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IR Observations of the K and F Corona During the 1991 Eclipse

Published online by Cambridge University Press:  03 August 2017

J. R. Kuhn
Affiliation:
Michigan State University, East Lansing, MI 48824, U.S.A.
H. Lin
Affiliation:
Michigan State University, East Lansing, MI 48824, U.S.A.
P. Lamy
Affiliation:
Laboratoire d'Astronomie Spatiale, F-13012 Marseille, France
S. Koutchmy
Affiliation:
Institut d'Astrophysique, Boulevard Arago, F-75014 Paris, France
R. N. Smartt
Affiliation:
National Solar Observatory, Sunspot, NM 88349, U.S.A.

Abstract

The availability of relatively large format IR array detectors is incentive for reexamining the classic question of whether or not there are “dust rings” around the sun – a problem for which there are conflicting observational answers. The 1991 eclipse path included a high altitude observatory and provided a potentially ideal opportunity to study the infrared properties and dust content of the corona. Here we report results from an experiment conducted from Mauna Kea using a HgCdTe array detector sensitive to wavelengths between 1-2.5 μm. Surface brightness measurements in the H-band and polarization data in the J-band were obtained over a field-of-view of ±6 R while K-band images further extend to 15 R on the western side of the Sun. J-band polarization data and H and K-band surface brightness data clearly show the inhomogeneous structure in the K corona and the ecliptical flattening of the F corona. We see no evidence of a circumsolar, local dust corona (dust rings) out to 15 R .

Type
Part 2: Infrared Observations of the 1991 Total Solar Eclipse
Copyright
Copyright © Kluwer 1994 

References

Koutchmy, S. and Lamy, P.: 1985, in Giese, R.H. and Lamy, P. (eds.), Properties and Interactions of Interplanetary Dust, p. 63.Google Scholar
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