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Sunspot temperatures from red and blue photometry

Published online by Cambridge University Press:  26 August 2011

G. A. Chapman ,
A. M. Cookson  and
D. G. Preminger
G. A. Chapman
Affiliation:
San Fernando Observatory, CSU Northridge, Northridge, CA 91330, USA
A. M. Cookson
Affiliation:
San Fernando Observatory, CSU Northridge, Northridge, CA 91330, USA
D. G. Preminger
Affiliation:
San Fernando Observatory, CSU Northridge, Northridge, CA 91330, USA
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Abstract

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Photometric images are used to measure the temperature of sunspots at different wavelengths. Images at 672.3 nm and 472.3 nm are obtained at the San Fernando Observatory using the CFDT2 (2.5” x 2.5” pixels). Images at 607.1 nm and 409.4 nm are obtained by the PSPT at Mauna Loa Observatory. Monochromatic intensities are converted to temperatures as in Steinegger et al (1990). The pixel by pixel temperature for a sunspot is converted into a bolometric contrast for that sunspot according to Chapman et al (1994). Sunspot temperatures, i.e., their bolometric contrasts, are calculated from both red (672.3 nm) and blue wavelengths (472.3 nm) and compared.

Keywords

Sun: irradiancesun: temperature
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 325 - 327
Copyright
Copyright © International Astronomical Union 2011

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