The Upgraded CARISMA Magnetometer Array in the THEMIS Era
Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unifie...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Mann, I. R. [verfasserIn] Milling, D. K. [verfasserIn] Rae, I. J. [verfasserIn] Ozeke, L. G. [verfasserIn] Kale, A. [verfasserIn] Kale, Z. C. [verfasserIn] Murphy, K. R. [verfasserIn] Parent, A. [verfasserIn] Usanova, M. [verfasserIn] Pahud, D. M. [verfasserIn] Lee, E.-A. [verfasserIn] Amalraj, V. [verfasserIn] Wallis, D. D. [verfasserIn] Angelopoulos, V. [verfasserIn] Glassmeier, K.-H. [verfasserIn] Russell, C. T. [verfasserIn] Auster, H.-U. [verfasserIn] Singer, H. J. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2008 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Space science reviews - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962, 141(2008), 1-4 vom: Dez., Seite 413-451 |
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| Übergeordnetes Werk: |
volume:141 ; year:2008 ; number:1-4 ; month:12 ; pages:413-451 |
| Links: |
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| DOI / URN: |
10.1007/s11214-008-9457-6 |
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| Katalog-ID: |
SPR017807166 |
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| 100 | 1 | |a Mann, I. R. |e verfasserin |4 aut | |
| 245 | 1 | 4 | |a The Upgraded CARISMA Magnetometer Array in the THEMIS Era |
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| 520 | |a Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. | ||
| 650 | 4 | |a Magnetosphere |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Magnetometry |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Ionospheric currents |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Remote-sensing |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Substorms |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a ULF waves |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radiation belts |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Plasmasphere |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Cross-phase |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Discrete wavelet transform |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Field line resonance |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Milling, D. K. |e verfasserin |4 aut | |
| 700 | 1 | |a Rae, I. J. |e verfasserin |4 aut | |
| 700 | 1 | |a Ozeke, L. G. |e verfasserin |4 aut | |
| 700 | 1 | |a Kale, A. |e verfasserin |4 aut | |
| 700 | 1 | |a Kale, Z. C. |e verfasserin |4 aut | |
| 700 | 1 | |a Murphy, K. R. |e verfasserin |4 aut | |
| 700 | 1 | |a Parent, A. |e verfasserin |4 aut | |
| 700 | 1 | |a Usanova, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Pahud, D. M. |e verfasserin |4 aut | |
| 700 | 1 | |a Lee, E.-A. |e verfasserin |4 aut | |
| 700 | 1 | |a Amalraj, V. |e verfasserin |4 aut | |
| 700 | 1 | |a Wallis, D. D. |e verfasserin |4 aut | |
| 700 | 1 | |a Angelopoulos, V. |e verfasserin |4 aut | |
| 700 | 1 | |a Glassmeier, K.-H. |e verfasserin |4 aut | |
| 700 | 1 | |a Russell, C. T. |e verfasserin |4 aut | |
| 700 | 1 | |a Auster, H.-U. |e verfasserin |4 aut | |
| 700 | 1 | |a Singer, H. J. |e verfasserin |4 aut | |
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10.1007/s11214-008-9457-6 doi (DE-627)SPR017807166 (SPR)s11214-008-9457-6-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl Mann, I. R. verfasserin aut The Upgraded CARISMA Magnetometer Array in the THEMIS Era 2008 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. Magnetosphere (dpeaa)DE-He213 Magnetometry (dpeaa)DE-He213 Ionospheric currents (dpeaa)DE-He213 Remote-sensing (dpeaa)DE-He213 Substorms (dpeaa)DE-He213 ULF waves (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Plasmasphere (dpeaa)DE-He213 Cross-phase (dpeaa)DE-He213 Discrete wavelet transform (dpeaa)DE-He213 Field line resonance (dpeaa)DE-He213 Milling, D. K. verfasserin aut Rae, I. J. verfasserin aut Ozeke, L. G. verfasserin aut Kale, A. verfasserin aut Kale, Z. C. verfasserin aut Murphy, K. R. verfasserin aut Parent, A. verfasserin aut Usanova, M. verfasserin aut Pahud, D. M. verfasserin aut Lee, E.-A. verfasserin aut Amalraj, V. verfasserin aut Wallis, D. D. verfasserin aut Angelopoulos, V. verfasserin aut Glassmeier, K.-H. verfasserin aut Russell, C. T. verfasserin aut Auster, H.-U. verfasserin aut Singer, H. J. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 141(2008), 1-4 vom: Dez., Seite 413-451 (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:141 year:2008 number:1-4 month:12 pages:413-451 https://dx.doi.org/10.1007/s11214-008-9457-6 lizenzpflichtig 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_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_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 39.00 ASE AR 141 2008 1-4 12 413-451 |
