A Comparison between Coronal Emission Lines from an Isothermal Spectrum Observed with the Coronal Diagnostic Spectrometer and CHIANTI Emissivities

2002 ◽  
Vol 574 (1) ◽  
pp. 495-503 ◽  
Author(s):  
E. Landi ◽  
U. Feldman ◽  
K. P. Dere
Keyword(s):  
Emission Lines ◽  
Coronal Emission ◽  
Coronal Diagnostic Spectrometer

Long-term Cyclic Variations of Prominences, Green and Red Coronae over Solar Cycles

2000 ◽  
Vol 179 ◽  
pp. 201-204
Author(s):  
Vojtech Rušin ◽  
Milan Minarovjech ◽  
Milan Rybanský
Keyword(s):  
Emission Lines ◽  
High Latitudes ◽  
Green Line ◽  
Solar Cycles ◽  
The South ◽  
Coronal Emission ◽  
Local Maxima ◽  
The North ◽  
Cyclic Variations

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.

The Origin of Coronal Emission Lines.

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

Near infrared spectral and polarization imaging observation of coronal emission lines during the 2008 total solar eclipse

2009 ◽  
Vol 52 (11) ◽  
pp. 1794-1798 ◽  
Author(s):  
XingMing Bao ◽  
ZhiYong Zhang ◽  
Jian Deng ◽  
KeLiang Hu ◽  
WeiJia Xuan ◽  
...  
Keyword(s):  
Solar Eclipse ◽  
Near Infrared ◽  
Total Solar Eclipse ◽  
Emission Lines ◽  
Coronal Emission ◽  
Polarization Imaging ◽  
Imaging Observation ◽  
Infrared Spectral

Complex Variations in the Line-Intensity Ratio of Coronal Emission Lines with Height above the Limb

2004 ◽  
Vol 617 (1) ◽  
pp. L81-L84 ◽  
Author(s):  
Jagdev Singh ◽  
Takashi Sakurai ◽  
Kiyoshi Ichimoto ◽  
Tetsuya Watanabe
Keyword(s):  
Line Intensity ◽  
Intensity Ratio ◽  
Emission Lines ◽  
Coronal Emission ◽  
Line Intensity Ratio

scholarly journals Non-thermal broadening of coronal emission lines in the onset phase of solar flares and CMEs

2006 ◽  
Vol 447 (2) ◽  
pp. 719-725 ◽  
Author(s):  
H. R. M. Kay ◽  
S. A. Matthews ◽  
L. K. Harra ◽  
J. L. Culhane
Keyword(s):  
Solar Flares ◽  
Emission Lines ◽  
Coronal Emission ◽  
Onset Phase

scholarly journals A Search for Coronal Emission Lines from Early-Type Stars

1988 ◽  
Vol 132 ◽  
pp. 123-125
Author(s):  
D. Baade ◽  
L. B. Lucy
Keyword(s):  
Stellar Wind ◽  
Controversial Issue ◽  
Emission Lines ◽  
Stellar Winds ◽  
Early Type ◽  
Wind Model ◽  
Coronal Emission ◽  
Early Type Stars ◽  
Hot Corona

For more than ten years now, a controversial issue in studies of stellar winds has concerned the existence or not of a coronal zone (T ∼ 106 K) at the base of the cool winds (T ∼ Teff) of early-type stars. The latest revival of interest in this possibility is due to Wolfire et al. (1985) who showed that Waldron's (1984) recombination stellar wind (RSW) version of the hot corona – cool wind model (Hearn 1975; Cassinelli et al. 1978) yields models for ξ Puppis (O4 If) that are consistent with both IRAS and Einstein IPC data, thus refuting an earlier claim (Lamers et al. 1984) to have excluded the existence of a coronal zone.

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