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The coronal green line monitoring: a traditional but powerful tool for coronal physics

Published online by Cambridge University Press:  27 November 2018

Yu Liu  and
Xuefei Zhang
Yu Liu
Affiliation:
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China email: [email protected]
Xuefei Zhang
Affiliation:
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China email: [email protected] University of Chinese Academy of Sciences, Beijing 100049, China
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Abstract

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The particular environment with high temperature and low plasma density in the corona results to the formation of some forbidden emission lines, in which the well-known green line at 530.3 nm has been utilized to diagnose the corona for a few decades. For the green line, besides its contribution on revealing the long-term coronal cycles as well as their relationship to the other solar phenomena, it is also helpful to detect limb coronal waves and ejections originated from the lower corona which seems not to be paid close attention to. Suggestions are presented that we not only need to keep the green line observation as a routine task for current coronagraph observations, but need to develop larger coronagraphs with advanced technology.

Keywords

Coronamagnetic fieldssunspotsemission lines
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 169 - 170
Copyright
Copyright © International Astronomical Union 2018 

References

Badalyan, O., Obridko, V., & Sýkora, J., 2001, Sol. Phys., 199, 421Google Scholar
Bludova, N. G., 2005, Astron. Astrophys. Transactions, 24, 39Google Scholar
Habbal, S., Druckmüller, M., Morgan, , et al. 2010, ApJ, 719, 1362Google Scholar
Ichimoto, K., Noguchi, M., Tanaka, N., et al. 1999, PASJ, 51, 383Google Scholar
Liu, Y., Song, T., Zhang, X., et al. 2016, IAU Symp., 320, 447Google Scholar
Ozguc, A. & Ucer, C., 1987, Sol. Phys., 114, 141Google Scholar
Sakurai, T., 1998, ASPC Seri., 140, 483Google Scholar
Sakurai, T. & Suematsu, Y., 2002, Adv. Space Research, 29, 1565Google Scholar
Sakurai, T., 2004, Adv. Space Research, 34, 297Google Scholar
Sýkora, J., 1992a, Sol. Phys., 140, 379Google Scholar
Sýkora, J., 1992b, Contr. of the Astron. Obser. Skalnate Pleso, 22, 55Google Scholar
Sýkora, J. & Rybák, J., 2010, Solar Phys., 261, 321Google Scholar