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10.1007/s11214-008-9457-6 doi (DE-627)SPR017807166 (SPR)s11214-008-9457-6-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl Mann, I. R. verfasserin aut The Upgraded CARISMA Magnetometer Array in the THEMIS Era 2008 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. Magnetosphere (dpeaa)DE-He213 Magnetometry (dpeaa)DE-He213 Ionospheric currents (dpeaa)DE-He213 Remote-sensing (dpeaa)DE-He213 Substorms (dpeaa)DE-He213 ULF waves (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Plasmasphere (dpeaa)DE-He213 Cross-phase (dpeaa)DE-He213 Discrete wavelet transform (dpeaa)DE-He213 Field line resonance (dpeaa)DE-He213 Milling, D. K. verfasserin aut Rae, I. J. verfasserin aut Ozeke, L. G. verfasserin aut Kale, A. verfasserin aut Kale, Z. C. verfasserin aut Murphy, K. R. verfasserin aut Parent, A. verfasserin aut Usanova, M. verfasserin aut Pahud, D. M. verfasserin aut Lee, E.-A. verfasserin aut Amalraj, V. verfasserin aut Wallis, D. D. verfasserin aut Angelopoulos, V. verfasserin aut Glassmeier, K.-H. verfasserin aut Russell, C. T. verfasserin aut Auster, H.-U. verfasserin aut Singer, H. J. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 141(2008), 1-4 vom: Dez., Seite 413-451 (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:141 year:2008 number:1-4 month:12 pages:413-451 https://dx.doi.org/10.1007/s11214-008-9457-6 lizenzpflichtig 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_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_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 39.00 ASE AR 141 2008 1-4 12 413-451 |
| allfields_unstemmed |
10.1007/s11214-008-9457-6 doi (DE-627)SPR017807166 (SPR)s11214-008-9457-6-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl Mann, I. R. verfasserin aut The Upgraded CARISMA Magnetometer Array in the THEMIS Era 2008 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. Magnetosphere (dpeaa)DE-He213 Magnetometry (dpeaa)DE-He213 Ionospheric currents (dpeaa)DE-He213 Remote-sensing (dpeaa)DE-He213 Substorms (dpeaa)DE-He213 ULF waves (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Plasmasphere (dpeaa)DE-He213 Cross-phase (dpeaa)DE-He213 Discrete wavelet transform (dpeaa)DE-He213 Field line resonance (dpeaa)DE-He213 Milling, D. K. verfasserin aut Rae, I. J. verfasserin aut Ozeke, L. G. verfasserin aut Kale, A. verfasserin aut Kale, Z. C. verfasserin aut Murphy, K. R. verfasserin aut Parent, A. verfasserin aut Usanova, M. verfasserin aut Pahud, D. M. verfasserin aut Lee, E.-A. verfasserin aut Amalraj, V. verfasserin aut Wallis, D. D. verfasserin aut Angelopoulos, V. verfasserin aut Glassmeier, K.-H. verfasserin aut Russell, C. T. verfasserin aut Auster, H.-U. verfasserin aut Singer, H. J. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 141(2008), 1-4 vom: Dez., Seite 413-451 (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:141 year:2008 number:1-4 month:12 pages:413-451 https://dx.doi.org/10.1007/s11214-008-9457-6 lizenzpflichtig 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_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_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 39.00 ASE AR 141 2008 1-4 12 413-451 |
| allfieldsGer |
10.1007/s11214-008-9457-6 doi (DE-627)SPR017807166 (SPR)s11214-008-9457-6-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl Mann, I. R. verfasserin aut The Upgraded CARISMA Magnetometer Array in the THEMIS Era 2008 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. Magnetosphere (dpeaa)DE-He213 Magnetometry (dpeaa)DE-He213 Ionospheric currents (dpeaa)DE-He213 Remote-sensing (dpeaa)DE-He213 Substorms (dpeaa)DE-He213 ULF waves (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Plasmasphere (dpeaa)DE-He213 Cross-phase (dpeaa)DE-He213 Discrete wavelet transform (dpeaa)DE-He213 Field line resonance (dpeaa)DE-He213 Milling, D. K. verfasserin aut Rae, I. J. verfasserin aut Ozeke, L. G. verfasserin aut Kale, A. verfasserin aut Kale, Z. C. verfasserin aut Murphy, K. R. verfasserin aut Parent, A. verfasserin aut Usanova, M. verfasserin aut Pahud, D. M. verfasserin aut Lee, E.