The Interface Region Imaging Spectrograph (IRIS)
Abstract 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 resolut...
Ausführliche Beschreibung
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| Autor*in: |
De Pontieu, B. [verfasserIn] Title, A. M. [verfasserIn] Lemen, J. R. [verfasserIn] Kushner, G. D. [verfasserIn] Akin, D. J. [verfasserIn] Allard, B. [verfasserIn] Berger, T. [verfasserIn] Boerner, P. [verfasserIn] Cheung, M. [verfasserIn] Chou, C. [verfasserIn] Drake, J. F. [verfasserIn] Duncan, D. W. [verfasserIn] Freeland, S. [verfasserIn] Heyman, G. F. [verfasserIn] Hoffman, C. [verfasserIn] Hurlburt, N. E. [verfasserIn] Lindgren, R. W. [verfasserIn] Mathur, D. [verfasserIn] Rehse, R. [verfasserIn] Sabolish, D. [verfasserIn] Seguin, R. [verfasserIn] Schrijver, C. J. [verfasserIn] Tarbell, T. D. [verfasserIn] Wülser, J.-P. [verfasserIn] Wolfson, C. J. [verfasserIn] Yanari, C. [verfasserIn] Mudge, J. [verfasserIn] Nguyen-Phuc, N. [verfasserIn] Timmons, R. [verfasserIn] van Bezooijen, R. [verfasserIn] Weingrod, I. [verfasserIn] Brookner, R. [verfasserIn] Butcher, G. [verfasserIn] Dougherty, B. [verfasserIn] Eder, J. [verfasserIn] Knagenhjelm, V. [verfasserIn] Larsen, S. [verfasserIn] Mansir, D. [verfasserIn] Phan, L. [verfasserIn] Boyle, P. [verfasserIn] Cheimets, P. N. [verfasserIn] DeLuca, E. E. [verfasserIn] Golub, L. [verfasserIn] Gates, R. [verfasserIn] Hertz, E. [verfasserIn] McKillop, S. [verfasserIn] Park, S. [verfasserIn] Perry, T. [verfasserIn] Podgorski, W. A. [verfasserIn] Reeves, K. [verfasserIn] Saar, S. [verfasserIn] Testa, P. [verfasserIn] Tian, H. [verfasserIn] Weber, M. [verfasserIn] Dunn, C. [verfasserIn] Eccles, S. [verfasserIn] Jaeggli, S. A. [verfasserIn] Kankelborg, C. C. [verfasserIn] Mashburn, K. [verfasserIn] Pust, N. [verfasserIn] Springer, L. [verfasserIn] Carvalho, R. [verfasserIn] Kleint, L. [verfasserIn] Marmie, J. [verfasserIn] Mazmanian, E. [verfasserIn] Pereira, T. M. D. [verfasserIn] Sawyer, S. [verfasserIn] Strong, J. [verfasserIn] Worden, S. P. [verfasserIn] Carlsson, M. [verfasserIn] Hansteen, V. H. [verfasserIn] Leenaarts, J. [verfasserIn] Wiesmann, M. [verfasserIn] Aloise, J. [verfasserIn] Chu, K.-C. [verfasserIn] Bush, R. I. [verfasserIn] Scherrer, P. H. [verfasserIn] Brekke, P. [verfasserIn] Martinez-Sykora, J. [verfasserIn] Lites, B. W. [verfasserIn] McIntosh, S. W. [verfasserIn] Uitenbroek, H. [verfasserIn] Okamoto, T. J. [verfasserIn] Gummin, M. A. [verfasserIn] Auker, G. [verfasserIn] Jerram, P. [verfasserIn] Pool, P. [verfasserIn] Waltham, N. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2014 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967, 289(2014), 7 vom: 13. Feb., Seite 2733-2779 |
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| Übergeordnetes Werk: |
volume:289 ; year:2014 ; number:7 ; day:13 ; month:02 ; pages:2733-2779 |
| Links: |
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| DOI / URN: |
10.1007/s11207-014-0485-y |
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| Katalog-ID: |
SPR017766206 |
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|---|---|---|---|
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| 003 | DE-627 | ||
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| 008 | 201006s2014 xx |||||o 00| ||eng c | ||
| 024 | 7 | |a 10.1007/s11207-014-0485-y |2 doi | |
| 035 | |a (DE-627)SPR017766206 | ||
| 035 | |a (SPR)s11207-014-0485-y-e | ||
| 040 | |a DE-627 |b ger |c DE-627 |e rakwb | ||
| 041 | |a eng | ||
| 082 | 0 | 4 | |a 530 |q ASE |
| 084 | |a 39.51 |2 bkl | ||
| 100 | 1 | |a De Pontieu, B. |e verfasserin |4 aut | |
| 245 | 1 | 4 | |a The Interface Region Imaging Spectrograph (IRIS) |
| 264 | 1 | |c 2014 | |
| 336 | |a Text |b txt |2 rdacontent | ||
| 337 | |a Computermedien |b c |2 rdamedia | ||
| 338 | |a Online-Ressource |b cr |2 rdacarrier | ||
| 520 | |a Abstract 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 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 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. | ||
| 650 | 4 | |a Heating, chromospheric |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Heating, coronal |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Chromosphere, models |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Chromosphere, active |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Corona, active |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Magnetic fields, chromosphere |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Instrumentation and data management |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Spectrum, ultraviolet |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Title, A. M. |e verfasserin |4 aut | |
