The Latest Jovian Trapped Proton and Heavy Ion Models
Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) p...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Garrett, Henry [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2017 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: IEEE transactions on nuclear science - New York, NY : IEEE, 1963, PP(2017), 99, Seite 2802-1 |
|---|---|
| Übergeordnetes Werk: |
volume:PP ; year:2017 ; number:99 ; pages:2802-1 |
| Links: |
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| DOI / URN: |
10.1109/TNS.2017.2755618 |
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| Katalog-ID: |
OLC1998989488 |
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| 520 | |a Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). | ||
| 520 | |a Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). | ||
| 650 | 4 | |a Magnetic fields | |
| 650 | 4 | |a Ions | |
| 650 | 4 | |a Protons | |
| 650 | 4 | |a Galileo interim radiation electron (GIRE) | |
| 650 | 4 | |a Belts | |
| 650 | 4 | |a GIRE | |
| 650 | 4 | |a Jupiter | |
| 650 | 4 | |a HIC | |
| 650 | 4 | |a Electron traps | |
| 650 | 4 | |a heavy ion counter (HIC) | |
| 650 | 4 | |a Jovian radiation belt | |
| 650 | 4 | |a Data models | |
| 700 | 1 | |a Garrett, Henry |4 oth | |
| 700 | 1 | |a Jun, Insoo |4 oth | |
| 700 | 1 | |a Jun, Insoo |4 oth | |
| 700 | 1 | |a Evans, Robin |4 oth | |
| 700 | 1 | |a Evans, Robin |4 oth | |
| 700 | 1 | |a Kim, Wousik |4 oth | |
| 700 | 1 | |a Kim, Wousik |4 oth | |
| 700 | 1 | |a Brinza, David |4 oth | |
| 700 | 1 | |a Brinza, David |4 oth | |
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10.1109/TNS.2017.2755618 doi PQ20171228 (DE-627)OLC1998989488 (DE-599)GBVOLC1998989488 (PRQ)i654-d6ac47eaae8c08f741570b34be7cfc707d560e6376a3498bbc4c82819744231a0 (KEY)0054996720170000000009902802latestjoviantrappedprotonandheavyionmodels DE-627 ger DE-627 rakwb eng 620 DNB Garrett, Henry verfasserin aut The Latest Jovian Trapped Proton and Heavy Ion Models 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Magnetic fields Ions Protons Galileo interim radiation electron (GIRE) Belts GIRE Jupiter HIC Electron traps heavy ion counter (HIC) Jovian radiation belt Data models Garrett, Henry oth Jun, Insoo oth Jun, Insoo oth Evans, Robin oth Evans, Robin oth Kim, Wousik oth Kim, Wousik oth Brinza, David oth Brinza, David oth Enthalten in IEEE transactions on nuclear science New York, NY : IEEE, 1963 PP(2017), 99, Seite 2802-1 (DE-627)129547352 (DE-600)218510-6 (DE-576)014998238 0018-9499 nnns volume:PP year:2017 number:99 pages:2802-1 http://dx.doi.org/10.1109/TNS.2017.2755618 Volltext http://ieeexplore.ieee.org/document/8048555 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-PHA GBV_ILN_70 AR PP 2017 99 2802-1 |
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10.1109/TNS.2017.2755618 doi PQ20171228 (DE-627)OLC1998989488 (DE-599)GBVOLC1998989488 (PRQ)i654-d6ac47eaae8c08f741570b34be7cfc707d560e6376a3498bbc4c82819744231a0 (KEY)0054996720170000000009902802latestjoviantrappedprotonandheavyionmodels DE-627 ger DE-627 rakwb eng 620 DNB Garrett, Henry verfasserin aut The Latest Jovian Trapped Proton and Heavy Ion Models 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Magnetic fields Ions Protons Galileo interim radiation electron (GIRE) Belts GIRE Jupiter HIC Electron traps heavy ion counter (HIC) Jovian radiation belt Data models Garrett, Henry oth Jun, Insoo oth Jun, Insoo oth Evans, Robin oth Evans, Robin oth Kim, Wousik oth Kim, Wousik oth Brinza, David oth Brinza, David oth Enthalten in IEEE transactions on nuclear science New York, NY : IEEE, 1963 PP(2017), 99, Seite 2802-1 (DE-627)129547352 (DE-600)218510-6 (DE-576)014998238 0018-9499 nnns volume:PP year:2017 number:99 pages:2802-1 http://dx.doi.org/10.1109/TNS.2017.2755618 Volltext http://ieeexplore.ieee.org/document/8048555 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-PHA GBV_ILN_70 AR PP 2017 99 2802-1 |
