The EUV Imaging Spectrometer for Hinode

Culhane, J. L.; Harra, L. K.; James, Ady; Al-Janabi, K.; Bradley, L.; Chaudry, R. A.; Rees, K.; Tandy, J. A.; Thomas, Padmaja B.; Whillock, M. C. R.; Winter, B.; Doschek, G. A.; Korendyke, C. M.; Brown, C. M.; Myers, S. H.; Mariska, J. T.; Seely, John F.; Lang, J.; Kent, B. J.; Shaughnessy, Bryan; Young, Peter R.; Simnett, G. M.; Castelli, C.; Mahmoud, Saad; Mapson-Menard, H.; Probyn, B. J.; Thomas, R. J.; Davila, J. M.; Dere, K. P.; Windt, David L.; Shea, J.; Hagood, R.; Moye, Robert W.; Hara, Hirohisa; Watanabe, Tetsuya; Matsuzaki, Keiichi; Kosugi, T.; Hansteen, V. H.; Wikstøl, Ø.

doi:10.1007/s01007-007-0293-1

Cited by 880 publications

(474 citation statements)

References 34 publications

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“…Spectrographs such as SUMER [52], EIS [53] or IRIS [54] provide not only Doppler shifts to deduce the velocities but also ratios of emission lines that can be used to deduce temperature, density or even elemental abundances, as noted in textbooks, e.g. [55].…”

Section: (A) Inversions Of Observationsmentioning

confidence: 99%

What can large-scale magnetohydrodynamic numerical experiments tell us about coronal heating?

Peter

2015

Phil. Trans. R. Soc. A.

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The upper atmosphere of the Sun is governed by the complex structure of the magnetic field. This controls the heating of the coronal plasma to over a million kelvin. Numerical experiments in the form of threedimensional magnetohydrodynamic simulations are used to investigate the intimate interaction between magnetic field and plasma. These models allow one to synthesize the coronal emission just as it would be observed by real solar instrumentation. Largescale models encompassing a whole active region form evolving coronal loops with properties similar to those seen in extreme ultraviolet light from the Sun, and reproduce a number of average observed quantities. This suggests that the spatial and temporal distributions of the heating as well as the energy distribution of individual heat deposition events in the model are a good representation of the real Sun. This provides evidence that the braiding of fieldlines through magneto-convective motions in the photosphere is a good concept to heat the upper atmosphere of the Sun.

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Section: (A) Inversions Of Observationsmentioning

confidence: 99%

What can large-scale magnetohydrodynamic numerical experiments tell us about coronal heating?

Peter

2015

Phil. Trans. R. Soc. A.

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“…The observation time period of the selected EIS data started at 1907:27 UT on 11 December 2006. Since the EIS instrument relies on slit scanning mechanism to obtain coronal loop images of EUV emission lines [Culhane et al, 2007], it needed several hours to obtain the whole field data of the active region NOAA 10930. As shown in Table 4, the EUV spectral line adopted to make the EIS picture is Fe xv 284.16 Å [Culhane et al, 2007].…”

Section: Xrt and Eis Coronal Loop Imagesmentioning

confidence: 99%

“…Since the EIS instrument relies on slit scanning mechanism to obtain coronal loop images of EUV emission lines [Culhane et al, 2007], it needed several hours to obtain the whole field data of the active region NOAA 10930. As shown in Table 4, the EUV spectral line adopted to make the EIS picture is Fe xv 284.16 Å [Culhane et al, 2007]. Among the nine EUV spectral line windows in the original EIS data, the emission line Fe xv 284.16 Å is selected because the image formed from this line best exhibits structures of coronal loops compared with other spectral lines.…”

Section: Xrt and Eis Coronal Loop Imagesmentioning

confidence: 99%

“…The XRT images after cropping are enlarged and shown in Figure 11. b The EIS instrument relies on slit scanning mechanism to obtain coronal images of EUV emission lines [Culhane et al, 2007]; it needed several hours to obtain the whole field data of the active region NOAA 10930. c There are totally nine EUV spectral line windows in the original EIS data. The emission line Fe xv 284.16 Å is adopted to make the EIS picture because the image formed from this line best exhibits structures of coronal loops.…”

Section: Internal Consistency Of the Extrapolated Fieldsmentioning

confidence: 99%

“…The Hinode satellite, which was formerly called Solar-B and was launched in September 2006, can obtain high-quality photospheric vector magnetograms of solar active regions by SOT-SP instrument, and the simultaneous coronal loop images of the same active regions in soft X-ray band by the X-Ray Telescope (XRT) Kano et al, 2008] as well as in extreme ultraviolet band by the EUV Imaging Spectrometer (EIS) [Culhane et al, 2007]. These advantages makes the data of Hinode be valuable for NLFFF extrapolation studies DeRosa et al, 2009].…”

Section: Introductionmentioning

confidence: 99%

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Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

Wang

Yan

2011

J. Geophys. Res.

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[1] The Hinode satellite can obtain high-quality photospheric vector magnetograms of solar active regions and the simultaneous coronal loop images in soft X-ray and extreme ultraviolet (EUV) bands. In this paper, we continue the work of and apply the newly developed upward boundary integration computational scheme for the nonlinear force-free field (NLFFF) extrapolation of the coronal magnetic field to the

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An integral field spectrograph utilizing mirrorlet arrays

Chamberlin

Gong

2016

JGR Space Physics

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An integral field spectrograph (IFS) has been developed that utilizes a new and novel optical design to observe two spatial dimensions simultaneously with one spectral dimension. This design employs an optical 2‐D array of reflecting and focusing mirrorlets. This mirrorlet array is placed at the imaging plane of the front‐end telescope to generate a 2‐D array of tiny spots replacing what would be the slit in a traditional slit spectrometer design. After the mirrorlet in the optical path, a grating on a concave mirror surface will image the spot array and provide high‐resolution spectrum for each spatial element at the same time; therefore, the IFS simultaneously obtains the 3‐D data cube of two spatial and one spectral dimensions. The new mirrorlet technology is currently in‐house and undergoing laboratory testing at NASA Goddard Space Flight Center. Section 1 describes traditional classes of instruments that are used in Heliophysics missions and a quick introduction to the new IFS design. Section 2 discusses the details of the most generic mirrorlet IFS, while section 3 presents test results of a lab‐based instrument. An example application to a Heliophysics mission to study solar eruptive events in extreme ultraviolet wavelengths is presented in section 4 that has high spatial resolution (0.5 arc sec pixels) in the two spatial dimensions and high spectral resolution (66 mÅ) across a 15 Å spectral window. Section 4 also concludes with some other optical variations that could be employed on the more basic IFS for further capabilities of this type of instrument.

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The EUV Imaging Spectrometer for Hinode

Cited by 880 publications

References 34 publications

What can large-scale magnetohydrodynamic numerical experiments tell us about coronal heating?

What can large-scale magnetohydrodynamic numerical experiments tell us about coronal heating?

Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

An integral field spectrograph utilizing mirrorlet arrays

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