| 700 | 1 | |a Lemen, J. R. |e verfasserin |4 aut | |
| 700 | 1 | |a Kushner, G. D. |e verfasserin |4 aut | |
| 700 | 1 | |a Akin, D. J. |e verfasserin |4 aut | |
| 700 | 1 | |a Allard, B. |e verfasserin |4 aut | |
| 700 | 1 | |a Berger, T. |e verfasserin |4 aut | |
| 700 | 1 | |a Boerner, P. |e verfasserin |4 aut | |
| 700 | 1 | |a Cheung, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Chou, C. |e verfasserin |4 aut | |
| 700 | 1 | |a Drake, J. F. |e verfasserin |4 aut | |
| 700 | 1 | |a Duncan, D. W. |e verfasserin |4 aut | |
| 700 | 1 | |a Freeland, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Heyman, G. F. |e verfasserin |4 aut | |
| 700 | 1 | |a Hoffman, C. |e verfasserin |4 aut | |
| 700 | 1 | |a Hurlburt, N. E. |e verfasserin |4 aut | |
| 700 | 1 | |a Lindgren, R. W. |e verfasserin |4 aut | |
| 700 | 1 | |a Mathur, D. |e verfasserin |4 aut | |
| 700 | 1 | |a Rehse, R. |e verfasserin |4 aut | |
| 700 | 1 | |a Sabolish, D. |e verfasserin |4 aut | |
| 700 | 1 | |a Seguin, R. |e verfasserin |4 aut | |
| 700 | 1 | |a Schrijver, C. J. |e verfasserin |4 aut | |
| 700 | 1 | |a Tarbell, T. D. |e verfasserin |4 aut | |
| 700 | 1 | |a Wülser, J.-P. |e verfasserin |4 aut | |
| 700 | 1 | |a Wolfson, C. J. |e verfasserin |4 aut | |
| 700 | 1 | |a Yanari, C. |e verfasserin |4 aut | |
| 700 | 1 | |a Mudge, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Nguyen-Phuc, N. |e verfasserin |4 aut | |
| 700 | 1 | |a Timmons, R. |e verfasserin |4 aut | |
| 700 | 1 | |a van Bezooijen, R. |e verfasserin |4 aut | |
| 700 | 1 | |a Weingrod, I. |e verfasserin |4 aut | |
| 700 | 1 | |a Brookner, R. |e verfasserin |4 aut | |
| 700 | 1 | |a Butcher, G. |e verfasserin |4 aut | |
| 700 | 1 | |a Dougherty, B. |e verfasserin |4 aut | |
| 700 | 1 | |a Eder, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Knagenhjelm, V. |e verfasserin |4 aut | |
| 700 | 1 | |a Larsen, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Mansir, D. |e verfasserin |4 aut | |
| 700 | 1 | |a Phan, L. |e verfasserin |4 aut | |
| 700 | 1 | |a Boyle, P. |e verfasserin |4 aut | |
| 700 | 1 | |a Cheimets, P. N. |e verfasserin |4 aut | |
| 700 | 1 | |a DeLuca, E. E. |e verfasserin |4 aut | |
| 700 | 1 | |a Golub, L. |e verfasserin |4 aut | |
| 700 | 1 | |a Gates, R. |e verfasserin |4 aut | |
| 700 | 1 | |a Hertz, E. |e verfasserin |4 aut | |
| 700 | 1 | |a McKillop, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Park, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Perry, T. |e verfasserin |4 aut | |
| 700 | 1 | |a Podgorski, W. A. |e verfasserin |4 aut | |
| 700 | 1 | |a Reeves, K. |e verfasserin |4 aut | |
| 700 | 1 | |a Saar, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Testa, P. |e verfasserin |4 aut | |
| 700 | 1 | |a Tian, H. |e verfasserin |4 aut | |
| 700 | 1 | |a Weber, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Dunn, C. |e verfasserin |4 aut | |
| 700 | 1 | |a Eccles, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Jaeggli, S. A. |e verfasserin |4 aut | |
| 700 | 1 | |a Kankelborg, C. C. |e verfasserin |4 aut | |
| 700 | 1 | |a Mashburn, K. |e verfasserin |4 aut | |
| 700 | 1 | |a Pust, N. |e verfasserin |4 aut | |
| 700 | 1 | |a Springer, L. |e verfasserin |4 aut | |
| 700 | 1 | |a Carvalho, R. |e verfasserin |4 aut | |
| 700 | 1 | |a Kleint, L. |e verfasserin |4 aut | |
| 700 | 1 | |a Marmie, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Mazmanian, E. |e verfasserin |4 aut | |
| 700 | 1 | |a Pereira, T. M. D. |e verfasserin |4 aut | |
| 700 | 1 | |a Sawyer, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Strong, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Worden, S. P. |e verfasserin |4 aut | |
| 700 | 1 | |a Carlsson, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Hansteen, V. H. |e verfasserin |4 aut | |
| 700 | 1 | |a Leenaarts, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Wiesmann, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Aloise, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Chu, K.-C. |e verfasserin |4 aut | |
| 700 | 1 | |a Bush, R. I. |e verfasserin |4 aut | |
| 700 | 1 | |a Scherrer, P. H. |e verfasserin |4 aut | |
| 700 | 1 | |a Brekke, P. |e verfasserin |4 aut | |
| 700 | 1 | |a Martinez-Sykora, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Lites, B. W. |e verfasserin |4 aut | |
| 700 | 1 | |a McIntosh, S. W. |e verfasserin |4 aut | |
| 700 | 1 | |a Uitenbroek, H. |e verfasserin |4 aut | |
| 700 | 1 | |a Okamoto, T. J. |e verfasserin |4 aut | |
| 700 | 1 | |a Gummin, M. A. |e verfasserin |4 aut | |
| 700 | 1 | |a Auker, G. |e verfasserin |4 aut | |
