Other
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1222l&link_type=abstract
American Astronomical Society, SPD meeting #40, #12.22; Bulletin of the American Astronomical Society, Vol. 41, p.831
Other
Scientific paper
We have investigated seven Extreme-Ultraviolet (EUV) bright points in the active region AR 0926 on 2006 December 2 by the EUV Imaging spectrometer (EIS) onboard Hinode spacecraft. We determined their Doppler velocities and non-thermal velocities from EUV spectral lines (log T=4.7-7.2) by fitting each line profile to a Gaussian function. We present the Doppler velocity map as a function of temperature which corresponds to a different height. As a result, these active region bright points can be classified into two types according to the pattern of doppler shifts. Type 1 bright point shows a systematic increase of Doppler velocity from -56km/s (blue shift) at log T=5.8 to 12km/s (red shift) at log T=6.7, while type 2 bright points have Doppler velocities in the range of -20km/s and 20km/s. Using MDI magnetograms, we found that only type 1 bright point was associated with the cancelling magnetic feature at the rate of Mx /hour. When assuming that these bright points are caused by magnetic reconnection and the Doppler shift indicates reconnection outflow, the pattern of the Doppler shift implies that type 1 bright point should be related to low atmosphere magnetic reconnection. We also determined their electron densities from line ratio as well as temperatures from emission measure loci using CHIANTI atomic database. The electron densities of all bright points are comparable to typical values of active regions (log Ne=9.9-10.4). The emission loci plots indicate that these bright points should not be isothermal. The DEM (Differential Emission Measure) analysis shows a broad temperature distribution near log T=6.3.
Kim Seongcheol
Lee Kyoung-Sun
Moon YaeEun
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