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The EUV Imaging Spectrometer for Hinode |
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| Authors: | J L Culhane L K Harra A M James K Al-Janabi L J Bradley R A Chaudry K Rees J A Tandy P Thomas M C R Whillock B Winter G A Doschek C M Korendyke C M Brown S Myers J Mariska J Seely J Lang B J Kent B M Shaughnessy P R Young G M Simnett C M Castelli S Mahmoud H Mapson-Menard B J Probyn R J Thomas J Davila K Dere D Windt J Shea R Hagood R Moye H Hara T Watanabe K Matsuzaki T Kosugi V Hansteen Ø Wikstol |
| Institution: | (1) Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT, UK;(2) Naval Research Laboratory, E.O. Hulburt Centre for Space Research, Washington, DC 20375-5320, USA;(3) Space Science and Technology Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire, OX11 0QX, UK;(4) Space Research Group, School of Physics and Space Research, University of Birmingham, Birmingham, UK;(5) NASA Goddard Space Flight Centre, Code 682, Greenbelt, MD 20771, USA;(6) School of Computational Sciences, George Mason University, 4400 University Drive, Fairfax, VA 22030, USA;(7) Pupin Physics Laboratories, Department of Astronomy, Columbia University, 550 West 120th Street, New York, 10027, USA;(8) Perdix Corporation, P.O. Box 23, 35 Howard Street, Wilton, NH 03086, USA;(9) Swales Aerospace, 5050 Powder Mill Road, Beltsville, MD 20705, USA;(10) Artep Inc., 2922 Excelsior Spring Ct., Ellicott City, MD 21042, USA;(11) National Astronomical Observatory of Japan, Mitaka, Tokyo 181, Japan;(12) Institute of Space and Astronautical Science, Sagamihara, Kanagawa 229, Japan;(13) Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029, Blindern, 0315 Oslo, Norway |
| Abstract: | The EUV Imaging Spectrometer (EIS) on Hinode will observe solar corona and upper transition region emission lines in the wavelength ranges 170?–?210 Å and 250?–?290 Å. 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 6×8.5 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. |
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