| 700 | 1 | |a Jerram, P. |e verfasserin |4 aut | |
| 700 | 1 | |a Pool, P. |e verfasserin |4 aut | |
| 700 | 1 | |a Waltham, N. |e verfasserin |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Solar physics |d Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 |g 289(2014), 7 vom: 13. Feb., Seite 2733-2779 |w (DE-627)269019162 |w (DE-600)1473830-2 |x 1573-093X |7 nnns |
| 773 | 1 | 8 | |g volume:289 |g year:2014 |g number:7 |g day:13 |g month:02 |g pages:2733-2779 |
| 856 | 4 | 0 | |u https://dx.doi.org/10.1007/s11207-014-0485-y |z kostenfrei |3 Volltext |
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10.1007/s11207-014-0485-y doi (DE-627)SPR017766206 (SPR)s11207-014-0485-y-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl De Pontieu, B. verfasserin aut The Interface Region Imaging Spectrograph (IRIS) 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 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 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. Heating, chromospheric (dpeaa)DE-He213 Heating, coronal (dpeaa)DE-He213 Chromosphere, models (dpeaa)DE-He213 Chromosphere, active (dpeaa)DE-He213 Corona, active (dpeaa)DE-He213 Magnetic fields, chromosphere (dpeaa)DE-He213 Instrumentation and data management (dpeaa)DE-He213 Spectrum, ultraviolet (dpeaa)DE-He213 Title, A. M. verfasserin aut Lemen, J. R. verfasserin aut Kushner, G. D. verfasserin aut Akin, D. J. verfasserin aut Allard, B. verfasserin aut Berger, T. verfasserin aut Boerner, P. verfasserin aut Cheung, M. verfasserin aut Chou, C. verfasserin aut Drake, J. F. verfasserin aut Duncan, D. W. verfasserin aut Freeland, S. verfasserin aut Heyman, G. F. verfasserin aut Hoffman, C. verfasserin aut Hurlburt, N. E. verfasserin aut Lindgren, R. W. verfasserin aut Mathur, D. verfasserin aut Rehse, R. verfasserin aut Sabolish, D. verfasserin aut Seguin, R. verfasserin aut Schrijver, C. J. verfasserin aut Tarbell, T. D. verfasserin aut Wülser, J.-P. verfasserin aut Wolfson, C. J. verfasserin aut Yanari, C. verfasserin aut Mudge, J. verfasserin aut Nguyen-Phuc, N. verfasserin aut Timmons, R. verfasserin aut van Bezooijen, R. verfasserin aut Weingrod, I. verfasserin aut Brookner, R. verfasserin aut Butcher, G. verfasserin aut Dougherty, B. verfasserin aut Eder, J. verfasserin aut Knagenhjelm, V. verfasserin aut Larsen, S. verfasserin aut Mansir, D. verfasserin aut Phan, L. verfasserin aut Boyle, P. verfasserin aut Cheimets, P. N. verfasserin aut DeLuca, E. E. verfasserin aut Golub, L. verfasserin aut Gates, R. verfasserin aut Hertz, E. verfasserin aut McKillop, S. verfasserin aut Park, S. verfasserin aut Perry, T. verfasserin aut Podgorski, W. A. verfasserin aut Reeves, K. verfasserin aut Saar, S. verfasserin aut Testa, P. verfasserin aut Tian, H. verfasserin aut Weber, M. verfasserin aut Dunn, C. verfasserin aut Eccles, S. verfasserin aut Jaeggli, S. A. verfasserin aut Kankelborg, C. C. verfasserin aut Mashburn, K. verfasserin aut Pust, N. verfasserin aut Springer, L. verfasserin aut Carvalho, R. verfasserin aut Kleint, L. verfasserin aut Marmie, J. verfasserin aut Mazmanian, E. verfasserin aut Pereira, T. M. D. verfasserin aut Sawyer, S. verfasserin aut Strong, J. verfasserin aut Worden, S. P. verfasserin aut Carlsson, M. verfasserin aut Hansteen, V. H. verfasserin aut Leenaarts, J. verfasserin aut Wiesmann, M. verfasserin aut Aloise, J. verfasserin aut Chu, K.-C. verfasserin aut Bush, R. I. verfasserin aut Scherrer, P. H. verfasserin aut Brekke, P. verfasserin aut Martinez-Sykora, J. verfasserin aut Lites, B. W. verfasserin aut McIntosh, S. W. verfasserin aut Uitenbroek, H. verfasserin aut Okamoto, T. J. verfasserin aut Gummin, M. A. verfasserin aut Auker, G. verfasserin aut Jerram, P. verfasserin aut Pool, P. verfasserin aut Waltham, N. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 289(2014), 7 vom: 13. Feb., Seite 2733-2779 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:289 year:2014 number:7 day:13 month:02 pages:2733-2779 https://dx.doi.org/10.1007/s11207-014-0485-y kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 289 2014 7 13 02 2733-2779 |
| spelling |
