Infalling of nano-dust because of air drag on Uranus
Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uran...
Ausführliche Beschreibung
Autor*in: |
Shih, Hua-Shan [verfasserIn] Ip, Wing-Huen [verfasserIn] |
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Format: |
E-Artikel |
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Sprache: |
Englisch |
Erschienen: |
2023 |
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Schlagwörter: |
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Übergeordnetes Werk: |
Enthalten in: Planetary and space science - Kidlington [u.a.] : Elsevier Science, 1959, 237 |
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Übergeordnetes Werk: |
volume:237 |
DOI / URN: |
10.1016/j.pss.2023.105782 |
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Katalog-ID: |
ELV065041364 |
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245 | 1 | 0 | |a Infalling of nano-dust because of air drag on Uranus |
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520 | |a Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. | ||
650 | 4 | |a Uranus | |
650 | 4 | |a Planetary science | |
650 | 4 | |a Planetary rings | |
650 | 4 | |a Circumplanetary dust | |
700 | 1 | |a Ip, Wing-Huen |e verfasserin |4 aut | |
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10.1016/j.pss.2023.105782 doi (DE-627)ELV065041364 (ELSEVIER)S0032-0633(23)00151-4 DE-627 ger DE-627 rda eng 620 VZ 39.00 bkl 50.93 bkl Shih, Hua-Shan verfasserin (orcid)0009-0002-6805-5422 aut Infalling of nano-dust because of air drag on Uranus 2023 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. Uranus Planetary science Planetary rings Circumplanetary dust Ip, Wing-Huen verfasserin aut Enthalten in Planetary and space science Kidlington [u.a.] : Elsevier Science, 1959 237 Online-Ressource (DE-627)320505650 (DE-600)2012795-9 (DE-576)255266839 1873-5088 nnns volume:237 GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2106 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 Astronomie: Allgemeines VZ 50.93 Weltraumforschung VZ AR 237 |
spelling |
10.1016/j.pss.2023.105782 doi (DE-627)ELV065041364 (ELSEVIER)S0032-0633(23)00151-4 DE-627 ger DE-627 rda eng 620 VZ 39.00 bkl 50.93 bkl Shih, Hua-Shan verfasserin (orcid)0009-0002-6805-5422 aut Infalling of nano-dust because of air drag on Uranus 2023 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. Uranus Planetary science Planetary rings Circumplanetary dust Ip, Wing-Huen verfasserin aut Enthalten in Planetary and space science Kidlington [u.a.] : Elsevier Science, 1959 237 Online-Ressource (DE-627)320505650 (DE-600)2012795-9 (DE-576)255266839 1873-5088 nnns volume:237 GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2106 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 Astronomie: Allgemeines VZ 50.93 Weltraumforschung VZ AR 237 |
allfields_unstemmed |
10.1016/j.pss.2023.105782 doi (DE-627)ELV065041364 (ELSEVIER)S0032-0633(23)00151-4 DE-627 ger DE-627 rda eng 620 VZ 39.00 bkl 50.93 bkl Shih, Hua-Shan verfasserin (orcid)0009-0002-6805-5422 aut Infalling of nano-dust because of air drag on Uranus 2023 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. Uranus Planetary science Planetary rings Circumplanetary dust Ip, Wing-Huen verfasserin aut Enthalten in Planetary and space science Kidlington [u.a.] : Elsevier Science, 1959 237 Online-Ressource (DE-627)320505650 (DE-600)2012795-9 (DE-576)255266839 1873-5088 nnns volume:237 GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2106 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 Astronomie: Allgemeines VZ 50.93 Weltraumforschung VZ AR 237 |
allfieldsGer |
10.1016/j.pss.2023.105782 doi (DE-627)ELV065041364 (ELSEVIER)S0032-0633(23)00151-4 DE-627 ger DE-627 rda eng 620 VZ 39.00 bkl 50.93 bkl Shih, Hua-Shan verfasserin (orcid)0009-0002-6805-5422 aut Infalling of nano-dust because of air drag on Uranus 2023 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. Uranus Planetary science Planetary rings Circumplanetary dust Ip, Wing-Huen verfasserin aut Enthalten in Planetary and space science Kidlington [u.a.] : Elsevier Science, 1959 237 Online-Ressource (DE-627)320505650 (DE-600)2012795-9 (DE-576)255266839 1873-5088 nnns volume:237 GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2106 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 Astronomie: Allgemeines VZ 50.93 Weltraumforschung VZ AR 237 |
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10.1016/j.pss.2023.105782 doi (DE-627)ELV065041364 (ELSEVIER)S0032-0633(23)00151-4 DE-627 ger DE-627 rda eng 620 VZ 39.00 bkl 50.93 bkl Shih, Hua-Shan verfasserin (orcid)0009-0002-6805-5422 aut Infalling of nano-dust because of air drag on Uranus 2023 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. Uranus Planetary science Planetary rings Circumplanetary dust Ip, Wing-Huen verfasserin aut Enthalten in Planetary and space science Kidlington [u.a.] : Elsevier Science, 1959 237 Online-Ressource (DE-627)320505650 (DE-600)2012795-9 (DE-576)255266839 1873-5088 nnns volume:237 GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2106 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2470 GBV_ILN_2507 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 Astronomie: Allgemeines VZ 50.93 Weltraumforschung VZ AR 237 |
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Infalling of nano-dust because of air drag on Uranus |
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Infalling of nano-dust because of air drag on Uranus |
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Shih, Hua-Shan |
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Shih, Hua-Shan Ip, Wing-Huen |
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Elektronische Aufsätze |
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Shih, Hua-Shan |
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title_sort |
infalling of nano-dust because of air drag on uranus |
title_auth |
Infalling of nano-dust because of air drag on Uranus |
abstract |
Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. |
abstractGer |
Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. |
abstract_unstemmed |
Uranus and Saturn share similarities in terms of their atmospheric composition, which is primarily made up of hydrogen and helium, as well as their ring systems. Uranus has 13 known rings, which are divided into narrow main rings, dusty rings, and outer rings. Unlike Saturn’s broad ring system, Uranus’ inner narrow main rings are relatively narrow, and likely consist of dark, radiation-processed organics that range from centimeters to meters in size. We assume that Uranus may have a mechanism similar to Saturn where tiny particles fall on-to the planet due to its gravity and the dragging force of the upper atmosphere. The uncharged nano-dust particles in Uranus’ inner narrow rings will collide with neutral gas molecules in the exosphere and fall onto the planet. This work derives a Monte Carlo simulation of the orbital behavior of nano-dust particles in the inner narrow rings of Uranus. The model shows that the braking of the dust grain motion takes place at altitudes between 6000 km and 8000 km, and the dust particles are gradually captured into corotation with the planetary atmosphere below 4000 km altitude. The larger the dust particles are, the lower the altitude at which they will be assimilated into co-rotation. The lifetime of 1-nm dust particles to 1000 km-altitudes is estimated to be about 32.5 ± 18.8 h, and that of 30 nm is about 2770.0 ± 213.9 h. |
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Infalling of nano-dust because of air drag on Uranus |
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