Some newly discovered coronal emission lines from high altitude infrared observations of the 7 March, 1970, solar eclipse

Solar Physics ◽  
1971 ◽  
Vol 21 (2) ◽  
pp. 360-371 ◽  
Author(s):  
Kenneth H. Olsen ◽  
Charles R. Anderson ◽  
John N. Stewart
2009 ◽  
Vol 52 (11) ◽  
pp. 1794-1798 ◽  
Author(s):  
XingMing Bao ◽  
ZhiYong Zhang ◽  
Jian Deng ◽  
KeLiang Hu ◽  
WeiJia Xuan ◽  
...  

2000 ◽  
Vol 179 ◽  
pp. 201-204
Author(s):  
Vojtech Rušin ◽  
Milan Minarovjech ◽  
Milan Rybanský

AbstractLong-term cyclic variations in the distribution of prominences and intensities of green (530.3 nm) and red (637.4 nm) coronal emission lines over solar cycles 18–23 are presented. Polar prominence branches will reach the poles at different epochs in cycle 23: the north branch at the beginning in 2002 and the south branch a year later (2003), respectively. The local maxima of intensities in the green line show both poleward- and equatorward-migrating branches. The poleward branches will reach the poles around cycle maxima like prominences, while the equatorward branches show a duration of 18 years and will end in cycle minima (2007). The red corona shows mostly equatorward branches. The possibility that these branches begin to develop at high latitudes in the preceding cycles cannot be excluded.


Science ◽  
1992 ◽  
Vol 257 (5075) ◽  
pp. 1377-1380 ◽  
Author(s):  
P. Lamy ◽  
J. R. Kuhn ◽  
H. Lin ◽  
S. Koutchmy ◽  
R. N. Smartt

1964 ◽  
Vol 140 ◽  
pp. 1192 ◽  
Author(s):  
M. H. L. Pryce

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