10.1007/s11207-014-0485-y doi (DE-627)SPR017766206 (SPR)s11207-014-0485-y-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl De Pontieu, B. verfasserin aut The Interface Region Imaging Spectrograph (IRIS) 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 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 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. Heating, chromospheric (dpeaa)DE-He213 Heating, coronal (dpeaa)DE-He213 Chromosphere, models (dpeaa)DE-He213 Chromosphere, active (dpeaa)DE-He213 Corona, active (dpeaa)DE-He213 Magnetic fields, chromosphere (dpeaa)DE-He213 Instrumentation and data management (dpeaa)DE-He213 Spectrum, ultraviolet (dpeaa)DE-He213 Title, A. M. verfasserin aut Lemen, J. R. verfasserin aut Kushner, G. D. verfasserin aut Akin, D. J. verfasserin aut Allard, B. verfasserin aut Berger, T. verfasserin aut Boerner, P. verfasserin aut Cheung, M. verfasserin aut Chou, C. verfasserin aut Drake, J. F. verfasserin aut Duncan, D. W. verfasserin aut Freeland, S. verfasserin aut Heyman, G. F. verfasserin aut Hoffman, C. verfasserin aut Hurlburt, N. E. verfasserin aut Lindgren, R. W. verfasserin aut Mathur, D. verfasserin aut Rehse, R. verfasserin aut Sabolish, D. verfasserin aut Seguin, R. verfasserin aut Schrijver, C. J. verfasserin aut Tarbell, T. D. verfasserin aut Wülser, J.-P. verfasserin aut Wolfson, C. J. verfasserin aut Yanari, C. verfasserin aut Mudge, J. verfasserin aut Nguyen-Phuc, N. verfasserin aut Timmons, R. verfasserin aut van Bezooijen, R. verfasserin aut Weingrod, I. verfasserin aut Brookner, R. verfasserin aut Butcher, G. verfasserin aut Dougherty, B. verfasserin aut Eder, J. verfasserin aut Knagenhjelm, V. verfasserin aut Larsen, S. verfasserin aut Mansir, D. verfasserin aut Phan, L. verfasserin aut Boyle, P. verfasserin aut Cheimets, P. N. verfasserin aut DeLuca, E. E. verfasserin aut Golub, L. verfasserin aut Gates, R. verfasserin aut Hertz, E. verfasserin aut McKillop, S. verfasserin aut Park, S. verfasserin aut Perry, T. verfasserin aut Podgorski, W. A. verfasserin aut Reeves, K. verfasserin aut Saar, S. verfasserin aut Testa, P. verfasserin aut Tian, H. verfasserin aut Weber, M. verfasserin aut Dunn, C. verfasserin aut Eccles, S. verfasserin aut Jaeggli, S. A. verfasserin aut Kankelborg, C. C. verfasserin aut Mashburn, K. verfasserin aut Pust, N. verfasserin aut Springer, L. verfasserin aut Carvalho, R. verfasserin aut Kleint, L. verfasserin aut Marmie, J. verfasserin aut Mazmanian, E. verfasserin aut Pereira, T. M. D. verfasserin aut Sawyer, S. verfasserin aut Strong, J. verfasserin aut Worden, S. P. verfasserin aut Carlsson, M. verfasserin aut Hansteen, V. H. verfasserin aut Leenaarts, J. verfasserin aut Wiesmann, M. verfasserin aut Aloise, J. verfasserin aut Chu, K.-C. verfasserin aut Bush, R. I. verfasserin aut Scherrer, P. H. verfasserin aut Brekke, P. verfasserin aut Martinez-Sykora, J. verfasserin aut Lites, B. W. verfasserin aut McIntosh, S. W. verfasserin aut Uitenbroek, H. verfasserin aut Okamoto, T. J. verfasserin aut Gummin, M. A. verfasserin aut Auker, G. verfasserin aut Jerram, P. verfasserin aut Pool, P. verfasserin aut Waltham, N. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 289(2014), 7 vom: 13. Feb., Seite 2733-2779 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:289 year:2014 number:7 day:13 month:02 pages:2733-2779 https://dx.doi.org/10.1007/s11207-014-0485-y kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 289 2014 7 13 02 2733-2779 |
| allfields_unstemmed |
10.1007/s11207-014-0485-y doi (DE-627)SPR017766206 (SPR)s11207-014-0485-y-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl De Pontieu, B. verfasserin aut The Interface Region Imaging Spectrograph (IRIS) 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 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 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. Heating, chromospheric (dpeaa)DE-He213 Heating, coronal (dpeaa)DE-He213 Chromosphere, models (dpeaa)DE-He213 Chromosphere, active (dpeaa)DE-He213 Corona, active (dpeaa)DE-He213 Magnetic fields, chromosphere (dpeaa)DE-He213 Instrumentation and data management (dpeaa)DE-He213 Spectrum, ultraviolet (dpeaa)DE-He213 Title, A. M. verfasserin aut Lemen, J. R. verfasserin aut Kushner, G. D. verfasserin aut Akin, D. J. verfasserin aut Allard, B. verfasserin aut Berger, T. verfasserin aut Boerner, P. verfasserin aut Cheung, M. verfasserin aut Chou, C. verfasserin aut Drake, J. F. verfasserin aut Duncan, D. W. verfasserin aut Freeland, S. verfasserin aut Heyman, G. F. verfasserin aut Hoffman, C. verfasserin aut Hurlburt, N. E. verfasserin aut Lindgren, R. W. verfasserin aut Mathur, D. verfasserin aut Rehse, R. verfasserin aut Sabolish, D. verfasserin aut Seguin, R. verfasserin aut Schrijver, C. J. verfasserin aut Tarbell, T. D. verfasserin aut Wülser, J.