Atomic data from the IRON project

Storey, P. J.; Zeippen, C. J.

doi:10.1051/0004-6361/200912689

Cited by 27 publications

(32 citation statements)

References 23 publications

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“…Averaged densities of 6 × 10 9 and 1 × 10 10 cm −3 for the rest and blue-wing components are found respectively. The density of the rest component, which corresponds to the foreground active region emission, is in excellent agreement with the density obtained from the Fe xiii 202.04, 203.83 Å ratio (5 × 10 9 cm −3 ), using the recent new scattering calculations of Storey & Zeippen (2010). If one assumes a unity filling factor (i.e.…”

Section: Flare Kernels: Source Regions Of Chromospheric Evaporationsupporting

confidence: 82%

The 22 May 2007 B-class flare: new insights fromHinodeobservations

Zanna¹,

Mitra-Kraev²,

Bradshaw

et al. 2010

A&A

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We present multi-wavelength observations of a small B-class flare which occurred on the Sun on 2007 May 22. The observations include data from Hinode, GOES, TRACE and the Nobeyama Radioheliograph. We obtained spatially and spectrally-resolved information from the Hinode EUV Imaging Spectrometer (EIS) during this event. The temporal and temperature coverage of the EIS observations provides new insights into our understanding of chromospheric evaporation and cooling. The flare showed many "typical" features, such as brightenings in the ribbons, hot (10 MK) loop emission and subsequent cooling. We also observed a new feature, strong (up to 170 km s −1 ) blue-shifted emission in lines formed around 2-3 MK, located at the footpoints of the 10 MK coronal emission and within the ribbons. Electron densities at 2 MK in the kernels are high, of the order of 10 11 cm −3 , suggesting a very narrow layer where the chromospheric evaporation occurs. We have run a non-equilibrium hydrodynamic numerical simulation using the HYDRAD code to study the cooling of the 10 MK plasma, finding good agreement between the predicted and observed temperatures, densities and ion populations. Line blending for some potentially useful diagnostic lines for flares, which are observed with Hinode/EIS, is also discussed.

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Section: Flare Kernels: Source Regions Of Chromospheric Evaporationsupporting

confidence: 82%

The 22 May 2007 B-class flare: new insights fromHinodeobservations

Zanna¹,

Mitra-Kraev²,

Bradshaw

et al. 2010

A&A

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“…The discrepancies between different ions are difficult to explain. We note that the atomic data for Si X and Fe XIII have recently been updated, as described in Liang et al (2009) and Storey & Zeippen (2010). The most recent atomic data for Fe XII is discussed in Storey et al (2005).…”

Section: Densitiesmentioning

confidence: 98%

Hinode extreme-ultraviolet imaging spectrometer observations of a limb active region

O’Dwyer¹,

Zanna²,

Mason³

et al. 2010

A&A

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Aims. We investigate the electron density and temperature structure of a limb active region. Methods. We have carried out a study of an active region close to the solar limb using observations from the Extreme-ultraviolet Imaging Spectrometer (EIS) and the X-ray telescope (XRT) on board Hinode. The electron density and temperature distributions of the coronal emission have been determined using emission line intensity ratios. Differential emission measure (DEM) analysis and the emission measure (EM) loci technique were used to examine the thermal structure of the emitting plasma as a function of distance from the limb. Results. The highest temperature and electron density values are found to be located in the core of the active region, with a peak electron number density value of 1.9 × 10 10 cm −3 measured using the Fe XII 186.887 Å to 192.394 Å line intensity ratio. The plasma along the line of sight in the active region was found to be multi-thermal at different distances from the limb. The EIS and XRT DEM analyses appear to be in agreement in the temperature interval from log T = 6.5−6.7. Conclusions. Our results provide new constraints for models of coronal heating in active regions.

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“…All previous EUV line identifications were reviewed by comparing the line intensities calculated with the latest atomic data from Storey & Zeippen (2010), supplemented with A-values. The benchmark provides for the first time (cf.…”

Section: Discussionmentioning

confidence: 99%

“…Notice that the ordering of the levels in AK05 is different from that of the other authors. Storey & Zeippen (2010) performed an extensive benchmark calculation using SUPERSTRUCTURE, which was used to validate the target for the scattering calculation. The target included terms arising from the 3s 2 3p 2 , 3s 3p 3 , 3s 2 3p 3d, 3p 4 , 3s 3p 2 3d, 3s 2 3d 2 , and 3p 3 3d configurations.…”

Section: Atomic Data and Benchmark Methodsmentioning

confidence: 99%

Benchmarking atomic data for astrophysics: Fe xiii EUV lines

Zanna

2011

A&A

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Recent atomic data for Fe xiii are benchmarked against high-resolution spectroscopic observations of the solar corona. All the identifications of the EUV lines are reviewed by also taking into account laboratory measurements. A few new identifications are proposed, and many wavelengths are revised. All the strongest EUV lines are now identified. Very good agreement between predicted and observed line intensities is generally found using the latest atomic calculations. We clearly indicate which EUV lines are blended, and which are best for electron-density measurements in different regimes.

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Atomic data from the IRON project

Cited by 27 publications

References 23 publications

The 22 May 2007 B-class flare: new insights fromHinodeobservations

The 22 May 2007 B-class flare: new insights fromHinodeobservations

Hinode extreme-ultraviolet imaging spectrometer observations of a limb active region

Benchmarking atomic data for astrophysics: Fe xiii EUV lines

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