LINEAR POLARIZATION OF FLASH SPECTRUM OBSERVED FROM A TOTAL SOLAR ECLIPSE IN 2008

2009 ◽  
Vol 695 (2) ◽  
pp. L194-L197 ◽  
Author(s):  
Z. Q. Qu ◽  
X. Y. Zhang ◽  
Z. K. Xue ◽  
G. T. Dun ◽  
S. H. Zhong ◽  
...  

1. General Arrangements . The expedition to observe the total solar eclipse of 1911, April 28, was organised by the Joint Permanent Eclipse Committee, the expenses being defrayed by the Government Grant Fund. Of the few islands in the South Pacific crossed by the track of the moon’s shadow during totality, Vavau, one of the northernmost group of the Tonga or Friendly Islands, was the most suitable for observing the eclipse, the duration of totality being computed at 217 seconds, and there being a reasonable prospect of good weather. The programme of observations consisted of photographs of the corona on a large and relatively small scale for coronal detail and extension of the streamers, and photographs of the spectrum of the corona and of the lower chromosphere. For these purposes the expedition was furnished with a 4-inch photographic lens of 20 feet focal length, kindly lent by the Council of the Royal Irish Academy, and the 4-inch Dallmeyer “Abney” lens of 34 inches focal length. For the spectrum of the corona Prof. Newall kindly lent the quartz spectroscope of four prisms, presented to the Cambridge Observatory by Major Hills, in order further to investigate the ultra-violet spectrum. The fourth instrument was made up of a large 7-inch prism of 40° in combination with a 6-inch Dallmeyer portrait lens of 30 inches focal length, This objective prismatic camera gave a short but very bright spectrum, 4⋅5 cm. from H α to H ζ . The intention was to investigate the red end of the coronal spectrum on dyed plates, and incidentally to photograph the flash spectrum. The members of the expedition were Father Cortie and Mr. W. McKeon, from the Stonyhurst College Observatory, and Father E. Pigot, Director of the Observatory of St. Ignatius’ College, Rivervievv, Sydney, N. S. W., who also acted as agent for the expedition in Sydney, in the preparation of huts to cover the instruments, and in the gathering of materials for building the piers for the foundations. The Admiralty gave instructions that H. M. S. “Encounter” should convey the observers and the instruments from Sydney to Vavau and back, and that every assistance should be rendered to the expedition in the erection of the instruments and in the observations. The expedition is greatly indebted to Captain Colomb, and to the officers and men of the “Encounter,” for their enthusiastic co-operation in the work of the expedition.


2009 ◽  
Vol 52 (11) ◽  
pp. 1799-1805 ◽  
Author(s):  
Hui Li ◽  
HaiSheng Ji ◽  
HouKun Ni ◽  
HaiYing Zhang ◽  
YaNan Zhang ◽  
...  

1994 ◽  
Vol 154 ◽  
pp. 173-178
Author(s):  
T. A. Clark ◽  
D. A. Naylor ◽  
G. J. Tompkins ◽  
C. Lindsey

Near IR total eclipse measurements have provided clear evidence during both 2nd and 3rd contacts for a limb extension of about 125 km for wavelengths in the range containing the CO fundamental vibration-rotation bands between 4.3 and 5.5 μm, when compared to the limb at nearby shorter wavelengths. This is interpreted as a “flash” spectrum in the CO lines, with the above extension representing the outer level of the CO emission layer. This height can be compared to the τCO = 1.0 level incorporated into recent representative atmospheric models (Ayres and Wiedemann, 1989) which is 90 km above the visible limb for a semi-empirical “hot chromosphere” model (Avrett, 1985) and 220 km for a “cool” radiative equilibrium model based upon work by Anderson (1989).


1954 ◽  
Vol 120 ◽  
pp. 94 ◽  
Author(s):  
R. Grant Athay ◽  
Donald E. Billings ◽  
John W. Evans ◽  
Walter O. Roberts

1994 ◽  
Vol 144 ◽  
pp. 593-596
Author(s):  
O. Bouchard ◽  
S. Koutchmy ◽  
L. November ◽  
J.-C. Vial ◽  
J. B. Zirker

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.


1994 ◽  
Vol 144 ◽  
pp. 541-547
Author(s):  
J. Sýkora ◽  
J. Rybák ◽  
P. Ambrož

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.


1917 ◽  
Vol 83 (2145supp) ◽  
pp. 93-93
Author(s):  
Edison Pettit

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

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