽  
Solar Wind Magnetic Field ◽  
Field Fluctuations ◽  
Time Variations

Abstract. The local ground geomagnetic field fluctuations (Δ B) are dominated by high frequencies and 83% of the power is located at periods of 32 min or less. By forming 10-min root-mean-square (RMS) of Δ B a major part of this variation is captured. Using measured geomagnetic induced currents (GIC), from a power grid transformer in Southern Sweden, it is shown that the 10-min standard deviation GIC may be computed from a linear model using the RMS Δ X and Δ Y at Brorfelde (BFE: 11.67° E, 55.63° N), Denmark, and Uppsala (UPS: 17.35° E, 59.90° N), Sweden, with a correlation of 0.926±0.015. From recurrent neural network models, that are driven by solar wind data, it is shown that the log RMS Δ X and Δ Y at the two locations may be predicted up to 30 min in advance with a correlation close to 0.8: 0.78±0.02 for both directions at BFE; 0.81±0.02 and 0.80±0.02 in the X- and Y-directions, respectively, at UPS. The most important inputs to the models are the 10-min averages of the solar wind magnetic field component Bz and velocity V, and the 10-min standard deviation of the proton number density σn. The average proton number density n has no influence. Keywords. Magnetospheric physics (Solar wind - magnetosphere interactions) – Geomagnetism and paleomagnetism (Rapid time variations)

scholarly journals Solar wind, mass and momentum losses during the solar cycle

2010 ◽  
Vol 6 (S271) ◽  
pp. 395-396
Author(s):  
R. Pinto ◽  
S. Brun ◽  
L. Jouve ◽  
R. Grappin
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Wind Speed ◽  
Mass Flux ◽  
Solar Minimum ◽  
Momentum Flux ◽  
Loss Rate ◽  
Convection Zone ◽  
Mass Loss Rate ◽  
Good Agreement

AbstractWe study the connections between the sun's convection zone evolution and the dynamics of the solar wind and corona. We input the magnetic fields generated by a 2.5D axisymmetric kinematic dynamo code (STELEM) into a 2.5D axisymmetric coronal MHD code (DIP). The computations were carried out for an 11 year cycle. We show that the solar wind's velocity and mass flux vary in latitude and in time in good agreement with the well known time-latitude assymptotic wind speed diagram. Overall sun's mass loss rate, momentum flux and magnetic breaking torque are maximal near the solar minimum.

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