The Corona Electropolarimetry during July 11, 1991 Solar Eclipse

1994 ◽  
Vol 144 ◽  
pp. 529-533 ◽  
Author(s):  
V. Kulidzanishvili ◽  
A. Mayer ◽  
V. Mayer ◽  
S. Danik
Keyword(s):  
Solar Corona ◽  
Solar Eclipse ◽  
Radial Direction ◽  
Polarization Plane ◽  
Polarization Degree ◽  
Plane Direction ◽  
Coronal Streamers ◽  
Academy Of Sciences

AbstractThe electropolarimetry of July 11, 1991 eclipse solar corona using the new photoelectric polarimeter of Abastumani Astrophysical Observatory of the Georgian Academy of Sciences, equipped with the IBM computer, is described in this paper.By means of measurable values the isopolarization lines were constructed, which turned out to be stretched along the coronal streamers. The polarization plane has, entirely, radial direction; however, small but real deviations from radiality were established. The errors of measurements of intensity, polarization degree and polarization plane direction are evaluated.

On the Optical Polarization of the White-Light Coronal Structures

1994 ◽  
Vol 144 ◽  
pp. 601-604
Author(s):  
B. P. Filippov ◽  
M. M. Molodensky ◽  
S. Koutchmy
Keyword(s):  
Solar Corona ◽  
White Light ◽  
Scattering Theory ◽  
Radial Direction ◽  
Polarization Plane ◽  
Solar Limb ◽  
Thomson Scattering ◽  
Optical Polarization ◽  
Special Experiment ◽  
Coronal Structures

AbstractA special experiment was designed to measure the orientation of the polarization plane in the solar corona during the total eclipse of July 11, 1991. Rotating polaroids with the axes directed at +45° and at −45° of the radial direction in all directions were used. The polarization plane was found to be tangential to the solar limb everywhere with an accuracy within 1°, in agreement with the Thomson scattering theory.

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.

scholarly journals Observations of the solar corona during the total solar eclipse on 21 August 2017

2017 ◽  
Vol 1 (1) ◽  
pp. 68-71 ◽  
Author(s):  
Hui Tian ◽  
◽  
ZhongQuan Qu ◽  
YaJie Chen ◽  
LinHua Deng ◽  
...  
Keyword(s):  
Solar Corona ◽  
Solar Eclipse ◽  
Total Solar Eclipse

Polarization neutral point pairs of the solar corona and the lunar disc observed during the total solar eclipse on 11 August 1999 in Hungary

2021 ◽  
Vol 60 (13) ◽  
pp. 3609
Author(s):  
Gábor Horváth ◽  
Judit Slíz-Balogh ◽  
István Pomozi ◽  
György Kriska
Keyword(s):  
Solar Corona ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Neutral Point

scholarly journals Properties of Different Coronal Streamers

2001 ◽  
Vol 203 ◽  
pp. 413-415
Author(s):  
S. Parenti ◽  
B. J. I. Bromage ◽  
G. Poletto ◽  
G. Noci ◽  
J. C. Raymond ◽  
...  
Keyword(s):  
Solar Corona ◽  
Ultra Violet ◽  
Physical Parameters ◽  
Altitude Range ◽  
Element Abundances ◽  
Coronal Streamers ◽  
Abundance Variation ◽  
Streamer Data ◽  
Different Altitudes ◽  
Coronal Diagnostic Spectrometer

In this paper a summary of results from coordinated observations of streamers acquired by the SOHO Coronal Diagnostic Spectrometer (CDS) and Ultra Violet Coronograph Spectrometer (UVCS) experiments is presented (Parenti et al. 2000). Data from different altitudes within the solar corona were taken, with the purpose of determining their physical parameters – densities, electron temperatures and element abundances – and their changes over the altitude range between 1.02 and 1.6 R⊙. Further UVCS streamer data, taken about two months later are used to compare with the behaviour seen in two different streamers. The streamers resulted to have a different behaviour in temperature and density. The low corona, covered by CDS data, shows little evidence of abundance variation with respect to photospheric values, while, at UVCS altitudes, a depletion of all element abundances is clearly evident.

Electron Temperatures and Flow Speeds of the Low Solar Corona: MACS Results from the Total Solar Eclipse of 29 March 2006 in Libya

Solar Physics ◽  
2011 ◽  
Vol 270 (1) ◽  
pp. 235-251 ◽  
Author(s):  
Nelson L. Reginald ◽  
Joseph M. Davila ◽  
O. C. St. Cyr ◽  
Douglas M. Rabin ◽  
Madhulika Guhathakurta ◽  
...  
Keyword(s):  
Solar Corona ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Flow Speeds

Residual Stress Measurements of 4H-SiC Crystals Using X-Ray Diffraction

2014 ◽  
Vol 778-780 ◽  
pp. 453-456 ◽  
Author(s):  
Masashi Nakabayashi ◽  
Tatsuo Fujimoto ◽  
Hiroshi Tsuge ◽  
Kiyoshi Kojima ◽  
Kozo Abe ◽  
...  
Keyword(s):  
Residual Stress ◽  
Temperature Distribution ◽  
Room Temperature ◽  
Radial Direction ◽  
Large Strain ◽  
Diffraction Method ◽  
X Ray Diffraction ◽  
X Ray ◽  
Plane Direction ◽  
Lateral Temperature

The room temperature residual stress of 4H-SiC wafers has been investigated using a precise X-ray diffraction method. A large strain was observed for the circumferential direction of wafers, more than ten times larger than those measured along the principal plane direction and the radial direction. Optimizing the lateral temperature distribution in growing crystals leads to reduction of residual stress of wafers with high crystal quality.

CCD polarimetry of the solar corona at the 1997-03-09 solar eclipse

1999 ◽  
Vol 23 (2) ◽  
pp. 221-228 ◽  
Author(s):  
Zhong-wei Hu ◽  
Ru-liang Li ◽  
Cheng Fang ◽  
Nai-yuan Xiao ◽  
Xiu-fa Gao
Keyword(s):  
Solar Corona ◽  
Solar Eclipse
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