Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation
Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plas...
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| Autor*in: |
E. R. de Paula [verfasserIn] A. R. F. Martinon [verfasserIn] A. O. Moraes [verfasserIn] C. Carrano [verfasserIn] A. C. Neto [verfasserIn] P. Doherty [verfasserIn] K. Groves [verfasserIn] C. E. Valladares [verfasserIn] G. Crowley [verfasserIn] I. Azeem [verfasserIn] A. Reynolds [verfasserIn] D. M. Akos [verfasserIn] T. Walter [verfasserIn] T. L. Beach [verfasserIn] J.‐M. Slewaegen [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2021 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
In: Earth and Space Science - American Geophysical Union (AGU), 2015, 8(2021), 2, Seite n/a-n/a |
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| Übergeordnetes Werk: |
volume:8 ; year:2021 ; number:2 ; pages:n/a-n/a |
| Links: |
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| DOI / URN: |
10.1029/2020EA001314 |
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| Katalog-ID: |
DOAJ054430852 |
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| 245 | 1 | 0 | |a Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation |
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| 520 | |a Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. | ||
| 650 | 4 | |a amplitude and phase scintillation indexes | |
| 650 | 4 | |a GNSS receiver performance | |
| 650 | 4 | |a ionospheric irregularities | |
| 650 | 4 | |a ionospheric scintillation | |
| 650 | 4 | |a scintillation monitor | |
| 653 | 0 | |a Astronomy | |
| 653 | 0 | |a Geology | |
| 700 | 0 | |a A. R. F. Martinon |e verfasserin |4 aut | |
| 700 | 0 | |a A. O. Moraes |e verfasserin |4 aut | |
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| 700 | 0 | |a A. C. Neto |e verfasserin |4 aut | |
| 700 | 0 | |a P. Doherty |e verfasserin |4 aut | |
| 700 | 0 | |a K. Groves |e verfasserin |4 aut | |
| 700 | 0 | |a C. E. Valladares |e verfasserin |4 aut | |
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| 700 | 0 | |a D. M. Akos |e verfasserin |4 aut | |
| 700 | 0 | |a T. Walter |e verfasserin |4 aut | |
| 700 | 0 | |a T. L. Beach |e verfasserin |4 aut | |
| 700 | 0 | |a J.‐M. Slewaegen |e verfasserin |4 aut | |
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10.1029/2020EA001314 doi (DE-627)DOAJ054430852 (DE-599)DOAJ39a5f79ed45649de82634ac5d0d1b1d4 DE-627 ger DE-627 rakwb eng QB1-991 QE1-996.5 E. R. de Paula verfasserin aut Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. amplitude and phase scintillation indexes GNSS receiver performance ionospheric irregularities ionospheric scintillation scintillation monitor Astronomy Geology A. R. F. Martinon verfasserin aut A. O. Moraes verfasserin aut C. Carrano verfasserin aut A. C. Neto verfasserin aut P. Doherty verfasserin aut K. Groves verfasserin aut C. E. Valladares verfasserin aut G. Crowley verfasserin aut I. Azeem verfasserin aut A. Reynolds verfasserin aut D. M. Akos verfasserin aut T. Walter verfasserin aut T. L. Beach verfasserin aut J.‐M. Slewaegen verfasserin aut In Earth and Space Science American Geophysical Union (AGU), 2015 8(2021), 2, Seite n/a-n/a (DE-627)816694206 (DE-600)2807271-6 23335084 nnns volume:8 year:2021 number:2 pages:n/a-n/a https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/article/39a5f79ed45649de82634ac5d0d1b1d4 kostenfrei https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/toc/2333-5084 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 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_2068 GBV_ILN_2088 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_2522 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_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_4367 GBV_ILN_4700 AR 8 2021 2 n/a-n/a |
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10.1029/2020EA001314 doi (DE-627)DOAJ054430852 (DE-599)DOAJ39a5f79ed45649de82634ac5d0d1b1d4 DE-627 ger DE-627 rakwb eng QB1-991 QE1-996.5 E. R. de Paula verfasserin aut Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. amplitude and phase scintillation indexes GNSS receiver performance ionospheric irregularities ionospheric scintillation scintillation monitor Astronomy Geology A. R. F. Martinon verfasserin aut A. O. Moraes verfasserin aut C. Carrano verfasserin aut A. C. Neto verfasserin aut P. Doherty verfasserin aut K. Groves verfasserin aut C. E. Valladares verfasserin aut G. Crowley verfasserin aut I. Azeem verfasserin aut A. Reynolds verfasserin aut D. M. Akos verfasserin aut T. Walter verfasserin aut T. L. Beach verfasserin aut J.‐M. Slewaegen verfasserin aut In Earth and Space Science American Geophysical Union (AGU), 2015 8(2021), 2, Seite n/a-n/a (DE-627)816694206 (DE-600)2807271-6 23335084 nnns volume:8 year:2021 number:2 pages:n/a-n/a https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/article/39a5f79ed45649de82634ac5d0d1b1d4 kostenfrei https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/toc/2333-5084 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 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_2068 GBV_ILN_2088 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_2522 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_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_4367 GBV_ILN_4700 AR 8 2021 2 n/a-n/a |
