Formation of the slow solar wind in a coronal streamer

1999 ◽  
Vol 104 (A1) ◽  
pp. 521-534 ◽  
Author(s):  
Giorgio Einaudi ◽  
Paolo Boncinelli ◽  
Russell B. Dahlburg ◽  
Judith T. Karpen
Keyword(s):  
Solar Wind ◽  
Slow Solar Wind ◽  
Coronal Streamer

scholarly journals Diamagnetic and Expansion Effects on the Observable Properties of the Slow Solar Wind in a Coronal Streamer

2005 ◽  
Vol 633 (1) ◽  
pp. 474-488 ◽  
Author(s):  
A. F. Rappazzo ◽  
M. Velli ◽  
G. Einaudi ◽  
R. B. Dahlburg
Keyword(s):  
Solar Wind ◽  
Slow Solar Wind ◽  
Coronal Streamer

scholarly journals Three-dimensional multi-fluid model of a coronal streamer belt with a tilted magnetic dipole

2015 ◽  
Vol 33 (1) ◽  
pp. 47-53 ◽  
Author(s):  
L. Ofman ◽  
E. Provornikova ◽  
L. Abbo ◽  
S. Giordano
Keyword(s):  
Solar Wind ◽  
Heavy Ions ◽  
Fluid Model ◽  
Slow Solar Wind ◽  
Streamer Belt ◽  
Lower Corona ◽  
Adequate Model ◽  
Coronal Streamer ◽  
Ion Emission ◽  
D Model

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.

scholarly journals Highly structured slow solar wind emerging from an equatorial coronal hole

Nature ◽  
2019 ◽  
Vol 576 (7786) ◽  
pp. 237-242 ◽  
Author(s):  
S. D. Bale ◽  
S. T. Badman ◽  
J. W. Bonnell ◽  
T. A. Bowen ◽  
D. Burgess ◽  
...  
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
Slow Solar Wind

scholarly journals A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND

2011 ◽  
Vol 731 (2) ◽  
pp. 112 ◽  
Author(s):  
S. K. Antiochos ◽  
Z. Mikić ◽  
V. S. Titov ◽  
R. Lionello ◽  
J. A. Linker
Keyword(s):  
Solar Wind ◽  
Slow Solar Wind

Elemental Fractionation in the Slow Solar Wind

1999 ◽  
Vol 521 (2) ◽  
pp. 859-867 ◽  
Author(s):  
N. A. Schwadron ◽  
L. A. Fisk ◽  
T. H. Zurbuchen
Keyword(s):  
Solar Wind ◽  
Slow Solar Wind ◽  
Elemental Fractionation
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