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The formation of an equatorial coronal hole

Published online by Cambridge University Press:  26 February 2010

Liheng Yang ,
Yunchun Jiang  and
Jun Zhang
Liheng Yang
Affiliation:
National Astronomical Observatories/Yunnan Observatory, CAS, Kunming 650011, China email: yangliheng@ynao.ac.cn
Yunchun Jiang
Affiliation:
National Astronomical Observatories/Yunnan Observatory, CAS, Kunming 650011, China email: yangliheng@ynao.ac.cn
Jun Zhang
Affiliation:
National Astronomical Observatories, CAS, Beijing 100012, China
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Abstract

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The formation of an equatorial coronal hole (CH) from 2006 January 9 to 12 was simultaneously observed by GOES-12/SXI, SOHO/EIT and SOHO/MDI instruments. The varieties of soft X-ray and EUV brightness, coronal temperature, and total magnetic flux in the CH were examined and compared with that of a quiet-sun (QS) region nearby. The following results are obtained. (1) A preexisting dark lane appeared on the location of the followed CH and was reinforced by three enhanced networks. (2) The CH gradually formed in about 81 hours and was predominated by positive magnetic flux. (3) During the formation, the soft X-ray and EUV brightness, coronal temperature, and total magnetic flux obviously decreased in the CH, but were almost no change in the QS region. The decrease of the total magnetic flux may be the result of magnetic reconnection between the open and closed magnetic lines, probably indicating the physical mechanism for the birth of the CH.

Keywords

Sun: coronaSun:evolutionSun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S264: Solar and Stellar Variability: Impact on Earth and Planets , August 2009 , pp. 295 - 297
Copyright
Copyright © International Astronomical Union 2010

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