Laboratory calibration of the Extreme-Ultraviolet Imaging Spectrometer for the Solar-B satellite

Lang, J.; Kent, B. J.; Paustian, Wolfgang; Brown, C. M.; Keyser, Christian; Anderson, Mark R.; Case, Giles C. R.; Chaudry, R. A.; James, Ady; Korendyke, C. M.; Pike, C. D.; Probyn, B. J.; Rippington, David J.; Seely, John F.; Tandy, J. A.; Whillock, M. C. R.

doi:10.1364/ao.45.008689

Cited by 109 publications

(88 citation statements)

References 19 publications

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“…We then converted the EIS radiances into simulated AIA count rates, for the 171, 193 and 211 Å channels, using the EIS (Lang et al 2006) and AIA ) effective areas (as currently available within Solarsoft). The results are shown in Fig.…”

Section: Discussion Of Cool Emission: Loop Footpointmentioning

confidence: 99%

SDO AIA and Hinode EIS observations of “warm” loops

Zanna

O’Dwyer

Mason

2011

A&A

130

106

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We present simultaneous observations of active region "warm" (1 MK) loops using the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) and Hinode EUV Imaging Spectrometer (EIS). Sample EIS spectra for a loop footpoint and a lop leg region are presented, and are used to describe the spectral lines which contribute to the six AIA EUV channels, both directly and predicted with DEM modeling. We find good overall agreement between observed and predicted count rates for the 131 Å, 193 Å, and 335 Å bands, but highlight a number of problems, partly to be ascribed to inter-calibration issues, partly due to the fact that a large number of lines remain unidentified for the 94 Å, 171 Å, and 211 Å bands. We also found that the 335 Å band is severely affected by cross-talk with the 131 Å band and by second order contributions. We extend our previous work where we highlighted the multi-thermal nature of the SDO AIA bands to show that emission from lines formed at typical transition region temperatures (log T [K] = 5.0-5.8) can be significant for all the EUV channels, and even dominant in some cases. We also assess the possibility of deriving accurate emission measures from the AIA observations. We have found that the inversion of the AIA data to obtain a description of the thermal characteristics of warm loops is unreliable. We highlight the need for further work on the relevant atomic data before the AIA data can be reliably used for plasma diagnostic purposes.

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Section: Discussion Of Cool Emission: Loop Footpointmentioning

confidence: 99%

SDO AIA and Hinode EIS observations of “warm” loops

Zanna

O’Dwyer

Mason

2011

A&A

130

106

View full text Add to dashboard Cite

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“…The interpolated spectrum is computed using the data in units of counts and then converted to physical units using both the pre-flight calibration (Lang et al 2006) and the revised calibration of Warren et al (2014), which includes time-and wavelength-dependent changes to the instrument sensitivity (see Del Zanna 2013a for an extensive discussion of EIS calibration issues). For this work we use the data calibrated using the effective areas of Warren et al (2014).…”

Section: Observationsmentioning

confidence: 99%

Transition Region Abundance Measurements During Impulsive Heating Events

Warren

Brooks

Doschek

et al. 2016

ApJ

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It is well established that elemental abundances vary in the solar atmosphere and that this variation is organized by first ionization potential (FIP). Previous studies have shown that in the solar corona, low-FIP elements such as Fe, Si, Mg, and Ca, are generally enriched relative to high-FIP elements such as C, N, O, Ar, and Ne. In this paper we report on measurements of plasma composition made during impulsive heating events observed at transition region temperatures with the Extreme Ultraviolet Imaging Spectrometer (EIS) on Hinode. During these events the intensities of O IV, V, and VI emission lines are enhanced relative to emission lines from Mg V, VI, and VII and Si VI and VII, and indicate a composition close to that of the photosphere. Long-lived coronal fan structures, in contrast, show an enrichment of low-FIP elements. We conjecture that the plasma composition is an important signature of the coronal heating process, with impulsive heating leading to the evaporation of unfractionated material from the lower layers of the solar atmosphere and higher-frequency heating leading to long-lived structures and the accumulation of low-FIP elements in the corona.

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“…The Fe XXIII 263.765 Å line, indicated with an arrow, is included as an upper limit. The error bars on the ratio correspond to a combination of the one sigma uncertainties on the line fitting and an uncertainty of 22% on the observed intensity based on the pre-flight calibration of EIS (Lang et al 2006). of 22% on the observed intensity based on the pre-flight calibration of EIS (Lang et al 2006).…”

Section: Emission Measurementioning

confidence: 99%

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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Laboratory calibration of the Extreme-Ultraviolet Imaging Spectrometer for the Solar-B satellite

Cited by 109 publications

References 19 publications

SDO AIA and Hinode EIS observations of “warm” loops

SDO AIA and Hinode EIS observations of “warm” loops

Transition Region Abundance Measurements During Impulsive Heating Events

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

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