Evolution of the solar wind acceleration region during 1990–1994

1996 ◽  
Author(s):  
Munetoshi Tokumaru ◽  
Tetsuro Kondo ◽  
Hiroshi Takaba ◽  
Hirotaka Mori ◽  
Takashi Tanaka
1998 ◽  
Vol 103 (A4) ◽  
pp. 6571-6583 ◽  
Author(s):  
Y. Yamauchi ◽  
M. Tokumaru ◽  
M. Kojima ◽  
P. K. Manoharan ◽  
R. Esser

1996 ◽  
Vol 154 ◽  
pp. 49-56
Author(s):  
Shadia Rifai Habbal

AbstractThe temperature in the acceleration region of the solar wind remains one of the most elusive parameters to measure. Knowledge of the temperature as well as its gradient in the inner corona is fundamental for placing constraints on physical mechanisms thought to be responsible for the coronal heating process, as well as for understanding the flow properties of the solar wind. Estimates of the helium abundance is essential for understanding the puzzling behavior of heavier ions in the solar wind. As an illustration of the difficulties and uncertainties involved in the inferences of plasma parameters in the solar wind acceleration region, the inference of electron temperature and helium abundance will be described. Prospects for future observations will be briefly discussed.


1994 ◽  
Vol 420 ◽  
pp. 913 ◽  
Author(s):  
Espen Lyngdal Olsen ◽  
Egil Leer ◽  
Thomas E. Holzer

Author(s):  
George L. Withbroe ◽  
John L. Kohl ◽  
Heinz Weiser ◽  
Richard H. Munro

2014 ◽  
Vol 798 (1) ◽  
pp. 47 ◽  
Author(s):  
S. Giordano ◽  
J. C. Raymond ◽  
P. Lamy ◽  
M. Uzzo ◽  
D. Dobrzycka

1982 ◽  
Vol 33 (1-2) ◽  
pp. 17-52 ◽  
Author(s):  
George L. Withbroe ◽  
John L. Kohl ◽  
Heinz Weiser ◽  
Richard H. Munro

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