-P. verfasserin aut Wolfson, C. J. verfasserin aut Yanari, C. verfasserin aut Mudge, J. verfasserin aut Nguyen-Phuc, N. verfasserin aut Timmons, R. verfasserin aut van Bezooijen, R. verfasserin aut Weingrod, I. verfasserin aut Brookner, R. verfasserin aut Butcher, G. verfasserin aut Dougherty, B. verfasserin aut Eder, J. verfasserin aut Knagenhjelm, V. verfasserin aut Larsen, S. verfasserin aut Mansir, D. verfasserin aut Phan, L. verfasserin aut Boyle, P. verfasserin aut Cheimets, P. N. verfasserin aut DeLuca, E. E. verfasserin aut Golub, L. verfasserin aut Gates, R. verfasserin aut Hertz, E. verfasserin aut McKillop, S. verfasserin aut Park, S. verfasserin aut Perry, T. verfasserin aut Podgorski, W. A. verfasserin aut Reeves, K. verfasserin aut Saar, S. verfasserin aut Testa, P. verfasserin aut Tian, H. verfasserin aut Weber, M. verfasserin aut Dunn, C. verfasserin aut Eccles, S. verfasserin aut Jaeggli, S. A. verfasserin aut Kankelborg, C. C. verfasserin aut Mashburn, K. verfasserin aut Pust, N. verfasserin aut Springer, L. verfasserin aut Carvalho, R. verfasserin aut Kleint, L. verfasserin aut Marmie, J. verfasserin aut Mazmanian, E. verfasserin aut Pereira, T. M. D. verfasserin aut Sawyer, S. verfasserin aut Strong, J. verfasserin aut Worden, S. P. verfasserin aut Carlsson, M. verfasserin aut Hansteen, V. H. verfasserin aut Leenaarts, J. verfasserin aut Wiesmann, M. verfasserin aut Aloise, J. verfasserin aut Chu, K.-C. verfasserin aut Bush, R. I. verfasserin aut Scherrer, P. H. verfasserin aut Brekke, P. verfasserin aut Martinez-Sykora, J. verfasserin aut Lites, B. W. verfasserin aut McIntosh, S. W. verfasserin aut Uitenbroek, H. verfasserin aut Okamoto, T. J. verfasserin aut Gummin, M. A. verfasserin aut Auker, G. verfasserin aut Jerram, P. verfasserin aut Pool, P. verfasserin aut Waltham, N. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 289(2014), 7 vom: 13. Feb., Seite 2733-2779 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:289 year:2014 number:7 day:13 month:02 pages:2733-2779 https://dx.doi.org/10.1007/s11207-014-0485-y kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 289 2014 7 13 02 2733-2779 |
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10.1007/s11207-014-0485-y doi (DE-627)SPR017766206 (SPR)s11207-014-0485-y-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl De Pontieu, B. verfasserin aut The Interface Region Imaging Spectrograph (IRIS) 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 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 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. Heating, chromospheric (dpeaa)DE-He213 Heating, coronal (dpeaa)DE-He213 Chromosphere, models (dpeaa)DE-He213 Chromosphere, active (dpeaa)DE-He213 Corona, active (dpeaa)DE-He213 Magnetic fields, chromosphere (dpeaa)DE-He213 Instrumentation and data management (dpeaa)DE-He213 Spectrum, ultraviolet (dpeaa)DE-He213 Title, A. M. verfasserin aut Lemen, J. R. verfasserin aut Kushner, G. D. verfasserin aut Akin, D. J. verfasserin aut Allard, B. verfasserin aut Berger, T. verfasserin aut Boerner, P. verfasserin aut Cheung, M. verfasserin aut Chou, C. verfasserin aut Drake, J. F. verfasserin aut Duncan, D. W. verfasserin aut Freeland, S. verfasserin aut Heyman, G. F. verfasserin aut Hoffman, C. verfasserin aut Hurlburt, N. E. verfasserin aut Lindgren, R. W. verfasserin aut Mathur, D. verfasserin aut Rehse, R. verfasserin aut Sabolish, D. verfasserin aut Seguin, R. verfasserin aut Schrijver, C. J. verfasserin aut Tarbell, T. D. verfasserin aut Wülser, J.-P. verfasserin aut Wolfson, C. J. verfasserin aut Yanari, C. verfasserin aut Mudge, J. verfasserin aut Nguyen-Phuc, N. verfasserin aut Timmons, R. verfasserin aut van Bezooijen, R. verfasserin aut Weingrod, I. verfasserin aut Brookner, R. verfasserin aut Butcher, G. verfasserin aut Dougherty, B. verfasserin aut Eder, J. verfasserin aut Knagenhjelm, V. verfasserin aut Larsen, S. verfasserin aut Mansir, D. verfasserin aut Phan, L. verfasserin aut Boyle, P. verfasserin aut Cheimets, P. N. verfasserin aut DeLuca, E. E. verfasserin aut Golub, L. verfasserin aut Gates, R. verfasserin aut Hertz, E. verfasserin aut McKillop, S. verfasserin aut Park, S. verfasserin aut Perry, T. verfasserin aut Podgorski, W. A. verfasserin aut Reeves, K. verfasserin aut Saar, S. verfasserin aut Testa, P. verfasserin aut Tian, H. verfasserin aut Weber, M. verfasserin aut Dunn, C. verfasserin aut Eccles, S. verfasserin aut Jaeggli, S. A. verfasserin aut Kankelborg, C. C. verfasserin aut Mashburn, K. verfasserin aut Pust, N. verfasserin aut Springer, L. verfasserin aut Carvalho, R. verfasserin aut Kleint, L. verfasserin aut Marmie, J. verfasserin aut Mazmanian, E. verfasserin aut Pereira, T. M. D. verfasserin aut Sawyer, S. verfasserin aut Strong, J. verfasserin aut Worden, S. P. verfasserin aut Carlsson, M. verfasserin aut Hansteen, V. H. verfasserin aut Leenaarts, J. verfasserin aut Wiesmann, M. verfasserin aut Aloise, J. verfasserin aut Chu, K.