The interface region imaging spectrograph for the IRIS Small Explorer mission

Wülser, J. P.; Title, A. M.; Lemen, J. R.; Pontieu, Bart De; Kankelborg, C. C.; Tarbell, T. D.; Berger, Thomas; Golub, L.; Kushner, G.; Chou, Cathy; Weingrod, Isaac; Holmes, B.; Mudge, Jason; Podgorski, William

doi:10.1117/12.927036

Cited by 11 publications

(6 citation statements)

References 4 publications

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“…The response of the STEREO/EUVI 171 Å as a function of plasma temperature is within the range log T e ≈ 5.1 − 6.7 (Wülser et al 2004). If we suppose the plasma cooling through this narrow band filter is dominated by radiative losses process, then the cooling time, τ cool ≈ τ rad , would be ranged from a few seconds to an hour (see e. g., Aschwanden 2000Aschwanden , 2004.…”

Section: Results For Stereo/euvimentioning

confidence: 75%

Can a Nanoflare Model of Extreme-Ultraviolet Irradiances Describe the Heating of the Solar Corona?

Tajfirouze

Safari

2011

ApJ

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Nanoflares, the basic unit of impulsive energy release may produce much of the solar background emission. Extrapolation of the energy frequency distribution of observed microflares, which follows a power law to lower energies can give an estimation of the importance of nanoflares for heating the solar corona. If the power law index is greater than 2, then the nanoflare contribution is dominant. We model time series of extreme ultraviolet emission radiance, as random flares with a power law exponent of the flare event distribution. The model is based on three key parameters, the flare rate, the flare duration and the power law exponent of the flare intensity frequency distribution. We use this model to simulate emission line radiance detected in 171Å, observed by STEREO/EUVI and SDO/AIA. The Observed light curves are matched with simulated light curves using an Artificial Neural Network and parameter values are determined across regions of active region, quiet sun, and coronal hole. The damping rate of nanoflares is compared with radiative losses cooling time. The effect of background emission, data cadence, and network sensitivity on the key parameters of model is studied.Most of the observed light curves have a power law exponent, α, greater than the critical value 2. At these sites nanoflare heating could be significant.

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Section: Results For Stereo/euvimentioning

confidence: 75%

Can a Nanoflare Model of Extreme-Ultraviolet Irradiances Describe the Heating of the Solar Corona?

Tajfirouze

Safari

2011

ApJ

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“…Portions of the IRIS instrument are described in some detail in pre-launch articles by Wülser et al (2012) and Podgorski et al (2012), and key parameters are provided in Table 1. Here we briefly summarize the instrument capabilities and refer the reader desiring more technical details to the above mentioned spectrograph and telescope articles.…”

Section: Instrument Overviewmentioning

confidence: 99%

“…After the collimator, the FUV and NUV SG spectrograph beams are fed to separate gratings, camera mirrors, and detectors (Table 2 and Figure 9). The FUV and NUV gratings, fabricated by Horiba Jobin-Yvon, have a groove density of 3600 lines mm −1 and are described in more detail by Wülser et al (2012). The FUV and NUV SG beams have separate shutters and are recorded onto three separate CCDs: two for the FUV and one for the NUV.…”

Section: Spectrographmentioning

confidence: 99%

“…The IRIS CCDs have been treated with a e2v proprietary backside-enhancement process, which enables a quantum efficiency of about 31 % at 1400 Å. The enhancement treatment results in an annealing pattern, visible in CCD flat-field images as an approximately rectangular grid of lines, which show sensitivity differences on the order of 5 -10 % (Wülser et al, 2012).…”

Section: Ccd Detector and Camera Systemmentioning

confidence: 99%

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The Interface Region Imaging Spectrograph (IRIS)

et al. 2014

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The Interface Region Imaging Spectrograph (IRIS) small explorer spacecraft provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 -0.4 arcsec spatial resolution, two-second temporal resolution, and 1 km s −1 velocity resolution over a field-of-view of up to 175 arcsec × 175 arcsec. . IRIS is sensitive to emission from plasma at temperatures between 5000 K and 10 MK and will advance our understanding of the flow of mass and energy through an interface region, formed by the chromosphere and transition region, between the photosphere and corona. This highly structured and dynamic region not only acts as the conduit of all mass and energy feeding into the corona and solar wind, it also requires an order of magnitude more energy to heat than the corona and solar wind combined. The IRIS investigation includes a strong numerical modeling component based on advanced radiative-MHD codes to facilitate interpretation of observations of this complex region. Approximately eight Gbytes of data (after compression) are acquired by B. De Pontieu (B) ·Harvard-Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA

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“…The IRIS CCDs have been treated with e2v's proprietary backside-enhancement process, which eables a quantum efficiency of about 31 % at 1400 Å. The enhancement treatment results in an annealing pattern, visible in CCD flat-field images as an approximately rectangular grid of lines that show sensitivity differences of order 5 -10 % (Wülser et al, 2012).…”

Section: Ccd Detector and Camera Systemmentioning

confidence: 99%

The Interface Region Imaging Spectrograph (IRIS)

De Pontieu,

Title,

Lemen

et al. 2014

Preprint

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The Interface Region Imaging Spectrograph (IRIS) small explorer spacecraft provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 -0.4 arcsec spatial resolution, 2 s temporal resolution and 1 km s −1 velocity resolution over a field-of-view of up to 175 arcsec × 175 arcsec. IRIS was launched into a Sun-synchronous orbit on 27 June 2013 using a Pegasus-XL rocket and consists of a 19-cm UV telescope that feeds a slit-based dual-bandpass imaging spectrograph. IRIS obtains spectra in passbands from 1332-1358 Å, 1389-1407 Å and 2783-2834 Å including bright spectral lines formed in the chromosphere (Mg ii h 2803 Å and Mg ii k 2796 Å) and transition region (C ii 1334/1335 Å and Si iv 1394/1403 Å). Slit-jaw images in four different passbands (C ii 1330, Si iv 1400, Mg ii k 2796 and Mg ii wing 2830 Å) can be taken simultaneously with spectral rasters that sample regions up to 130 arcsec × 175 arcsec at a variety of spatial samplings (from 0.33 arcsec and up). IRIS is sensitive to emission from plasma at temperatures between 5000 K and 10 MK and will advance our understanding of the flow of mass and energy through an interface region, formed by the chromosphere and transition region, between the photosphere and corona. This highly structured and dynamic region not only acts as the conduit of all mass and energy feeding into the corona and solar wind, it also requires an order of magnitude more energy to heat than the corona and solar wind combined. The IRIS investigation includes a strong numerical modeling component based on advanced radiative-MHD codes

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The interface region imaging spectrograph for the IRIS Small Explorer mission

Cited by 11 publications

References 4 publications

Can a Nanoflare Model of Extreme-Ultraviolet Irradiances Describe the Heating of the Solar Corona?

Can a Nanoflare Model of Extreme-Ultraviolet Irradiances Describe the Heating of the Solar Corona?

The Interface Region Imaging Spectrograph (IRIS)

The Interface Region Imaging Spectrograph (IRIS)

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