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10.1109/TNS.2017.2755618 doi PQ20171228 (DE-627)OLC1998989488 (DE-599)GBVOLC1998989488 (PRQ)i654-d6ac47eaae8c08f741570b34be7cfc707d560e6376a3498bbc4c82819744231a0 (KEY)0054996720170000000009902802latestjoviantrappedprotonandheavyionmodels DE-627 ger DE-627 rakwb eng 620 DNB Garrett, Henry verfasserin aut The Latest Jovian Trapped Proton and Heavy Ion Models 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Magnetic fields Ions Protons Galileo interim radiation electron (GIRE) Belts GIRE Jupiter HIC Electron traps heavy ion counter (HIC) Jovian radiation belt Data models Garrett, Henry oth Jun, Insoo oth Jun, Insoo oth Evans, Robin oth Evans, Robin oth Kim, Wousik oth Kim, Wousik oth Brinza, David oth Brinza, David oth Enthalten in IEEE transactions on nuclear science New York, NY : IEEE, 1963 PP(2017), 99, Seite 2802-1 (DE-627)129547352 (DE-600)218510-6 (DE-576)014998238 0018-9499 nnns volume:PP year:2017 number:99 pages:2802-1 http://dx.doi.org/10.1109/TNS.2017.2755618 Volltext http://ieeexplore.ieee.org/document/8048555 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-PHA GBV_ILN_70 AR PP 2017 99 2802-1 |
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10.1109/TNS.2017.2755618 doi PQ20171228 (DE-627)OLC1998989488 (DE-599)GBVOLC1998989488 (PRQ)i654-d6ac47eaae8c08f741570b34be7cfc707d560e6376a3498bbc4c82819744231a0 (KEY)0054996720170000000009902802latestjoviantrappedprotonandheavyionmodels DE-627 ger DE-627 rakwb eng 620 DNB Garrett, Henry verfasserin aut The Latest Jovian Trapped Proton and Heavy Ion Models 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Magnetic fields Ions Protons Galileo interim radiation electron (GIRE) Belts GIRE Jupiter HIC Electron traps heavy ion counter (HIC) Jovian radiation belt Data models Garrett, Henry oth Jun, Insoo oth Jun, Insoo oth Evans, Robin oth Evans, Robin oth Kim, Wousik oth Kim, Wousik oth Brinza, David oth Brinza, David oth Enthalten in IEEE transactions on nuclear science New York, NY : IEEE, 1963 PP(2017), 99, Seite 2802-1 (DE-627)129547352 (DE-600)218510-6 (DE-576)014998238 0018-9499 nnns volume:PP year:2017 number:99 pages:2802-1 http://dx.doi.org/10.1109/TNS.2017.2755618 Volltext http://ieeexplore.ieee.org/document/8048555 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-PHA GBV_ILN_70 AR PP 2017 99 2802-1 |
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10.1109/TNS.2017.2755618 doi PQ20171228 (DE-627)OLC1998989488 (DE-599)GBVOLC1998989488 (PRQ)i654-d6ac47eaae8c08f741570b34be7cfc707d560e6376a3498bbc4c82819744231a0 (KEY)0054996720170000000009902802latestjoviantrappedprotonandheavyionmodels DE-627 ger DE-627 rakwb eng 620 DNB Garrett, Henry verfasserin aut The Latest Jovian Trapped Proton and Heavy Ion Models 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Magnetic fields Ions Protons Galileo interim radiation electron (GIRE) Belts GIRE Jupiter HIC Electron traps heavy ion counter (HIC) Jovian radiation belt Data models Garrett, Henry oth Jun, Insoo oth Jun, Insoo oth Evans, Robin oth Evans, Robin oth Kim, Wousik oth Kim, Wousik oth Brinza, David oth Brinza, David oth Enthalten in IEEE transactions on nuclear science New York, NY : IEEE, 1963 PP(2017), 99, Seite 2802-1 (DE-627)129547352 (DE-600)218510-6 (DE-576)014998238 0018-9499 nnns volume:PP year:2017 number:99 pages:2802-1 http://dx.doi.org/10.1109/TNS.2017.2755618 Volltext http://ieeexplore.ieee.org/document/8048555 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-PHA GBV_ILN_70 AR PP 2017 99 2802-1 |
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Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). |
| abstractGer |
Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). |
| abstract_unstemmed |
Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian trapped radiation environment are a pre-requisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nucleon for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo Energetic Particle Detector (EPD) and Heavy Ion Counter (HIC) have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose (TID) and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mils of coverglass). In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays). |
