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Photospheric brightness differences associated with the solar supergranulation

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Abstract

The large scale (> 5000 km) intensity structure of the photosphere has been examined. The power per frequency unit indicates a continuous increase towards smaller spatial frequency. No excess power exists at wavelengths near the size of the supergranulation (30000 km) or at any other wavelength between 5000 and 100000 km. However, direct measurement of the intensity distribution in 1652 supergranulation cells shows a very small increase of the intensity towards the cell boundary. The amount of this increase is larger near the solar limb. It is probably due to a weak continuum emission associated with the chromospheric network. Any temperature difference arising from the supergranulation convection is obscured by this emission and is probably less than 1 K.

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Authors and Affiliations

  1. Sacramento Peak Observatory Air Force Cambridge Research Laboratories, Sunspot, N.M., U.S.A.

    Jacques M. Beckers

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  1. Jacques M. Beckers
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Beckers, J.M. Photospheric brightness differences associated with the solar supergranulation. Sol Phys 5, 309–322 (1968). https://doi.org/10.1007/BF00147143

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  • DOI: https://doi.org/10.1007/BF00147143

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