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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 ,
H. Lin ,
P. Lamy ,
S. Koutchmy  and
R. N. Smartt
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

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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 ⊙.

Keywords

eclipsesinfrared: starsinterplanetary mediumSun: corona
Type
Part 2: Infrared Observations of the 1991 Total Solar Eclipse
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 185 - 197
Copyright
Copyright © Kluwer 1994 

References

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