-C. verfasserin aut Bush, R. I. verfasserin aut Scherrer, P. H. verfasserin aut Brekke, P. verfasserin aut Martinez-Sykora, J. verfasserin aut Lites, B. W. verfasserin aut McIntosh, S. W. verfasserin aut Uitenbroek, H. verfasserin aut Okamoto, T. J. verfasserin aut Gummin, M. A. verfasserin aut Auker, G. verfasserin aut Jerram, P. verfasserin aut Pool, P. verfasserin aut Waltham, N. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 289(2014), 7 vom: 13. Feb., Seite 2733-2779 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:289 year:2014 number:7 day:13 month:02 pages:2733-2779 https://dx.doi.org/10.1007/s11207-014-0485-y kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 289 2014 7 13 02 2733-2779 |
| allfieldsSound |
10.1007/s11207-014-0485-y doi (DE-627)SPR017766206 (SPR)s11207-014-0485-y-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl De Pontieu, B. verfasserin aut The Interface Region Imaging Spectrograph (IRIS) 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 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 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. Heating, chromospheric (dpeaa)DE-He213 Heating, coronal (dpeaa)DE-He213 Chromosphere, models (dpeaa)DE-He213 Chromosphere, active (dpeaa)DE-He213 Corona, active (dpeaa)DE-He213 Magnetic fields, chromosphere (dpeaa)DE-He213 Instrumentation and data management (dpeaa)DE-He213 Spectrum, ultraviolet (dpeaa)DE-He213 Title, A. M. verfasserin aut Lemen, J. R. verfasserin aut Kushner, G. D. verfasserin aut Akin, D. J. verfasserin aut Allard, B. verfasserin aut Berger, T. verfasserin aut Boerner, P. verfasserin aut Cheung, M. verfasserin aut Chou, C. verfasserin aut Drake, J. F. verfasserin aut Duncan, D. W. verfasserin aut Freeland, S. verfasserin aut Heyman, G. F. verfasserin aut Hoffman, C. verfasserin aut Hurlburt, N. E. verfasserin aut Lindgren, R. W. verfasserin aut Mathur, D. verfasserin aut Rehse, R. verfasserin aut Sabolish, D. verfasserin aut Seguin, R. verfasserin aut Schrijver, C. J. verfasserin aut Tarbell, T. D. verfasserin aut Wülser, J.-P. verfasserin aut Wolfson, C. J. verfasserin aut Yanari, C. verfasserin aut Mudge, J. verfasserin aut Nguyen-Phuc, N. verfasserin aut Timmons, R. verfasserin aut van Bezooijen, R. verfasserin aut Weingrod, I. verfasserin aut Brookner, R. verfasserin aut Butcher, G. verfasserin aut Dougherty, B. verfasserin aut Eder, J. verfasserin aut Knagenhjelm, V. verfasserin aut Larsen, S. verfasserin aut Mansir, D. verfasserin aut Phan, L. verfasserin aut Boyle, P. verfasserin aut Cheimets, P. N. verfasserin aut DeLuca, E. E. verfasserin aut Golub, L. verfasserin aut Gates, R. verfasserin aut Hertz, E. verfasserin aut McKillop, S. verfasserin aut Park, S. verfasserin aut Perry, T. verfasserin aut Podgorski, W. A. verfasserin aut Reeves, K. verfasserin aut Saar, S. verfasserin aut Testa, P. verfasserin aut Tian, H. verfasserin aut Weber, M. verfasserin aut Dunn, C. verfasserin aut Eccles, S. verfasserin aut Jaeggli, S. A. verfasserin aut Kankelborg, C. C. verfasserin aut Mashburn, K. verfasserin aut Pust, N. verfasserin aut Springer, L. verfasserin aut Carvalho, R. verfasserin aut Kleint, L. verfasserin aut Marmie, J. verfasserin aut Mazmanian, E. verfasserin aut Pereira, T. M. D. verfasserin aut Sawyer, S. verfasserin aut Strong, J. verfasserin aut Worden, S. P. verfasserin aut Carlsson, M. verfasserin aut Hansteen, V. H. verfasserin aut Leenaarts, J. verfasserin aut Wiesmann, M. verfasserin aut Aloise, J. verfasserin aut Chu, K.-C. verfasserin aut Bush, R. I. verfasserin aut Scherrer, P. H. verfasserin aut Brekke, P. verfasserin aut Martinez-Sykora, J. verfasserin aut Lites, B. W. verfasserin aut McIntosh, S. W. verfasserin aut Uitenbroek, H. verfasserin aut Okamoto, T. J. verfasserin aut Gummin, M. A. verfasserin aut Auker, G. verfasserin aut Jerram, P. verfasserin aut Pool, P. verfasserin aut Waltham, N. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 289(2014), 7 vom: 13. Feb., Seite 2733-2779 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:289 year:2014 number:7 day:13 month:02 pages:2733-2779 https://dx.doi.org/10.1007/s11207-014-0485-y kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 289 2014 7 13 02 2733-2779 |
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Enthalten in Solar physics 289(2014), 7 vom: 13. Feb., Seite 2733-2779 volume:289 year:2014 number:7 day:13 month:02 pages:2733-2779 |
