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 ) \times 10 ^ { 19 } Mx while the maximum area ranges from 17 to 182 arcsec ^ { 2 } .
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 ) \times 10 ^ { 19 } Mx hr ^ { -1 } , which are positively correlated to the total emerging flux .
The upper atmosphere responds to the flux emergence in the 1600Å chromospheric line first , and then tens and hundreds of seconds later , in coronal lines , such as the 171Å ( T=10 ^ { 5.8 } K ) and 211Å ( T=10 ^ { 6.3 } K ) lines almost simultaneously , suggesting the successively heating of atmosphere from the chromosphere to the corona .