-A. verfasserin aut Amalraj, V. verfasserin aut Wallis, D. D. verfasserin aut Angelopoulos, V. verfasserin aut Glassmeier, K.-H. verfasserin aut Russell, C. T. verfasserin aut Auster, H.-U. verfasserin aut Singer, H. J. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 141(2008), 1-4 vom: Dez., Seite 413-451 (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:141 year:2008 number:1-4 month:12 pages:413-451 https://dx.doi.org/10.1007/s11214-008-9457-6 lizenzpflichtig 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_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_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 39.00 ASE AR 141 2008 1-4 12 413-451 |
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10.1007/s11214-008-9457-6 doi (DE-627)SPR017807166 (SPR)s11214-008-9457-6-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl Mann, I. R. verfasserin aut The Upgraded CARISMA Magnetometer Array in the THEMIS Era 2008 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. Magnetosphere (dpeaa)DE-He213 Magnetometry (dpeaa)DE-He213 Ionospheric currents (dpeaa)DE-He213 Remote-sensing (dpeaa)DE-He213 Substorms (dpeaa)DE-He213 ULF waves (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Plasmasphere (dpeaa)DE-He213 Cross-phase (dpeaa)DE-He213 Discrete wavelet transform (dpeaa)DE-He213 Field line resonance (dpeaa)DE-He213 Milling, D. K. verfasserin aut Rae, I. J. verfasserin aut Ozeke, L. G. verfasserin aut Kale, A. verfasserin aut Kale, Z. C. verfasserin aut Murphy, K. R. verfasserin aut Parent, A. verfasserin aut Usanova, M. verfasserin aut Pahud, D. M. verfasserin aut Lee, E.-A. verfasserin aut Amalraj, V. verfasserin aut Wallis, D. D. verfasserin aut Angelopoulos, V. verfasserin aut Glassmeier, K.-H. verfasserin aut Russell, C. T. verfasserin aut Auster, H.-U. verfasserin aut Singer, H. J. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 141(2008), 1-4 vom: Dez., Seite 413-451 (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:141 year:2008 number:1-4 month:12 pages:413-451 https://dx.doi.org/10.1007/s11214-008-9457-6 lizenzpflichtig 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_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_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 39.00 ASE AR 141 2008 1-4 12 413-451 |
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Enthalten in Space science reviews 141(2008), 1-4 vom: Dez., Seite 413-451 volume:141 year:2008 number:1-4 month:12 pages:413-451 |
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Mann, I. R. @@aut@@ Milling, D. K. @@aut@@ Rae, I. J. @@aut@@ Ozeke, L. G. @@aut@@ Kale, A. @@aut@@ Kale, Z. C. @@aut@@ Murphy, K. R. @@aut@@ Parent, A. @@aut@@ Usanova, M. @@aut@@ Pahud, D. M. @@aut@@ Lee, E.-A. @@aut@@ Amalraj, V. @@aut@@ Wallis, D. D. @@aut@@ Angelopoulos, V. @@aut@@ Glassmeier, K.-H. @@aut@@ Russell, C. T. @@aut@@ Auster, H.-U. @@aut@@ Singer, H. J. @@aut@@ |
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Mann, I. R. |
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Mann, I. R. ddc 600 bkl 39.00 misc Magnetosphere misc Magnetometry misc Ionospheric currents misc Remote-sensing misc Substorms misc ULF waves misc Radiation belts misc Plasmasphere misc Cross-phase misc Discrete wavelet transform misc Field line resonance The Upgraded CARISMA Magnetometer Array in the THEMIS Era |
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600 ASE 39.00 bkl The Upgraded CARISMA Magnetometer Array in the THEMIS Era Magnetosphere (dpeaa)DE-He213 Magnetometry (dpeaa)DE-He213 Ionospheric currents (dpeaa)DE-He213 Remote-sensing (dpeaa)DE-He213 Substorms (dpeaa)DE-He213 ULF waves (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Plasmasphere (dpeaa)DE-He213 Cross-phase (dpeaa)DE-He213 Discrete wavelet transform (dpeaa)DE-He213 Field line resonance (dpeaa)DE-He213 |
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ddc 600 bkl 39.00 misc Magnetosphere misc Magnetometry misc Ionospheric currents misc Remote-sensing misc Substorms misc ULF waves misc Radiation belts misc Plasmasphere misc Cross-phase misc Discrete wavelet transform misc Field line resonance |
