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Title: The EUV Imaging Spectrometer for Hinode

Abstract

The EUV Imaging Spectrometer (EIS) on Hinode will observe solar corona and upper transition region emission lines in the wavelength ranges 170?-?210 Angstroms and 250?-?290 Angstroms . The line centroid positions and profile widths will allow plasma velocities and turbulent or non-thermal line broadenings to be measured. We will derive local plasma temperatures and densities from the line intensities. The spectra will allow accurate determination of differential emission measure and element abundances within a variety of corona and transition region structures. These powerful spectroscopic diagnostics will allow identification and characterization of magnetic reconnection and wave propagation processes in the upper solar atmosphere. We will also directly study the detailed evolution and heating of coronal loops. The EIS instrument incorporates a unique two element, normal incidence design. The optics are coated with optimized multilayer coatings. We have selected highly efficient, backside-illuminated, thinned CCDs. These design features result in an instrument that has significantly greater effective area than previous orbiting EUV spectrographs with typical active region 2?-?5 s exposure times in the brightest lines. EIS can scan a field of 6x8.5 arc?min with spatial and velocity scales of 1 arc?sec and 25 km?s-1 per pixel. The instrument design, its absolute calibration, andmore » performance are described in detail in this paper. EIS will be used along with the Solar Optical Telescope (SOT) and the X-ray Telescope (XRT) for a wide range of studies of the solar atmosphere.« less

Authors:
; ; ; ; ; ; ; ; ;
Publication Date:
Research Org.:
Brookhaven National Laboratory (BNL) National Synchrotron Light Source
Sponsoring Org.:
Doe - Office Of Science
OSTI Identifier:
960141
Report Number(s):
BNL-83127-2009-JA
Journal ID: ISSN 0038-0938; SLPHAX; TRN: US201016%%1285
DOE Contract Number:
DE-AC02-98CH10886
Resource Type:
Journal Article
Resource Relation:
Journal Name: Solar Physics; Journal Volume: 243
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CALIBRATION; COATINGS; DESIGN; ELECTRON TEMPERATURE; ELEMENT ABUNDANCE; HEATING; ION TEMPERATURE; LINE BROADENING; MAGNETIC RECONNECTION; OPTICS; PERFORMANCE; PLASMA; SOLAR ATMOSPHERE; SOLAR CORONA; SPECTRA; SPECTROMETERS; TELESCOPES; VELOCITY; WAVE PROPAGATION; WAVELENGTHS; national synchrotron light source

Citation Formats

Culhane,J., Harra, L., James, A., Al-Janabi, K., Bradley, L., Chaudry, R., Rees, K., Tandy, J., Thomas, P., and et al. The EUV Imaging Spectrometer for Hinode. United States: N. p., 2007. Web. doi:10.1007/s01007-007-0293-1.
Culhane,J., Harra, L., James, A., Al-Janabi, K., Bradley, L., Chaudry, R., Rees, K., Tandy, J., Thomas, P., & et al. The EUV Imaging Spectrometer for Hinode. United States. doi:10.1007/s01007-007-0293-1.
Culhane,J., Harra, L., James, A., Al-Janabi, K., Bradley, L., Chaudry, R., Rees, K., Tandy, J., Thomas, P., and et al. Mon . "The EUV Imaging Spectrometer for Hinode". United States. doi:10.1007/s01007-007-0293-1.
@article{osti_960141,
title = {The EUV Imaging Spectrometer for Hinode},
author = {Culhane,J. and Harra, L. and James, A. and Al-Janabi, K. and Bradley, L. and Chaudry, R. and Rees, K. and Tandy, J. and Thomas, P. and et al},
abstractNote = {The EUV Imaging Spectrometer (EIS) on Hinode will observe solar corona and upper transition region emission lines in the wavelength ranges 170?-?210 Angstroms and 250?-?290 Angstroms . The line centroid positions and profile widths will allow plasma velocities and turbulent or non-thermal line broadenings to be measured. We will derive local plasma temperatures and densities from the line intensities. The spectra will allow accurate determination of differential emission measure and element abundances within a variety of corona and transition region structures. These powerful spectroscopic diagnostics will allow identification and characterization of magnetic reconnection and wave propagation processes in the upper solar atmosphere. We will also directly study the detailed evolution and heating of coronal loops. The EIS instrument incorporates a unique two element, normal incidence design. The optics are coated with optimized multilayer coatings. We have selected highly efficient, backside-illuminated, thinned CCDs. These design features result in an instrument that has significantly greater effective area than previous orbiting EUV spectrographs with typical active region 2?-?5 s exposure times in the brightest lines. EIS can scan a field of 6x8.5 arc?min with spatial and velocity scales of 1 arc?sec and 25 km?s-1 per pixel. The instrument design, its absolute calibration, and performance are described in detail in this paper. EIS will be used along with the Solar Optical Telescope (SOT) and the X-ray Telescope (XRT) for a wide range of studies of the solar atmosphere.},
doi = {10.1007/s01007-007-0293-1},
journal = {Solar Physics},
number = ,
volume = 243,
place = {United States},
year = {Mon Jan 01 00:00:00 EST 2007},
month = {Mon Jan 01 00:00:00 EST 2007}
}