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De Pontieu, B. @@aut@@ Title, A. M. @@aut@@ Lemen, J. R. @@aut@@ Kushner, G. D. @@aut@@ Akin, D. J. @@aut@@ Allard, B. @@aut@@ Berger, T. @@aut@@ Boerner, P. @@aut@@ Cheung, M. @@aut@@ Chou, C. @@aut@@ Drake, J. F. @@aut@@ Duncan, D. W. @@aut@@ Freeland, S. @@aut@@ Heyman, G. F. @@aut@@ Hoffman, C. @@aut@@ Hurlburt, N. E. @@aut@@ Lindgren, R. W. @@aut@@ Mathur, D. @@aut@@ Rehse, R. @@aut@@ Sabolish, D. @@aut@@ Seguin, R. @@aut@@ Schrijver, C. J. @@aut@@ Tarbell, T. D. @@aut@@ Wülser, J.-P. @@aut@@ Wolfson, C. J. @@aut@@ Yanari, C. @@aut@@ Mudge, J. @@aut@@ Nguyen-Phuc, N. @@aut@@ Timmons, R. @@aut@@ van Bezooijen, R. @@aut@@ Weingrod, I. @@aut@@ Brookner, R. @@aut@@ Butcher, G. @@aut@@ Dougherty, B. @@aut@@ Eder, J. @@aut@@ Knagenhjelm, V. @@aut@@ Larsen, S. @@aut@@ Mansir, D. @@aut@@ Phan, L. @@aut@@ Boyle, P. @@aut@@ Cheimets, P. N. @@aut@@ DeLuca, E. E. @@aut@@ Golub, L. @@aut@@ Gates, R. @@aut@@ Hertz, E. @@aut@@ McKillop, S. @@aut@@ Park, S. @@aut@@ Perry, T. @@aut@@ Podgorski, W. A. @@aut@@ Reeves, K. @@aut@@ Saar, S. @@aut@@ Testa, P. @@aut@@ Tian, H. @@aut@@ Weber, M. @@aut@@ Dunn, C. @@aut@@ Eccles, S. @@aut@@ Jaeggli, S. A. @@aut@@ Kankelborg, C. C. @@aut@@ Mashburn, K. @@aut@@ Pust, N. @@aut@@ Springer, L. @@aut@@ Carvalho, R. @@aut@@ Kleint, L. @@aut@@ Marmie, J. @@aut@@ Mazmanian, E. @@aut@@ Pereira, T. M. D. @@aut@@ Sawyer, S. @@aut@@ Strong, J. @@aut@@ Worden, S. P. @@aut@@ Carlsson, M. @@aut@@ Hansteen, V. H. @@aut@@ Leenaarts, J. @@aut@@ Wiesmann, M. @@aut@@ Aloise, J. @@aut@@ Chu, K.-C. @@aut@@ Bush, R. I. @@aut@@ Scherrer, P. H. @@aut@@ Brekke, P. @@aut@@ Martinez-Sykora, J. @@aut@@ Lites, B. W. @@aut@@ McIntosh, S. W. @@aut@@ Uitenbroek, H. @@aut@@ Okamoto, T. J. @@aut@@ Gummin, M. A. @@aut@@ Auker, G. @@aut@@ Jerram, P. @@aut@@ Pool, P. @@aut@@ Waltham, N. @@aut@@ |
| publishDateDaySort_date |
2014-02-13T00:00:00Z |
| hierarchy_top_id |
269019162 |
| dewey-sort |
3530 |
| id |
SPR017766206 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">SPR017766206</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220111053522.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">201006s2014 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/s11207-014-0485-y</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)SPR017766206</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(SPR)s11207-014-0485-y-e</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">530</subfield><subfield code="q">ASE</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">39.51</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">De Pontieu, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The Interface Region Imaging Spectrograph (IRIS)</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2014</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract 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 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 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.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Heating, chromospheric</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Heating, coronal</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Chromosphere, models</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Chromosphere, active</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Corona, active</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Magnetic fields, chromosphere</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Instrumentation and data management</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Spectrum, ultraviolet</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Title, A. M.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Lemen, J. R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kushner, G. D.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Akin, D. 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De Pontieu, B. |
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De Pontieu, B. ddc 530 bkl 39.51 misc Heating, chromospheric misc Heating, coronal misc Chromosphere, models misc Chromosphere, active misc Corona, active misc Magnetic fields, chromosphere misc Instrumentation and data management misc Spectrum, ultraviolet The Interface Region Imaging Spectrograph (IRIS) |
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530 ASE 39.51 bkl The Interface Region Imaging Spectrograph (IRIS) Heating, chromospheric (dpeaa)DE-He213 Heating, coronal (dpeaa)DE-He213 Chromosphere, models (dpeaa)DE-He213 Chromosphere, active (dpeaa)DE-He213 Corona, active (dpeaa)DE-He213 Magnetic fields, chromosphere (dpeaa)DE-He213 Instrumentation and data management (dpeaa)DE-He213 Spectrum, ultraviolet (dpeaa)DE-He213 |
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The Interface Region Imaging Spectrograph (IRIS) |
