The Interface Region Imaging Spectrograph (IRIS)
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- 作者：B. De?Pontieu (1) (7)
A. M. Title (1)
J. R. Lemen (1)
G. D. Kushner (1)
D. J. Akin (1)
B. Allard (1)
T. Berger (1) (12)
P. Boerner (1)
M. Cheung (1)
C. Chou (1)
J. F. Drake (1)
D. W. Duncan (1)
S. Freeland (1)
G. F. Heyman (1)
C. Hoffman (1)
N. E. Hurlburt (1)
R. W. Lindgren (1)
D. Mathur (1)
R. Rehse (1)
D. Sabolish (1)
R. Seguin (1)
C. J. Schrijver (1)
T. D. Tarbell (1)
J.-P. Wülser (1)
C. J. Wolfson (1)
C. Yanari (1)
J. Mudge (2)
N. Nguyen-Phuc (2)
R. Timmons (2)
R. van Bezooijen (2)
I. Weingrod (2)
R. Brookner (3)
G. Butcher (3)
B. Dougherty (3)
J. Eder (3)
V. Knagenhjelm (3)
S. Larsen (3)
D. Mansir (3)
L. Phan (3)
P. Boyle (3)
P. N. Cheimets (4)
E. E. DeLuca (4)
L. Golub (4)
R. Gates (4)
E. Hertz (4)
S. McKillop (4)
S. Park (4)
T. Perry (4)
W. A. Podgorski (4)
K. Reeves (4)
S. Saar (4)
P. Testa (4)
H. Tian (4)
M. Weber (4)
C. Dunn (5)
S. Eccles (5)
S. A. Jaeggli (5)
C. C. Kankelborg (5)
K. Mashburn (5)
N. Pust (5)
L. Springer (5)
R. Carvalho (6)
L. Kleint (10) (6)
J. Marmie (6)
E. Mazmanian (6)
T. M. D. Pereira (6) (7)
S. Sawyer (6)
J. Strong (6)
S. P. Worden (6)
M. Carlsson (7)
V. H. Hansteen (7)
J. Leenaarts (7)
M. Wiesmann (7)
J. Aloise (8)
K.-C. Chu (8)
R. I. Bush (8)
P. H. Scherrer (8)
P. Brekke (9)
J. Martinez-Sykora (1) (10)
B. W. Lites (11)
S. W. McIntosh (11)
H. Uitenbroek (12)
T. J. Okamoto (13)
M. A. Gummin (14)
G. Auker (15)
P. Jerram (15)
P. Pool (15)
N. Waltham (16) - 关键词：Heating ; chromospheric ; Heating ; coronal ; Chromosphere ; models ; Chromosphere ; active ; Corona ; active ; Magnetic fields ; chromosphere ; Instrumentation and data management ; Spectrum ; ultraviolet
- 刊名：Solar Physics
- 出版年：2014
- 出版时间：July 2014
- 年：2014
- 卷：289
- 期：7
- 页码：2733-2779
- 全文大小：4,110 KB
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1. Lockheed Martin Solar & Astrophysics Laboratory, Lockheed Martin Advanced Technology Center, Org. A021S, Bldg. 252, 3251 Hanover St., Palo Alto, CA, 94304, USA
7. Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, Oslo, Norway
12. National Solar Observatory, Sacramento Peak, P.O. Box 62, Sunspot, NM, 88349-0062, USA
2. Lockheed Martin Advanced Technology Center, Palo Alto, 3251 Hanover St., Palo Alto, CA, 94304, USA
3. Lockheed Martin, 1111 Lockheed Martin Way, Sunnyvale, CA, 94089, USA
4. Harvard-Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA, 02138, USA
5. Department of Physics, Montana State University, Bozeman, P.O. Box 173840, Bozeman, MT, 59717, USA
6. NASA Ames Research Center, Moffet Field, CA, 94305, USA
10. Bay Area Environmental Research Institute, 596 1st St West, Sonoma, CA, 95476, USA
8. W.W. Hansen Experimental Physics Laboratory, Center for Space Science and Astrophysics, Stanford University, Stanford, CA, 94305, USA
9. Norwegian Space Centre, P.O. Box 113 Sk?yen, 0212, Oslo, Norway
11. High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO, 80307, USA
13. ISAS/JAXA, Sagamihara, Kanagawa, 252-5210, Japan
14. Alias Aerospace, Inc., 1731 Saint Andrews Court, St. Helena, CA, 94584, USA
15. e2v technologies, 106 Waterhouse Lane, Chelmsford, Essex, CM1 2QU, UK
16. Rutherford Appleton Laboratory, Harwell Business Innovation Campus, Didcot, Oxon, OX11 0QX, UK - ISSN：1573-093X
文摘
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?–-.4?arcsec spatial resolution, two-second temporal resolution, and 1?km?s? 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?–-358??, 1389?–-407??, and 2783?–-834??, including bright spectral lines formed in the chromosphere (Mg?ii h 2803?? and Mg?ii k 2796??) and transition region (C?ii 1334/1335?? and Si?iv 1394/1403??). Slit-jaw images in four different passbands (C?ii 1330, Si?iv 1400, Mg?ii k 2796, and Mg?ii wing 2830??) 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 to facilitate interpretation of observations of this complex region. Approximately eight Gbytes of data (after compression) are acquired by IRIS each day and made available for unrestricted use within a few days of the observation.