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ddc 600 bkl 39.00 misc Magnetosphere misc Magnetometry misc Ionospheric currents misc Remote-sensing misc Substorms misc ULF waves misc Radiation belts misc Plasmasphere misc Cross-phase misc Discrete wavelet transform misc Field line resonance |
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ddc 600 bkl 39.00 misc Magnetosphere misc Magnetometry misc Ionospheric currents misc Remote-sensing misc Substorms misc ULF waves misc Radiation belts misc Plasmasphere misc Cross-phase misc Discrete wavelet transform misc Field line resonance |
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The Upgraded CARISMA Magnetometer Array in the THEMIS Era |
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The Upgraded CARISMA Magnetometer Array in the THEMIS Era |
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Mann, I. R. |
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Mann, I. R. Milling, D. K. Rae, I. J. Ozeke, L. G. Kale, A. Kale, Z. C. Murphy, K. R. Parent, A. Usanova, M. Pahud, D. M. Lee, E.-A. Amalraj, V. Wallis, D. D. Angelopoulos, V. Glassmeier, K.-H. Russell, C. T. Auster, H.-U. Singer, H. J. |
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Elektronische Aufsätze |
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Mann, I. R. |
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10.1007/s11214-008-9457-6 |
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verfasserin |
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upgraded carisma magnetometer array in the themis era |
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The Upgraded CARISMA Magnetometer Array in the THEMIS Era |
| abstract |
Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. |
| abstractGer |
Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. |
| abstract_unstemmed |
Abstract This review describes the infrastructure and capabilities of the expanded and upgraded Canadian Array for Realtime InvestigationS of Magnetic Activity (CARISMA) magnetometer array in the era of the THEMIS mission. Formerly operated as the Canadian Auroral Network for the OPEN Program Unified Study (CANOPUS) magnetometer array until 2003, CARISMA capabilities have been extended with the deployment of additional fluxgate magnetometer stations (to a total of 28), the upgrading of the fluxgate magnetometer cadence to a standard data product of 1 sample/s (raw sampled 8 samples/s data stream available on request), and the deployment of a new network of 8 pairs of induction coils (100 samples per second). CARISMA data, GPS-timed and backed up at remote field stations, is collected using Very Small Aperture Terminal (VSAT) satellite internet in real-time providing a real-time monitor for magnetic activity on a continent-wide scale. Operating under the magnetic footprint of the THEMIS probes, data from 5 CARISMA stations at 29–30 samples/s also forms part of the formal THEMIS ground-based observatory (GBO) data-stream. In addition to technical details, in this review we also outline some of the scientific capabilities of the CARISMA array for addressing all three of the scientific objectives of the THEMIS mission, namely: 1. Onset and evolution of the macroscale substorm instability, 2. Production of storm-time MeV electrons, and 3. Control of the solar wind-magnetosphere coupling by the bow shock, magnetosheath, and magnetopause. We further discuss some of the compelling questions related to these three THEMIS mission science objectives which can be addressed with CARISMA. |
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The Upgraded CARISMA Magnetometer Array in the THEMIS Era |
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https://dx.doi.org/10.1007/s11214-008-9457-6 |
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| author2 |
Milling, D. K. Rae, I. J. Ozeke, L. G. Kale, A. Kale, Z. C. Murphy, K. R. Parent, A. Usanova, M. Pahud, D. M. Lee, E.-A. Amalraj, V. Wallis, D. D. Angelopoulos, V. Glassmeier, K.-H. Russell, C. T. Auster, H.-U. Singer, H. J. |
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Milling, D. K. Rae, I. J. Ozeke, L. G. Kale, A. Kale, Z. C. Murphy, K. R. Parent, A. Usanova, M. Pahud, D. M. Lee, E.-A. Amalraj, V. Wallis, D. D. Angelopoulos, V. Glassmeier, K.-H. Russell, C. T. Auster, H.-U. Singer, H. J. |
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10.1007/s11214-008-9457-6 |
| up_date |
2024-07-03T15:19:43.878Z |
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| score |
7.401634 |