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Near Infrared Imaging Magnetometry

Published online by Cambridge University Press:  03 August 2017

Douglas Rabin
Douglas Rabin*
Affiliation:
National Solar Observatory, National Optical Astronomy Observatories,* P. O. Box 26732, Tucson, Arizona 85726, U.S.A.

Abstract

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Infrared array detectors are a new and promising tool for investigating the properties of magnetic field concentrations in the solar photosphere. Array measurements provide large statistical samples of polarized line profiles and display the spatial organization of the magnetic field. The wavelength region near 1.6 μm has important advantages for magnetometry: spectral lines with magnetic sensitivites ranging from low to very high; low continuum opacity; high continuum flux; and the possibility of sub-arcsecond angular resolution with existing telescopes. Initial results have extended earlier work on the distribution of field strength and flux in plages and revealed new properties specifically connected with spatial structure. The quality and flexibility of near infrared magnetographs can be expected to improve rapidly.

Keywords

flux tubesinfrared: starsinstrumentation: polarimetersSun: faculae, plagesSun: magnetic fields
Type
Part 5: Magnetic Fields and Infrared Magnetometry
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 449 - 457
Copyright
Copyright © Kluwer 1994 

References

Avrett, E. H., Chang, E. S., and Loeser, R.: 1993, these proceedings.Google Scholar
Deming, D., Boyle, R.J., Jennings, D.E., and Wiedemann, G.: 1988, Astrophys. J. 333, 978.CrossRefGoogle Scholar
Harvey, J. W.: 1977, in Müller, E. A. (ed.), Highlights of Astronomy 4, 223.CrossRefGoogle Scholar
Harvey, J. W., and Hall, D.: 1975, Bull. Amer. Astron. Soc. 7, 459.Google Scholar
Kopp, G., and Rabin, D.: 1993, these proceedings.Google Scholar
Lites, B. W., Elmore, D., Murphy, G., Skumanich, A., Tomczyk, S., and Dunn, R. B.: 1991, in November, L. (ed.), Solar Polarimetry, Proc. 11th Sacramento Peak Workshop, NSO, Sunspot, New Mexico, p. 3.Google Scholar
McPherson, M. R., Lin, H., and Kuhn, J. R.: 1992, Solar Phys. 139, 255.CrossRefGoogle Scholar
Rabin, D.: 1992a, Astrophys. J. (Letters) 390, L103.CrossRefGoogle Scholar
Rabin, D.: 1992b, Astrophys. J. 391, 832.CrossRefGoogle Scholar
Roddier, F., and Graves, J. E.: 1993, these proceedings.Google Scholar
Rüedi, I., Solanki, S. K., and Rabin, D. 1992, Astron. Astrophys. 261, L21.Google Scholar
Rutten, R. J., and Carlsson, M.: 1993, these proceedings.Google Scholar
Saar, S.: 1993, these proceedings.Google Scholar
Solanki, S. K.: 1993, these proceedings.Google Scholar
Spruit, H.: 1981, in Jordan, S. (ed.), The Sun as a Star, NASA SP-450, NASA, Washington, D.C., p. 385.Google Scholar
Steiner, O.: 1993, these proceedings.Google Scholar
Stenflo, J. O., Solanki, S. K., and Harvey, J. W.: 1987, Astron. Astrophys. 173, 167.Google Scholar
Zayer, I., Solanki, S. K., and Stenflo, J. O.: 1989, Astron. Astrophys. 211, 463.Google Scholar