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The Interface Region Imaging Spectrograph (IRIS) |
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De Pontieu, B. Title, A. M. Lemen, J. R. Kushner, G. D. Akin, D. J. Allard, B. Berger, T. Boerner, P. Cheung, M. Chou, C. Drake, J. F. Duncan, D. W. Freeland, S. Heyman, G. F. Hoffman, C. Hurlburt, N. E. Lindgren, R. W. Mathur, D. Rehse, R. Sabolish, D. Seguin, R. Schrijver, C. J. Tarbell, T. D. Wülser, J.-P. Wolfson, C. J. Yanari, C. Mudge, J. Nguyen-Phuc, N. Timmons, R. van Bezooijen, R. Weingrod, I. Brookner, R. Butcher, G. Dougherty, B. Eder, J. Knagenhjelm, V. Larsen, S. Mansir, D. Phan, L. Boyle, P. Cheimets, P. N. DeLuca, E. E. Golub, L. Gates, R. Hertz, E. McKillop, S. Park, S. Perry, T. Podgorski, W. A. Reeves, K. Saar, S. Testa, P. Tian, H. Weber, M. Dunn, C. Eccles, S. Jaeggli, S. A. Kankelborg, C. C. Mashburn, K. Pust, N. Springer, L. Carvalho, R. Kleint, L. Marmie, J. Mazmanian, E. Pereira, T. M. D. Sawyer, S. Strong, J. Worden, S. P. Carlsson, M. Hansteen, V. H. Leenaarts, J. Wiesmann, M. Aloise, J. Chu, K.-C. Bush, R. I. Scherrer, P. H. Brekke, P. Martinez-Sykora, J. Lites, B. W. McIntosh, S. W. Uitenbroek, H. Okamoto, T. J. Gummin, M. A. Auker, G. Jerram, P. Pool, P. Waltham, N. |
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interface region imaging spectrograph (iris) |
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The Interface Region Imaging Spectrograph (IRIS) |
| abstract |
Abstract 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 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 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. |
| abstractGer |
Abstract 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 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 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. |
| abstract_unstemmed |
Abstract 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 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 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. |
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The Interface Region Imaging Spectrograph (IRIS) |
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Title, A. M. Lemen, J. R. Kushner, G. D. Akin, D. J. Allard, B. Berger, T. Boerner, P. Cheung, M. Chou, C. Drake, J. F. Duncan, D. W. Freeland, S. Heyman, G. F. Hoffman, C. Hurlburt, N. E. Lindgren, R. W. Mathur, D. Rehse, R. Sabolish, D. Seguin, R. Schrijver, C. J. Tarbell, T. D. Wülser, J.-P. Wolfson, C. J. Yanari, C. Mudge, J. Nguyen-Phuc, N. Timmons, R. van Bezooijen, R. Weingrod, I. Brookner, R. Butcher, G. Dougherty, B. Eder, J. Knagenhjelm, V. Larsen, S. Mansir, D. Phan, L. Boyle, P. Cheimets, P. N. DeLuca, E. E. Golub, L. Gates, R. Hertz, E. McKillop, S. Park, S. Perry, T. Podgorski, W. A. Reeves, K. Saar, S. Testa, P. Tian, H. Weber, M. Dunn, C. Eccles, S. Jaeggli, S. A. Kankelborg, C. C. Mashburn, K. Pust, N. Springer, L. Carvalho, R. Kleint, L. Marmie, J. Mazmanian, E. Pereira, T. M. D. Sawyer, S. Strong, J. Worden, S. P. Carlsson, M. Hansteen, V. H. Leenaarts, J. Wiesmann, M. Aloise, J. Chu, K.-C. Bush, R. I. Scherrer, P. H. Brekke, P. Martinez-Sykora, J. Lites, B. W. McIntosh, S. W. Uitenbroek, H. Okamoto, T. J. Gummin, M. A. Auker, G. Jerram, P. Pool, P. Waltham, N. |
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Title, A. M. Lemen, J. R. Kushner, G. D. Akin, D. J. Allard, B. Berger, T. Boerner, P. Cheung, M. Chou, C. Drake, J. F. Duncan, D. W. Freeland, S. Heyman, G. F. Hoffman, C. Hurlburt, N. E. Lindgren, R. W. Mathur, D. Rehse, R. Sabolish, D. Seguin, R. Schrijver, C. J. Tarbell, T. D. Wülser, J.-P. Wolfson, C. J. Yanari, C. Mudge, J. Nguyen-Phuc, N. Timmons, R. van Bezooijen, R. Weingrod, I. Brookner, R. Butcher, G. Dougherty, B. Eder, J. Knagenhjelm, V. Larsen, S. Mansir, D. Phan, L. Boyle, P. Cheimets, P. N. DeLuca, E. E. Golub, L. Gates, R. Hertz, E. McKillop, S. Park, S. Perry, T. Podgorski, W. A. Reeves, K. Saar, S. Testa, P. Tian, H. Weber, M. Dunn, C. Eccles, S. Jaeggli, S. A. Kankelborg, C. C. Mashburn, K. Pust, N. Springer, L. Carvalho, R. Kleint, L. Marmie, J. Mazmanian, E. Pereira, T. M. D. Sawyer, S. Strong, J. Worden, S. P. Carlsson, M. Hansteen, V. H. Leenaarts, J. Wiesmann, M. Aloise, J. Chu, K.-C. Bush, R. I. Scherrer, P. H. Brekke, P. Martinez-Sykora, J. Lites, B. W. McIntosh, S. W. Uitenbroek, H. Okamoto, T. J. Gummin, M. A. Auker, G. Jerram, P. Pool, P. Waltham, N. |
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10.1007/s11207-014-0485-y |
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| score |
7.4022093 |