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In contrast, although they will be described here for completeness, the Jovian trapped heavy ions are typically not a driving environmental consideration for SEE evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays).</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Jupiter possesses the harshest trapped radiation environment in the solar system. Models of the Jovian-trapped radiation environment are a prerequisite for planning missions to this extreme environment. The high energy (>0.1 MeV for electrons and >1 MeV/nuc for protons and heavier ions) particle environment drives the shielding and microelectronic parts design for a spacecraft. Recently, models based on the measurements by the Galileo energetic particle detector and heavy ion counter have been updated for the trapped protons and heavy ions. The purpose of this paper is to describe these changes to the proton and heavy ion models and demonstrate their application to and relative impact on mission design. While trapped electrons at Jupiter dominate for total ionizing dose and displacement damage dose for typically shielded parts/materials (e.g., with ~100 mil or 2.54 mm of aluminum shielding), trapped protons can be a significant contributor to lightly shielded components (e.g., solar cells under 10-20 mil of cover glass). In contrast, although they will be described here for completeness, the Jovian-trapped heavy ions are typically not a driving environmental consideration for single event effects evaluations (their energies are so low that a small amount of shielding will attenuate the fluxes to levels below the interplanetary solar energetic particle and galactic cosmic rays).</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Magnetic fields</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Ions</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Protons</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Galileo interim radiation electron (GIRE)</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Belts</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">GIRE</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Jupiter</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">HIC</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Electron traps</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">heavy ion counter (HIC)</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Jovian radiation belt</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Data models</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Garrett, Henry</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Jun, Insoo</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Jun, Insoo</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Evans, Robin</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Evans, Robin</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kim, Wousik</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kim, Wousik</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Brinza, David</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Brinza, David</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">IEEE transactions on nuclear science</subfield><subfield code="d">New York, NY : IEEE, 1963</subfield><subfield code="g">PP(2017), 99, Seite 2802-1</subfield><subfield code="w">(DE-627)129547352</subfield><subfield code="w">(DE-600)218510-6</subfield><subfield code="w">(DE-576)014998238</subfield><subfield code="x">0018-9499</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:PP</subfield><subfield code="g">year:2017</subfield><subfield code="g">number:99</subfield><subfield code="g">pages:2802-1</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">http://dx.doi.org/10.1109/TNS.2017.2755618</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">http://ieeexplore.ieee.org/document/8048555</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-TEC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHA</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">PP</subfield><subfield code="j">2017</subfield><subfield code="e">99</subfield><subfield code="h">2802-1</subfield></datafield></record></collection>
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