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1.5 μm Observations and the Depth of Sunspot Penumbrae

Published online by Cambridge University Press:  03 August 2017

S. K. Solanki ,
I. Rüedi ,
W. Livingston  and
H. U. Schmidt
S. K. Solanki
Affiliation:
Institute of Astronomy, ETH-Zentrum, CH-8092 Zürich, Switzerland
I. Rüedi
Affiliation:
Institute of Astronomy, ETH-Zentrum, CH-8092 Zürich, Switzerland
W. Livingston
Affiliation:
National Solar Observatory, NOAO,* P. O. Box 26732, Tucson, AZ 85726, U.S.A.
H. U. Schmidt
Affiliation:
Max-Planck-Institute of Astrophysics, Garching, Germany

Abstract

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The magnetic structure of a simple, relatively symmetric sunspot is determined using the extremely Zeeman sensitive Landé g = 3 line of Fe I at 1.5648 μm. From the measured strength and inclination of the magnetic field we estimate the fraction of the total magnetic flux of the sunspot passing through the solar surface in the penumbra. It is found that on average approximately 1/2–2/3 of the total magnetic flux of the spot emerges in the penumbra. Sunspot penumbrae are therefore deep, i.e., the τ = 1 level does not correspond to the lower magnetic boundary of the spot in its penumbra.

Keywords

infrared: starsSun: magnetic fieldssunspots
Type
Part 5: Magnetic Fields and Infrared Magnetometry
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 471 - 475
Copyright
Copyright © Kluwer 1994 

References

Beckers, J. M., Schröter, E. H.: 1969, Solar Phys. 10, 384.CrossRefGoogle Scholar
Deinzer, W.: 1965, Astrophys. J. 141, 548.CrossRefGoogle Scholar
Giovanelli, R. G.: 1982, Solar Phys. 80, 21.Google Scholar
Jahn, K.: 1989, Astron. Astrophys. 222, 264.Google Scholar
Kawakami, H.: 1983, Pub. Astron. Soc. Japan 35, 459.Google Scholar
Lites, B. W., Skumanich, A.: 1990, Astrophys. J. 348, 747.Google Scholar
Nordlund, Å, Stein, R. F.: 1989, in Rutten, R. J. and Severino, G. (eds.), Solar and Stellar Granulation, Kluwer Academic Publishers, Dordrecht, p. 453.Google Scholar
Pizzo, V. J.: 1986, Astrophys. J. 302, 785.Google Scholar
Schlüter, A., Temesvary, S.: 1958, in Lehnert, B. (ed.), ‘Electrodynamic Phenomena in Cosmical Physics’, IAU Symp. 6, 263.Google Scholar
Schmidt, H. U., Spruit, H. C., Weiss, N. O.: 1986, Astron. Astrophys. 158, 351.Google Scholar
Solanki, S. K., Schmidt, H. U.: 1992, Astron. Astrophys., submitted.Google Scholar
Solanki, , Rüedi, I., Livingston, W. 1992, Astron. Astrophys. 263, 312.Google Scholar
Wittmann, A. D.: 1974, Solar Phys. 36, 29.Google Scholar
Yun, H. S.: 1971, Solar Phys. 16, 398.Google Scholar