Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes
An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCS...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Wang, Sicheng [verfasserIn] |
|---|
| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2015transfer abstract |
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| Schlagwörter: |
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| Umfang: |
7 |
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| Übergeordnetes Werk: |
Enthalten in: Posttranscriptional actions of triiodothyronine on - Bargi-Souza, Paula ELSEVIER, 2018, including COSPAR information bulletin : the official journal of the Committee on Space Research (COSPAR), a scientific committee of the International Council of Scientific Unions (ICSU), Amsterdam [u.a.] |
|---|---|
| Übergeordnetes Werk: |
volume:56 ; year:2015 ; number:5 ; day:1 ; month:09 ; pages:893-899 ; extent:7 |
| Links: |
|---|
| DOI / URN: |
10.1016/j.asr.2015.04.021 |
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| Katalog-ID: |
ELV023495022 |
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| 245 | 1 | 0 | |a Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes |
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| 520 | |a An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. | ||
| 520 | |a An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. | ||
| 650 | 7 | |a Vary-Chap scale height |2 Elsevier | |
| 650 | 7 | |a Topside ionosphere at midlatitudes |2 Elsevier | |
| 650 | 7 | |a IRI-2012 model |2 Elsevier | |
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| 700 | 1 | |a Fang, Hanxian |4 oth | |
| 773 | 0 | 8 | |i Enthalten in |n Elsevier Science |a Bargi-Souza, Paula ELSEVIER |t Posttranscriptional actions of triiodothyronine on |d 2018 |d including COSPAR information bulletin : the official journal of the Committee on Space Research (COSPAR), a scientific committee of the International Council of Scientific Unions (ICSU) |g Amsterdam [u.a.] |w (DE-627)ELV000905844 |
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10.1016/j.asr.2015.04.021 doi GBVA2015008000020.pica (DE-627)ELV023495022 (ELSEVIER)S0273-1177(15)00298-7 DE-627 ger DE-627 rakwb eng 520 620 520 DE-600 620 DE-600 610 570 VZ 44.89 bkl Wang, Sicheng verfasserin aut Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes 2015transfer abstract 7 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. Vary-Chap scale height Elsevier Topside ionosphere at midlatitudes Elsevier IRI-2012 model Elsevier Huang, Sixun oth Fang, Hanxian oth Enthalten in Elsevier Science Bargi-Souza, Paula ELSEVIER Posttranscriptional actions of triiodothyronine on 2018 including COSPAR information bulletin : the official journal of the Committee on Space Research (COSPAR), a scientific committee of the International Council of Scientific Unions (ICSU) Amsterdam [u.a.] (DE-627)ELV000905844 volume:56 year:2015 number:5 day:1 month:09 pages:893-899 extent:7 https://doi.org/10.1016/j.asr.2015.04.021 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA 44.89 Endokrinologie VZ AR 56 2015 5 1 0901 893-899 7 045F 520 |
| spelling |
10.1016/j.asr.2015.04.021 doi GBVA2015008000020.pica (DE-627)ELV023495022 (ELSEVIER)S0273-1177(15)00298-7 DE-627 ger DE-627 rakwb eng 520 620 520 DE-600 620 DE-600 610 570 VZ 44.89 bkl Wang, Sicheng verfasserin aut Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes 2015transfer abstract 7 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. Vary-Chap scale height Elsevier Topside ionosphere at midlatitudes Elsevier IRI-2012 model Elsevier Huang, Sixun oth Fang, Hanxian oth Enthalten in Elsevier Science Bargi-Souza, Paula ELSEVIER Posttranscriptional actions of triiodothyronine on 2018 including COSPAR information bulletin : the official journal of the Committee on Space Research (COSPAR), a scientific committee of the International Council of Scientific Unions (ICSU) Amsterdam [u.a.] (DE-627)ELV000905844 volume:56 year:2015 number:5 day:1 month:09 pages:893-899 extent:7 https://doi.org/10.1016/j.asr.2015.04.021 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA 44.89 Endokrinologie VZ AR 56 2015 5 1 0901 893-899 7 045F 520 |
| allfields_unstemmed |
10.1016/j.asr.2015.04.021 doi GBVA2015008000020.pica (DE-627)ELV023495022 (ELSEVIER)S0273-1177(15)00298-7 DE-627 ger DE-627 rakwb eng 520 620 520 DE-600 620 DE-600 610 570 VZ 44.89 bkl Wang, Sicheng verfasserin aut Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes 2015transfer abstract 7 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. Vary-Chap scale height Elsevier Topside ionosphere at midlatitudes Elsevier IRI-2012 model Elsevier Huang, Sixun oth Fang, Hanxian oth Enthalten in Elsevier Science Bargi-Souza, Paula ELSEVIER Posttranscriptional actions of triiodothyronine on 2018 including COSPAR information bulletin : the official journal of the Committee on Space Research (COSPAR), a scientific committee of the International Council of Scientific Unions (ICSU) Amsterdam [u.a.] (DE-627)ELV000905844 volume:56 year:2015 number:5 day:1 month:09 pages:893-899 extent:7 https://doi.org/10.1016/j.asr.2015.04.021 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA 44.89 Endokrinologie VZ AR 56 2015 5 1 0901 893-899 7 045F 520 |
