Observations of solar wind stream with high abundance of heavy ions and relation with coronal conditions

1981 ◽  
Vol 29 (11) ◽  
pp. 1235-1240 ◽  
Author(s):  
G.N Zastenker ◽  
Yu.I Yermolaev
1997 ◽  
Vol 102 (A8) ◽  
pp. 17419-17432 ◽  
Author(s):  
Xing Li ◽  
Ruth Esser ◽  
Shadia R. Habbal ◽  
You-Qiu Hu

2016 ◽  
Vol 116 (25) ◽  
Author(s):  
Patrick J. Tracy ◽  
Justin C. Kasper ◽  
Jim M. Raines ◽  
Paul Shearer ◽  
Jason A. Gilbert ◽  
...  

2009 ◽  
Vol 27 (8) ◽  
pp. 3089-3100 ◽  
Author(s):  
P. Janhunen

Abstract. An electric solar wind sail is a recently introduced propellantless space propulsion method whose technical development has also started. The electric sail consists of a set of long, thin, centrifugally stretched and conducting tethers which are charged positively and kept in a high positive potential of order 20 kV by an onboard electron gun. The positively charged tethers deflect solar wind protons, thus tapping momentum from the solar wind stream and producing thrust. The amount of obtained propulsive thrust depends on how many electrons are trapped by the potential structures of the tethers, because the trapped electrons tend to shield the charged tether and reduce its effect on the solar wind. Here we present physical arguments and test particle calculations indicating that in a realistic three-dimensional electric sail spacecraft there exist a natural mechanism which tends to remove the trapped electrons by chaotising their orbits and causing them to eventually collide with the conducting tethers. We present calculations which indicate that if these mechanisms were able to remove trapped electrons nearly completely, the electric sail performance could be about five times higher than previously estimated, about 500 nN/m, corresponding to 1 N thrust for a baseline construction with 2000 km total tether length.


2015 ◽  
Vol 33 (1) ◽  
pp. 47-53 ◽  
Author(s):  
L. Ofman ◽  
E. Provornikova ◽  
L. Abbo ◽  
S. Giordano

Abstract. Observations of streamers in extreme ultraviolet (EUV) emission with SOHO/UVCS show dramatic differences in line profiles and latitudinal variations in heavy ion emission compared to hydrogen Ly-α emission. In order to use ion emission observations of streamers as the diagnostics of the slow solar wind properties, an adequate model of a streamer including heavy ions is required. We extended a previous 2.5-D multi-species magnetohydrodynamics (MHD) model of a coronal streamer to 3-D spherical geometry, and in the first approach we consider a tilted dipole configuration of the solar magnetic field. The aim of the present study is to test the 3-D results by comparing to previous 2.5-D model result for a 3-D case with moderate departure from azimuthal symmetry. The model includes O5+ ions with preferential empirical heating and allows for calculation of their density, velocity and temperature in coronal streamers. We present the first results of our 3-D multi-fluid model showing the parameters of protons, electrons and heavy ions (O5+) at the steady-state solar corona with a tilted steamer belt. We find that the 3-D results are in qualitative agreement with our previous 2.5-D model, and show longitudinal variation in the variables in accordance with the tilted streamer belt structure. Properties of heavy coronal ions obtained from the 3-D model together with EUV spectroscopic observations of streamers will help understanding the 3-D structures of streamers reducing line-of-sight integration ambiguities and identifying the sources of the slow solar wind in the lower corona. This leads to improved understanding of the physics of the slow solar wind.


1987 ◽  
Vol 37 (6) ◽  
pp. 759-774 ◽  
Author(s):  
L. Avanov ◽  
N. Borodkova ◽  
Z. NĚmeček ◽  
A. Omeltchenko ◽  
J. Šafránková ◽  
...  

1996 ◽  
Vol 101 (A12) ◽  
pp. 27565-27571 ◽  
Author(s):  
Hironori Shimazu ◽  
Motohiko Tanaka ◽  
Shinobu Machida

1986 ◽  
Vol 13 (4) ◽  
pp. 411-414 ◽  
Author(s):  
T. R. Sanderson ◽  
K-P. Wenzel ◽  
P. Daly ◽  
S. W. H. Cowley ◽  
R. J. Hynds ◽  
...  
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