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Statistical Study of Emerging Flux Regions and the Upper Atmosphere Response View all abstracts by submitter

Jie Zhao   Submitted: 2012-07-04 19:42

We statistically study the property of emerging flux regions (EFRs) and the upper solar atmosphere response to the flux emergence by using data from the Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). Parameters including the total emerged flux, the flux growth rate, the maximum area, the duration of the emergence and the separation speed of the opposite polarities are adopted to delineate the property of the EFRs. The response of the upper atmosphere is addressed by the response of the atmosphere at different wavelengths (and thus at different temperatures). According to our results, the total emerged fluxes are in the range of (0.44 - 11.2) imes1019 Mx while the maximum area ranges from 17 to 182 arcsec2. The durations of the emergence are between 1 and 12 hours, which are positively correlated to both the total emerged flux and the maximum area. The maximum distances between the opposite polarities are 7 - 25 arcsec and are also correlated to the duration positively. The separation speeds are from 0.05 to 1.08 km s-1, negatively correlated to the duration. The derived flux growth rates are (0.1 - 1.3) imes1019 Mx hr-1, which are positively correlated to the total emerging flux. The upper atmosphere responds to the flux emergence in the 1600AA chromospheric line first, and then tens and hundreds of seconds later, in coronal lines, such as the 171AA (T=105.8 K) and 211AA (T=106.3 K) lines almost simultaneously, suggesting the successively heating of atmosphere from the chromosphere to the corona.

Authors: Zhao, Jie; Li, Hui
Projects: None

Publication Status: Accepted for publication in RAA
Last Modified: 2012-07-05 07:17
Go to main E-Print page  Principal Component Analysis of Background and Sunspot Magnetic Field Variations During Solar Cycles 21-23  Secondary Waves, and/or the ''Reflection'' From and ''Transmission'' Through a Coronal Hole of an EUV Wave Associated With the 2011 February 15 X2.2 Flare Observed With SDO/AIA and STEREO/EUVI  Edit Entry  Download Preprint  Delete Entry 

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