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Imaging coronal emission lines under high sky-background conditions

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Abstract

We have obtained images in solar coronal emission lines under high sky-background conditions by making precise differential measurements between the coronal emission line and the near-by continuum, which is primarily due to scattered light from the solar disk. Chopping between the two wavelengths was performed at 100 kHz to avoid artifacts from fast-flying dust particles and other aerosols, and also from seeing effects. The differential signal was detected with a novel CCD camera that demodulates signals up to 100 kHz. These preliminary observations show coronal emission at the 0.2% level of the scattered-light background and pave the way to efficient and precise imaging of coronal emission features under less than ideal ‘coronal-sky’ conditions.

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Authors and Affiliations

  1. National Solar Observatory, National Optical Astronomy Observatories, P.O.box 26732, 85726-6732, Tucson, AZ, U.S.A.

    C. U. Keller

  2. National Solar Observatory, National Optical Astronomy Observatories, P.O.Box 62, 88349-0062, Sunspot, NM, USA

    R. N. Smartt

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  1. C. U. Keller
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  2. R. N. Smartt
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Operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation.

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Keller, C.U., Smartt, R.N. Imaging coronal emission lines under high sky-background conditions. Sol Phys 166, 311–315 (1996). https://doi.org/10.1007/BF00149401

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  • DOI: https://doi.org/10.1007/BF00149401

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