The correlation between expansion speed and magnetic field in solar flare ribbons

Wenbin Xie; Haimin Wang; Ju Jing; Xingming Bao; Hongqi Zhang

doi:10.1007/s11433-009-0239-2

The correlation between expansion speed and magnetic field in solar flare ribbons

Wenbin Xie, Haimin Wang, Ju Jing, Xingming Bao, Hongqi Zhang

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1 Scopus citations

Abstract

In this paper, we study the correlation between the expansion speed of two-ribbon flares and the magnetic field measured in the ribbon location, and compare such correlation for two events with different magnetic configurations. These two events are: an M1.0 flare in the quiet sun on September 12, 2000 and an X2.3 flare in Active Region NOAA 9415 on April 10, 2001. The magnetic configuration of the M1.0 flare is simple, while that of X2.3 event is complex. We have derived a power-law correlation between the ribbon expansion speed (V _r ) and the longitudinal magnetic field (B _z ) with an empirical relationship V _r = A×B- _z ^-δ, where A is a constant and δ is the index of the power-law correlation. We have found that δ for the M1.0 flare in the simple magnetic configuration is larger than that for the X2.3 flare in the complex magnetic configuration.

Original language	English (US)
Pages (from-to)	1754-1759
Number of pages	6
Journal	Science in China, Series G: Physics, Mechanics and Astronomy
Volume	52
Issue number	11
DOIs	https://doi.org/10.1007/s11433-009-0239-2
State	Published - Nov 2009

All Science Journal Classification (ASJC) codes

Physics and Astronomy(all)

Keywords

Solar activity
Solar flares
Solar magnetic field

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10.1007/s11433-009-0239-2

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@article{1213082971c94131ba1f784589fb7998,

title = "The correlation between expansion speed and magnetic field in solar flare ribbons",

abstract = "In this paper, we study the correlation between the expansion speed of two-ribbon flares and the magnetic field measured in the ribbon location, and compare such correlation for two events with different magnetic configurations. These two events are: an M1.0 flare in the quiet sun on September 12, 2000 and an X2.3 flare in Active Region NOAA 9415 on April 10, 2001. The magnetic configuration of the M1.0 flare is simple, while that of X2.3 event is complex. We have derived a power-law correlation between the ribbon expansion speed (V r ) and the longitudinal magnetic field (B z ) with an empirical relationship V r = A×B- z -δ, where A is a constant and δ is the index of the power-law correlation. We have found that δ for the M1.0 flare in the simple magnetic configuration is larger than that for the X2.3 flare in the complex magnetic configuration.",

keywords = "Solar activity, Solar flares, Solar magnetic field",

author = "Wenbin Xie and Haimin Wang and Ju Jing and Xingming Bao and Hongqi Zhang",

note = "Funding Information: Received July 29, 2009; accepted August 18, 2009 doi: 10.1007/s11433-009-0239-2 †Corresponding author (email: wb xie@bao.ac.cn) Supported by the National Natural Science Foundation of China (Grant Nos. 10611120338, 10473016, 10673016, and 60673158), the National Basic Research Program of China (Grant No. 2006CB806301), the Chinese Academy of Sciences (Grant No. KLCX2-YW-T04), and the National Aeronautics and Space Administration of USA (Grant Nos. NNX0-7AH78G and NNX0-8AQ90G) Xie W B, Wang H M, Jing J, et al. The correlation between expansion speed and magnetic field in solar flare ribbons. Sci China Ser G, 2009, 52(11): 1754-1759, doi: 10.1007/s11433-009-0239-2",

year = "2009",

month = nov,

doi = "10.1007/s11433-009-0239-2",

language = "English (US)",

volume = "52",

pages = "1754--1759",

journal = "Science in China, Series G: Physics Astronomy",

issn = "1674-7348",

publisher = "Science in China Press",

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TY - JOUR

T1 - The correlation between expansion speed and magnetic field in solar flare ribbons

AU - Xie, Wenbin

AU - Wang, Haimin

AU - Jing, Ju

AU - Bao, Xingming

AU - Zhang, Hongqi

N1 - Funding Information: Received July 29, 2009; accepted August 18, 2009 doi: 10.1007/s11433-009-0239-2 †Corresponding author (email: wb xie@bao.ac.cn) Supported by the National Natural Science Foundation of China (Grant Nos. 10611120338, 10473016, 10673016, and 60673158), the National Basic Research Program of China (Grant No. 2006CB806301), the Chinese Academy of Sciences (Grant No. KLCX2-YW-T04), and the National Aeronautics and Space Administration of USA (Grant Nos. NNX0-7AH78G and NNX0-8AQ90G) Xie W B, Wang H M, Jing J, et al. The correlation between expansion speed and magnetic field in solar flare ribbons. Sci China Ser G, 2009, 52(11): 1754-1759, doi: 10.1007/s11433-009-0239-2

PY - 2009/11

Y1 - 2009/11

N2 - In this paper, we study the correlation between the expansion speed of two-ribbon flares and the magnetic field measured in the ribbon location, and compare such correlation for two events with different magnetic configurations. These two events are: an M1.0 flare in the quiet sun on September 12, 2000 and an X2.3 flare in Active Region NOAA 9415 on April 10, 2001. The magnetic configuration of the M1.0 flare is simple, while that of X2.3 event is complex. We have derived a power-law correlation between the ribbon expansion speed (V r ) and the longitudinal magnetic field (B z ) with an empirical relationship V r = A×B- z -δ, where A is a constant and δ is the index of the power-law correlation. We have found that δ for the M1.0 flare in the simple magnetic configuration is larger than that for the X2.3 flare in the complex magnetic configuration.

AB - In this paper, we study the correlation between the expansion speed of two-ribbon flares and the magnetic field measured in the ribbon location, and compare such correlation for two events with different magnetic configurations. These two events are: an M1.0 flare in the quiet sun on September 12, 2000 and an X2.3 flare in Active Region NOAA 9415 on April 10, 2001. The magnetic configuration of the M1.0 flare is simple, while that of X2.3 event is complex. We have derived a power-law correlation between the ribbon expansion speed (V r ) and the longitudinal magnetic field (B z ) with an empirical relationship V r = A×B- z -δ, where A is a constant and δ is the index of the power-law correlation. We have found that δ for the M1.0 flare in the simple magnetic configuration is larger than that for the X2.3 flare in the complex magnetic configuration.

KW - Solar activity

KW - Solar flares

KW - Solar magnetic field

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JO - Science in China, Series G: Physics Astronomy

JF - Science in China, Series G: Physics Astronomy

IS - 11

ER -

The correlation between expansion speed and magnetic field in solar flare ribbons

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