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10.1029/2020EA001314 doi (DE-627)DOAJ054430852 (DE-599)DOAJ39a5f79ed45649de82634ac5d0d1b1d4 DE-627 ger DE-627 rakwb eng QB1-991 QE1-996.5 E. R. de Paula verfasserin aut Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. amplitude and phase scintillation indexes GNSS receiver performance ionospheric irregularities ionospheric scintillation scintillation monitor Astronomy Geology A. R. F. Martinon verfasserin aut A. O. Moraes verfasserin aut C. Carrano verfasserin aut A. C. Neto verfasserin aut P. Doherty verfasserin aut K. Groves verfasserin aut C. E. Valladares verfasserin aut G. Crowley verfasserin aut I. Azeem verfasserin aut A. Reynolds verfasserin aut D. M. Akos verfasserin aut T. Walter verfasserin aut T. L. Beach verfasserin aut J.‐M. Slewaegen verfasserin aut In Earth and Space Science American Geophysical Union (AGU), 2015 8(2021), 2, Seite n/a-n/a (DE-627)816694206 (DE-600)2807271-6 23335084 nnns volume:8 year:2021 number:2 pages:n/a-n/a https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/article/39a5f79ed45649de82634ac5d0d1b1d4 kostenfrei https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/toc/2333-5084 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 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_2068 GBV_ILN_2088 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_2522 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_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_4367 GBV_ILN_4700 AR 8 2021 2 n/a-n/a |
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10.1029/2020EA001314 doi (DE-627)DOAJ054430852 (DE-599)DOAJ39a5f79ed45649de82634ac5d0d1b1d4 DE-627 ger DE-627 rakwb eng QB1-991 QE1-996.5 E. R. de Paula verfasserin aut Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. amplitude and phase scintillation indexes GNSS receiver performance ionospheric irregularities ionospheric scintillation scintillation monitor Astronomy Geology A. R. F. Martinon verfasserin aut A. O. Moraes verfasserin aut C. Carrano verfasserin aut A. C. Neto verfasserin aut P. Doherty verfasserin aut K. Groves verfasserin aut C. E. Valladares verfasserin aut G. Crowley verfasserin aut I. Azeem verfasserin aut A. Reynolds verfasserin aut D. M. Akos verfasserin aut T. Walter verfasserin aut T. L. Beach verfasserin aut J.‐M. Slewaegen verfasserin aut In Earth and Space Science American Geophysical Union (AGU), 2015 8(2021), 2, Seite n/a-n/a (DE-627)816694206 (DE-600)2807271-6 23335084 nnns volume:8 year:2021 number:2 pages:n/a-n/a https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/article/39a5f79ed45649de82634ac5d0d1b1d4 kostenfrei https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/toc/2333-5084 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 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_2068 GBV_ILN_2088 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_2522 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_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_4367 GBV_ILN_4700 AR 8 2021 2 n/a-n/a |
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10.1029/2020EA001314 doi (DE-627)DOAJ054430852 (DE-599)DOAJ39a5f79ed45649de82634ac5d0d1b1d4 DE-627 ger DE-627 rakwb eng QB1-991 QE1-996.5 E. R. de Paula verfasserin aut Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. amplitude and phase scintillation indexes GNSS receiver performance ionospheric irregularities ionospheric scintillation scintillation monitor Astronomy Geology A. R. F. Martinon verfasserin aut A. O. Moraes verfasserin aut C. Carrano verfasserin aut A. C. Neto verfasserin aut P. Doherty verfasserin aut K. Groves verfasserin aut C. E. Valladares verfasserin aut G. Crowley verfasserin aut I. Azeem verfasserin aut A. Reynolds verfasserin aut D. M. Akos verfasserin aut T. Walter verfasserin aut T. L. Beach verfasserin aut J.‐M. Slewaegen verfasserin aut In Earth and Space Science American Geophysical Union (AGU), 2015 8(2021), 2, Seite n/a-n/a (DE-627)816694206 (DE-600)2807271-6 23335084 nnns volume:8 year:2021 number:2 pages:n/a-n/a https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/article/39a5f79ed45649de82634ac5d0d1b1d4 kostenfrei https://doi.org/10.1029/2020EA001314 kostenfrei https://doaj.org/toc/2333-5084 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 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_2068 GBV_ILN_2088 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_2522 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_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_4367 GBV_ILN_4700 AR 8 2021 2 n/a-n/a |
