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A Synthesized Method for Solving the 180° Ambiguity of Solar Transverse Magnetic Field

Published online by Cambridge University Press:  12 April 2016

Wang Huaning  and
Lin Yuanzhang
Wang Huaning
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences
Lin Yuanzhang
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences

Extract

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The 180° ambiguity of the transverse magnetic field measured by a heliomagnetograph is an intrinsic problem due to the linear polarization in Zeeman effect(Harvey, 1969). Thus we have to make use of some criteria for calibrating the transverse magnetic fields in vector magnetograms. Up to now, a few criteria have been suggested by some solar physicists (Harvey, 1969; Krall et al., 1982; Sakurai et al., 1985; Aly, 1989; Wu and Ai, 1990; Canfield et al., 1991. The existing criteria could be classified as observational criteria and mathematical criteria. The former is based on the observation facts, such as the fibrils and the filaments in solar filtergrams, and the latter is derived from the mathematical model of solar magnetic field, such as divergence equation (∆. B = 0), potential field model and force-free field model. These criteria, however, are not applicable to all solar active regions, especially to those with complicated magnetic fields. For this reason, we suggest a synthesized method for calibrating the transverse magnetic fields in solar vector magnetograms.

Type
Session 7. Magnetic Shear and Electric Currents
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 461 - 464
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Ai, G. and Hu, Y. 1986, Publ. Beijing Astron. Obs. 8, 1.Google Scholar
Ai, G., Li, w., and Zhang, H. 1982, Acta Astron. Sinica 23, 39.Google Scholar
Aly, J.J. 1989, Solar Physics, 120, 19 CrossRefGoogle Scholar
Canfield, R. C., Fan, Y., Leka, K.D., McClymont, A.N., Wülser, J., Lites, B.W., and Zirin, H. 1991, in Solar Polarimetry, ed. November, L., NSO/SP Summer Workshop Series No. 11, p. 296.Google Scholar
Harvey, J.W. 1969, NCAR Cooperative Thesis No.17, University of Colorado, Boulder, Colorado.Google Scholar
Krall, K.R., Smith, J.B. Jr., Hagyard, M.J., West, E.A., and Cummings, N.P. 1982, Solar Physics 79, 59.Google Scholar
Ming, C., Han, F., Zhang, H., Ai, G., Kong, F. 1988, Acta Astron. Sinica, 29, 346 Google Scholar
Sakurai, T., Makita, M., and Shibasaki, K. 1985, in Theoretical Problems in High Resolution Solar Physics, ed. Schmidt, H. U., MPA, 212, 313.Google Scholar
Wu, L. and Ai, G. 1990, Acta Astrophys. Sinica, 10, 371 Google Scholar
Zhang, H. 1986, Acta Astron. Sinica, 27, 217 Google Scholar