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Microwave Depolarization above Sunspots

Published online by Cambridge University Press:  26 August 2011

Jeongwoo Lee
Affiliation:
Physics Department, New Jersey Institute of Technology, Newark, NJ 07102, U.S.A. email: [email protected]
Stephen M. White
Affiliation:
AFRL, Space Vehicles Directorate, Kirtland AFB, Albuquerque, NM 87117, U.S.A. email: [email protected]
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Abstract

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Microwave emissions from sunspots are circularly polarized in the sense of rotation (right or left) determined by the polarity (north or south) of coronal magnetic fields. However, they may convert into unpolarized emissions under certain conditions of magnetic field and electron density in the corona, and this phenomenon of depolarization could be used to derive those parameters. We propose another diagnostic use of microwave depolarization based on the fact that an observed depolarization strip actually represents the coronal magnetic polarity inversion line (PIL) at the heights of effective mode coupling, and its location itself carries information on the distribution of magnetic polarity in the corona. To demonstrate this diagnostic utility we generate a set of magnetic field models for a complex active region with the observed line-of-sight magnetic fields but varying current density distribution and compare them with the 4.9 GHz polarization map obtained with the Very Large Array (VLA). The field extrapolation predicts very different locations of the depolarization strip in the corona depending on the amount of electric currents assumed to exist in the photosphere. Such high sensitivity of microwave depolarization to the coronal magnetic field can therefore be useful for validating electric current density maps inferred from vector magnetic fields observed in the photosphere.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Alissandrakis, C. E., Borgioli, F., Chiuderi Drago, F., Hagyard, M., & Shibasaki, K. 1996, Solar Phys., 167, 167CrossRefGoogle Scholar
Alissandrakis, C. E., Chiuderi-Drago, F. 1994, ApJ, 428, 73CrossRefGoogle Scholar
Cohen, M. H. 1960, ApJ, 131, 664Google Scholar
Dalgarno, A. & Layzer, D. 1987, Spectroscopy of astrophysical plasmas, Cambridge U. Press, Cambridge and New YorkCrossRefGoogle Scholar
Dulk, G. A. & McLean, D. J. 1978, Solar Phys., 57, 279CrossRefGoogle Scholar
Kakinuma, T. & Swarup, G. 1962, ApJ, 136, 975Google Scholar
Kundu, M. R. & Alissandrakis, C. E. 1984, Solar Phys., 94, 249CrossRefGoogle Scholar
Lee, J., White, S. M., Kundu, M. R., Mikic, Z., & McClymont, A. N. 1998, Solar Phys., 180, 193CrossRefGoogle Scholar
Lin, H., Penn, M. J., & Tomczyk, S. 2000, ApJ, 541, L83CrossRefGoogle Scholar
Ratcliffe, J. A. 1959, The Magneto-ionic Theory and its Applications to the Ionosphere, Cambridge U. Press, CambridgeGoogle Scholar
Ryabov, B. I., Pilyeva, N. A., Alissandrakis, C. E., Shibasaki, K., Bogod, V. M., Garaimov, V. I., & Gelfreikh, G. B. 1999, Solar Phys., 185, 157CrossRefGoogle Scholar
Zirin, H. 1988, Astrophysics of the Sun, Cambridge U. Press, Cambridge and New YorkGoogle Scholar