The Effects of Solar Wind Structure on Nanodust Dynamics in the Inner Heliosphere

2020 ◽  
Vol 125 (10) ◽  
Author(s):  
A. R. Poppe ◽  
C. O. Lee
Keyword(s):  
Solar Wind ◽  
Wind Structure ◽  
Solar Wind Structure ◽  
Inner Heliosphere

scholarly journals Solar cycle changes of large-scale solar wind structure

2009 ◽  
Vol 5 (S264) ◽  
pp. 356-358 ◽  
Author(s):  
P. K. Manoharan
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Large Scale ◽  
Interplanetary Space ◽  
The Sun ◽  
Wind Structure ◽  
Level Of Activity ◽  
Solar Wind Structure ◽  
Current Minimum ◽  
Inner Heliosphere

AbstractIn this paper, I present the results on large-scale evolution of density turbulence of solar wind in the inner heliosphere during 1985–2009. At a given distance from the Sun, the density turbulence is maximum around the maximum phase of the solar cycle and it reduces to ~70%, near the minimum phase. However, in the current minimum of solar activity, the level of turbulence has gradually decreased, starting from the year 2005, to the present level of ~30%. These results suggest that the source of solar wind changes globally, with the important implication that the supply of mass and energy from the Sun to the interplanetary space has significantly reduced in the present low level of activity.

Structure and connectivity of CME-driven shocks and sheaths through the inner heliosphere

2021 ◽  
Author(s):  
Erika Palmerio ◽  
Christina Lee ◽  
Dusan Odstrcil ◽  
Leila Mays
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
The Sun ◽  
Interplanetary Shocks ◽  
Plasma Parameters ◽  
Wind Structure ◽  
Solar Wind Structure ◽  
Magnetohydrodynamic Simulations ◽  
Comprehensive Study ◽  
Inner Heliosphere

<p>The evolution of coronal mass ejections (CMEs) as they travel away from the Sun is one of the major issues in heliophysics and space weather. During propagation, CMEs and the structures ahead of them (i.e., interplanetary shocks and sheath regions, if present) are significantly affected by the ambient solar wind, which is able to alter their speed, trajectory, and orientation. The scarcity of multi-spacecraft measurements of the same CME, however, implies that little is known about how and where (in terms of distance from the Sun) these various processes exactly come into play.</p><p>To address this issue, we run a series of 3D magnetohydrodynamic simulations using the coupled solar–heliospheric WSA–Enlil model, in which we launch idealised CMEs as hydrodynamic (non-magnetised) structures. This allows us to focus on the evolution of CME-driven shocks and sheath regions through a multi-point study. We launch CMEs of various speeds through different solar wind backgrounds and at different heliolongitudes with respect to the streamer belt position. Then, we investigate the resulting magnetic field and plasma parameters at a series of synthetic spacecraft placed at various longitudes around the CME apex and at various heliocentric distances between 0.5 AU and 2 AU. We also analyse how the magnetic connectivity at these spacecraft evolves as the CME propagates. This work represents a comprehensive study of the interaction of CME-driven shocks and sheath regions with the large-scale solar wind structure throughout the inner heliosphere, with the aim to establish a range of expected behaviours and outcomes useful to interpret real events.</p>

Empirical inner boundary conditions and rotation rates for solar wind models

2021 ◽  
Author(s):  
Huw Morgan
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Boundary Conditions ◽  
Coronal Magnetic Field ◽  
Height Range ◽  
Rotation Rates ◽  
Wind Structure ◽  
Solar Wind Structure ◽  
Coronal Electron ◽  
Made In

<p>To date, the inner boundary conditions for solar wind models are either directly or indirectly based on magnetic field extrapolation models of the photosphere. Furthermore, between the photosphere and Earth, there are no other direct empirical constraints on models. New breakthroughs in coronal rotation tomography, applied to coronagraph observations, allow maps of the coronal electron density to be made in the heliocentric height range 4-12 solar radii (Rs). We show that these maps (i) give a new empirical boundary condition for solar wind structure at a height where the coronal magnetic field has become radial, thus avoiding the need to model the complex inner coronal magnetic field, and (ii) give accurate rotation rates for the corona, of crucial importance to the accuracy of solar wind models and forecasts.</p>

The Long Term Cosmic Ray Variation Relevant to Solar Wind Structure in the Outer Heliosphere

1990 ◽  
pp. 199-203
Author(s):  
M.V. Alania ◽  
R.G. Aslamazashvili ◽  
T.B. Bochorishvili ◽  
L.I. Dorman ◽  
R.T. Guschina ◽  
...  
Keyword(s):  
Solar Wind ◽  
Cosmic Ray ◽  
Outer Heliosphere ◽  
Wind Structure ◽  
Solar Wind Structure

Solar wind structure at 0.1-1 AU reconstructed from IPS observations using tomography

1997 ◽  
Author(s):  
M. Kojima ◽  
K. Asai ◽  
P. L. Hick ◽  
B. V. Jackson ◽  
M. Tokumaru ◽  
...  
Keyword(s):  
Solar Wind ◽  
Wind Structure ◽  
Solar Wind Structure

Large-scale solar-wind structure near the Sun detected by Doppler scintillation

Nature ◽  
1993 ◽  
Vol 366 (6455) ◽  
pp. 543-545 ◽  
Author(s):  
Richard Woo ◽  
Paul Gazis
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
The Sun ◽  
Wind Structure ◽  
Solar Wind Structure

scholarly journals Non‐dipolar solar wind structure observed in the cycle 23/24 minimum

2009 ◽  
Vol 36 (9) ◽  
Author(s):  
M. Tokumaru ◽  
M. Kojima ◽  
K. Fujiki ◽  
K. Hayashi
Keyword(s):  
Solar Wind ◽  
Wind Structure ◽  
Solar Wind Structure
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