scholarly journals Temporal Observations of the λ5303 Emission Line Profile During the 74 Minute Totality from the Concorde SST at the 30 June 1973 Total Solar Eclipse: Preliminary Intensity Variations Above an Active Region

1974 ◽  
Vol 57 ◽  
pp. 485-487
Author(s):  
D. H. Liebenberg ◽  
M. M. Hoffman
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Solar Eclipse ◽  
Scattered Light ◽  
Total Solar Eclipse ◽  
Coronal Emission ◽  
Fabry Perot ◽  
Coronal Emission Line ◽  
Prime Objective ◽  
Scientific Laboratory

(Nature). Apparatus was flown aboard the French-British Concorde SST to obtain high resolution emission line intensity profiles during the 30 June 1973 total solar eclipse. A prime objective was to obtain profiles that could be used to determine the presence in the Fe xiv coronal emission line, 530.3 nm, of the 300 s periodicity such as is observed in the photosphere and chromosphere. The long totality duration of 74 min on the French Concorde 001 provided a unique opportunity for this study. At the 55000 ft cruise altitude weather influences are negligible, scattered light background reduced and seeing conditions excellent. The instrumentation included a high resolution pressure scanned Fabry-Perot interferometer and high resolution recordind. This instrumentation was perfected in earlier Los Alamos Scientific Laboratory solar eclipse flights since 1965 (Liebenberg, 1965, 1967; Hoffman et al., 1970). A 12 cm aperture window and 7.7 cm aperture f/13 telescope were designed to optimize the use of the available space as shown in Figure 1.

FeXIV Line Emission Polarization of the July 11, 1991 Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 541-547
Author(s):  
J. Sýkora ◽  
J. Rybák ◽  
P. Ambrož
Keyword(s):  
High Resolution ◽  
Solar Corona ◽  
Emission Line ◽  
Solar Eclipse ◽  
White Light ◽  
Preliminary Analysis ◽  
Line Emission ◽  
Total Solar Eclipse ◽  
Degree Of Polarization ◽  
High Resolution Images

AbstractHigh resolution images, obtained during July 11, 1991 total solar eclipse, allowed us to estimate the degree of solar corona polarization in the light of FeXIV 530.3 nm emission line and in the white light, as well. Very preliminary analysis reveals remarkable differences in the degree of polarization for both sets of data, particularly as for level of polarization and its distribution around the Sun’s limb.

Very High Resolution Analysis of the Dynamics of a Coronal Plasmoid

1994 ◽  
Vol 144 ◽  
pp. 593-596
Author(s):  
O. Bouchard ◽  
S. Koutchmy ◽  
L. November ◽  
J.-C. Vial ◽  
J. B. Zirker
Keyword(s):  
High Resolution ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Field Of View ◽  
Small Field ◽  
High Resolution Analysis ◽  
Ccd Observations ◽  
Resolution Analysis ◽  
Very High ◽  
Small Field Of View

AbstractWe present the results of the analysis of a movie taken over a small field of view in the intermediate corona at a spatial resolution of 0.5“, a temporal resolution of 1 s and a spectral passband of 7 nm. These CCD observations were made at the prime focus of the 3.6 m aperture CFHT telescope during the 1991 total solar eclipse.

Coronal emission line polarization

Solar Physics ◽  
1972 ◽  
Vol 23 (1) ◽  
pp. 103-119 ◽  
Author(s):  
Lewis L. House
Keyword(s):  
Emission Line ◽  
Coronal Emission ◽  
Coronal Emission Line

How bright is the [Si X] 1431 nm coronal emission line?

Solar Physics ◽  
1994 ◽  
Vol 151 (1) ◽  
pp. 51-56 ◽  
Author(s):  
M. J. Penn ◽  
J. R. Kuhn
Keyword(s):  
Emission Line ◽  
Coronal Emission ◽  
Coronal Emission Line

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

Fine Structures of the Inner Corona Observed at the 1991 Total Solar Eclipse

1994 ◽  
Vol 144 ◽  
pp. 565-566 ◽  
Author(s):  
A. Takeda ◽  
H. Kurokawa ◽  
R. Kitai ◽  
K. Ishiura
Keyword(s):  
High Resolution ◽  
Solar Eclipse ◽  
Baja California ◽  
Total Solar Eclipse ◽  
Emission Lines ◽  
Coronal Loops ◽  
Temperature Structure ◽  
Baja California Sur ◽  
High Resolution Images ◽  
Fine Structures

Extended AbstractThe Kwasan and Hida Observatories team (three of the authors but A. T.) observed the total solar eclipse of 11 July, 1991 with the multi-channel telescope at UABCS (Universidad Autonoma de Baja California Sur) campus in La Paz, Baja California Sur, Mexico. The primary purpose of our obsevation is to get high-resolution images of the inner corona at the wavelength of coronal emission lines and continuum shown in Table 1. Thanks to the clear sky and good seeing condition, we successfully got many images of high spatial resolution with photographic cameras and video recorders. Details of the observation have already been published by Kurokawaet al. (1992). In this paper, we present the results obtained from the photographic data reduction on fine structures of the inner corona. The procedure of photometrical measurement and image processing are fully described in another paper (Takeda, 1993).There have been published several observational works on the temperature structure of the coronal loops. Some authors proposed that hot coronal loops have cool cores (Foukal, 1975; Hanaokaet al., 1988), but others denied such coaxial models (Chenget al., 1980; Dere, 1982). Our high-resolution images obtained at the eclipse enables us to compare the positions of the loops seen in different emission lines of different ionization temperatures more precisely than any other previous observations. Main results are summarized as follows.

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