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E. R. de Paula @@aut@@ A. R. F. Martinon @@aut@@ A. O. Moraes @@aut@@ C. Carrano @@aut@@ A. C. Neto @@aut@@ P. Doherty @@aut@@ K. Groves @@aut@@ C. E. Valladares @@aut@@ G. Crowley @@aut@@ I. Azeem @@aut@@ A. Reynolds @@aut@@ D. M. Akos @@aut@@ T. Walter @@aut@@ T. L. Beach @@aut@@ J.‐M. Slewaegen @@aut@@ |
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E. R. de Paula |
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E. R. de Paula misc QB1-991 misc QE1-996.5 misc amplitude and phase scintillation indexes misc GNSS receiver performance misc ionospheric irregularities misc ionospheric scintillation misc scintillation monitor misc Astronomy misc Geology Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation |
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QB1-991 QE1-996.5 Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation amplitude and phase scintillation indexes GNSS receiver performance ionospheric irregularities ionospheric scintillation scintillation monitor |
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Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation |
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Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation |
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E. R. de Paula A. R. F. Martinon A. O. Moraes C. Carrano A. C. Neto P. Doherty K. Groves C. E. Valladares G. Crowley I. Azeem A. Reynolds D. M. Akos T. Walter T. L. Beach J.‐M. Slewaegen |
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performance of 6 different global navigation satellite system receivers at low latitude under moderate and strong scintillation |
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QB1-991 |
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Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation |
| abstract |
Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. |
| abstractGer |
Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. |
| abstract_unstemmed |
Abstract After sunset, in the equatorial regions ionospheric plasma irregularities are generated due to the generalized Rayleigh‐Taylor instability. Under favorable conditions these irregularities develop in the equatorial region while mapping along the magnetic field lines giving rise to large plasma depletion structures called Equatorial Plasma Bubbles with embedded smaller structures on their walls. The global navigation satellite system (GNSS) L1 band frequency is sensitive to irregularities of the size of 300–400 m in the first Fresnel zone, which cause scattering and diffraction of the signal and produce amplitude and/or phase scintillation. Severe scintillation of GNSS signals can in turn cause loss of lock of the receiver code and/or carrier loops. As a result, GNSS navigation and positioning solution can be adversely affected by the ionospheric scintillation. There are multiple GNSS receivers designed to monitor scintillations. These receivers are based on different hardware designs and use different methodologies to process the raw data. When using simultaneous data from different GNSS scintillation monitors it is important to evaluate and compare their performances under similar scintillation conditions. The scintillation monitoring techniques may be useful for many applications that use GNSS signal. The aim of this work is to evaluate the performance of six different GNSS receivers located at São José dos Campos (23.1°S, 45.8°W, dip latitude 17.3°S) during moderate and strong scintillation activity. The amplitude (S4) and phase (σϕ) scintillation indexes from these receivers were analyzed and compared for the nights February 20–21 and November 27–28, 2013. |
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Performance of 6 Different Global Navigation Satellite System Receivers at Low Latitude Under Moderate and Strong Scintillation |
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https://doi.org/10.1029/2020EA001314 https://doaj.org/article/39a5f79ed45649de82634ac5d0d1b1d4 https://doaj.org/toc/2333-5084 |
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A. R. F. Martinon A. O. Moraes C. Carrano A. C. Neto P. Doherty K. Groves C. E. Valladares G. Crowley I. Azeem A. Reynolds D. M. Akos T. Walter T. L. Beach J.‐M. Slewaegen |
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A. R. F. Martinon A. O. Moraes C. Carrano A. C. Neto P. Doherty K. Groves C. E. Valladares G. Crowley I. Azeem A. Reynolds D. M. Akos T. Walter T. L. Beach J.‐M. Slewaegen |
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10.1029/2020EA001314 |
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