| allfieldsGer |
10.1016/j.asr.2015.04.021 doi GBVA2015008000020.pica (DE-627)ELV023495022 (ELSEVIER)S0273-1177(15)00298-7 DE-627 ger DE-627 rakwb eng 520 620 520 DE-600 620 DE-600 610 570 VZ 44.89 bkl Wang, Sicheng verfasserin aut Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes 2015transfer abstract 7 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. Vary-Chap scale height Elsevier Topside ionosphere at midlatitudes Elsevier IRI-2012 model Elsevier Huang, Sixun oth Fang, Hanxian oth Enthalten in Elsevier Science Bargi-Souza, Paula ELSEVIER Posttranscriptional actions of triiodothyronine on 2018 including COSPAR information bulletin : the official journal of the Committee on Space Research (COSPAR), a scientific committee of the International Council of Scientific Unions (ICSU) Amsterdam [u.a.] (DE-627)ELV000905844 volume:56 year:2015 number:5 day:1 month:09 pages:893-899 extent:7 https://doi.org/10.1016/j.asr.2015.04.021 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA 44.89 Endokrinologie VZ AR 56 2015 5 1 0901 893-899 7 045F 520 |
| allfieldsSound |
10.1016/j.asr.2015.04.021 doi GBVA2015008000020.pica (DE-627)ELV023495022 (ELSEVIER)S0273-1177(15)00298-7 DE-627 ger DE-627 rakwb eng 520 620 520 DE-600 620 DE-600 610 570 VZ 44.89 bkl Wang, Sicheng verfasserin aut Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes 2015transfer abstract 7 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. Vary-Chap scale height Elsevier Topside ionosphere at midlatitudes Elsevier IRI-2012 model Elsevier Huang, Sixun oth Fang, Hanxian oth Enthalten in Elsevier Science Bargi-Souza, Paula ELSEVIER Posttranscriptional actions of triiodothyronine on 2018 including COSPAR information bulletin : the official journal of the Committee on Space Research (COSPAR), a scientific committee of the International Council of Scientific Unions (ICSU) Amsterdam [u.a.] (DE-627)ELV000905844 volume:56 year:2015 number:5 day:1 month:09 pages:893-899 extent:7 https://doi.org/10.1016/j.asr.2015.04.021 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA 44.89 Endokrinologie VZ AR 56 2015 5 1 0901 893-899 7 045F 520 |
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Enthalten in Posttranscriptional actions of triiodothyronine on Amsterdam [u.a.] volume:56 year:2015 number:5 day:1 month:09 pages:893-899 extent:7 |
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topside ionospheric vary-chap scale height retrieved from the cosmic/formosat-3 data at midlatitudes |
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Topside ionospheric Vary-Chap scale height retrieved from the COSMIC/FORMOSAT-3 data at midlatitudes |
| abstract |
An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. |
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An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. |
| abstract_unstemmed |
An α-Chapman function with a continuously varying scale height can be used to describe the topside F2 vertical electron density profile that seamlessly connects the ionosphere with the plasmasphere. The local time, seasonal, latitudinal and longitudinal variations of the Vary-Chap scale heights (VCSHs) in 2007 at midlatitudes are investigated using the electron density profiles retrieved from the COSMIC/FORMOSAT-3 ionospheric radio occultation observations. The results show that the VCSHs at 400–550km have prominent altitudinal dependence and diurnal, seasonal variations, and are not tightly correlated with the neutral or plasma-scale heights. The values of the VCSHs in the daytime are larger than those in the nighttime in spring, autumn and winter, comparable and even larger nighttime ones can be detected in summer. The VCSHs change slowly from the midnight to predawn and change abruptly around the sunrise, and the daytime maximum are in winter and the minimum are in summer. In the midlatitudes, the daytime VCSHs decrease with latitude, while at nighttime, the latitudinal changes of VCSHs are not so distinct. The daytime VCSHs in northern hemisphere are larger than those in southern hemisphere. The VCSHs have complicated longitudinal variations and no obvious wavelike structures. What is more, the IRI-2012 model is capable of reproducing the trend of the diurnal, seasonal and latitudinal VCSH variations. But the values have large differences with those retrieved from the COSMIC/FORMOSAT-3 data. |
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