PMO OpenIR  > 太阳活动的多波段观测研究团组
Observations of solar flares with IRIS and SDO
Li, D.1,2,3; Innes, D. E.2; Ning, Z. J.1
2016-03-01
Source PublicationASTRONOMY & ASTROPHYSICS
Volume587
AbstractFlare kernels brighten simultaneously in all Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) channels making it difficult to determine their temperature structure. The Interface Region Imaging Spectrograph (IRIS) is able to spectrally resolve Fe XXI emission from cold chromospheric brightenings, so it can be used to infer the amount of Fe XXI emission in the 131 angstrom AIA channel. We use observations of two small solar flares seen by IRIS and SDO to compare the emission measures (EMs) deduced from the IRIS Fe XXI line and the AIA 131 angstrom channel to determine the fraction of Fe XXI emission in flare kernels in the 131 angstrom channel of AIA. Cotemporal and cospatial pseudo-raster AIA images are compared with the IRIS results. We use multi-Gaussian line fitting to separate the blending chromospheric emission so as to derive Fe XXI intensities and Doppler shifts in IRIS spectra. We define loop and kernel regions based on the brightness of the 131 angstrom and 1600 angstrom intensities. In the loop regions the Fe XXI EMs are typically 80% of the 131 angstrom values, and range from 67% to 92%. Much of the scatter is due to small misalignments, but the largest site with low Fe XXI contributions was probably affected by a recent injection of cool plasma into the loop. In flare kernels the contribution of Fe XXI increases from less than 10% at the low-intensity 131 angstrom sites to 40-80% in the brighter kernels. Here the Fe XXI is superimposed on bright chromospheric emission and the Fe XXI line shows blueshifts, sometimes extending up to the edge of the spectral window, 200 km s(-1). The AIA 131 angstrom emission in flare loops is due to Fe XXI emission with a 10-20% contribution from continuum, Fe XXIII, and cooler background plasma emission. In bright flare kernels up to 52% of the 131 angstrom is from cooler plasma. The wide range seen in the kernels is caused by significant structure in the kernels, which is seen as sharp gradients in Fe XXI EM at sites of molecular and transition region emission.
KeywordSun: Flares Sun: Uv Radiation Line: Profiles Techniques: Spectroscopic
WOS HeadingsScience & Technology ; Physical Sciences
DOI10.1051/0004-6361/201525642
WOS KeywordREGION-IMAGING-SPECTROGRAPH ; CHROMOSPHERIC EVAPORATION ; RESOLUTION OBSERVATIONS ; IMPULSIVE PHASE ; QUIET SUN ; EMISSION ; FOOTPOINTS ; DYNAMICS ; SDO/AIA ; PLASMA
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000371589800022
Citation statistics
Cited Times:9[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/16184
Collection太阳活动的多波段观测研究团组
Affiliation1.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Peoples R China
2.Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany
3.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
Recommended Citation
GB/T 7714
Li, D.,Innes, D. E.,Ning, Z. J.. Observations of solar flares with IRIS and SDO[J]. ASTRONOMY & ASTROPHYSICS,2016,587.
APA Li, D.,Innes, D. E.,&Ning, Z. J..(2016).Observations of solar flares with IRIS and SDO.ASTRONOMY & ASTROPHYSICS,587.
MLA Li, D.,et al."Observations of solar flares with IRIS and SDO".ASTRONOMY & ASTROPHYSICS 587(2016).
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