Mars: Clearing of the 1971 dust storm
A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cann...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1974 |
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| Reproduktion: |
Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 |
|---|---|
| Übergeordnetes Werk: |
in: Icarus - Amsterdam : Elsevier, 21(1974), 1, Seite 28-34 |
| Übergeordnetes Werk: |
volume:21 ; year:1974 ; number:1 ; pages:28-34 |
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NLEJ180420941 |
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| 520 | |a A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. | ||
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(DE-627)NLEJ180420941 (DE-599)GBVNLZ180420941 DE-627 ger DE-627 rakwb eng Mars: Clearing of the 1971 dust storm 1974 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, W.K. oth Price, M.J. oth in Icarus Amsterdam : Elsevier 21(1974), 1, Seite 28-34 (DE-627)NLEJ176861017 (DE-600)1467991-7 0019-1035 nnns volume:21 year:1974 number:1 pages:28-34 http://dx.doi.org/10.1016/0019-1035(74)90087-6 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 21 1974 1 28-34 |
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(DE-627)NLEJ180420941 (DE-599)GBVNLZ180420941 DE-627 ger DE-627 rakwb eng Mars: Clearing of the 1971 dust storm 1974 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, W.K. oth Price, M.J. oth in Icarus Amsterdam : Elsevier 21(1974), 1, Seite 28-34 (DE-627)NLEJ176861017 (DE-600)1467991-7 0019-1035 nnns volume:21 year:1974 number:1 pages:28-34 http://dx.doi.org/10.1016/0019-1035(74)90087-6 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 21 1974 1 28-34 |
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(DE-627)NLEJ180420941 (DE-599)GBVNLZ180420941 DE-627 ger DE-627 rakwb eng Mars: Clearing of the 1971 dust storm 1974 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, W.K. oth Price, M.J. oth in Icarus Amsterdam : Elsevier 21(1974), 1, Seite 28-34 (DE-627)NLEJ176861017 (DE-600)1467991-7 0019-1035 nnns volume:21 year:1974 number:1 pages:28-34 http://dx.doi.org/10.1016/0019-1035(74)90087-6 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 21 1974 1 28-34 |
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(DE-627)NLEJ180420941 (DE-599)GBVNLZ180420941 DE-627 ger DE-627 rakwb eng Mars: Clearing of the 1971 dust storm 1974 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, W.K. oth Price, M.J. oth in Icarus Amsterdam : Elsevier 21(1974), 1, Seite 28-34 (DE-627)NLEJ176861017 (DE-600)1467991-7 0019-1035 nnns volume:21 year:1974 number:1 pages:28-34 http://dx.doi.org/10.1016/0019-1035(74)90087-6 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 21 1974 1 28-34 |
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(DE-627)NLEJ180420941 (DE-599)GBVNLZ180420941 DE-627 ger DE-627 rakwb eng Mars: Clearing of the 1971 dust storm 1974 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, W.K. oth Price, M.J. oth in Icarus Amsterdam : Elsevier 21(1974), 1, Seite 28-34 (DE-627)NLEJ176861017 (DE-600)1467991-7 0019-1035 nnns volume:21 year:1974 number:1 pages:28-34 http://dx.doi.org/10.1016/0019-1035(74)90087-6 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 21 1974 1 28-34 |
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A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. |
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A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. |
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A semiquantitative analysis of clearing in the 1971 great dust storm on Mars is presented as a function of time and altitude, using Mariner 9 orange- and visual-light photos. Steady settling of dust approximately accounts for the decline of the storm after December 22, 1971. Continuous settling cannot be invoked prior to that date; injection of dust into the atmosphere, i.e., a storm resurgence, occurred in mid-December 1971. Theoretical models of optical depth versus time are developed for various distributions of particles in the atmosphere. By intespreting settling in terms of Stokes' law, estimates of the maximum radii of dust particles throughout the atmosphere have been obtained. Models which best account for the dust-storm decline indicate particles 5μm in diameter high in the atmosphere, with a concentration of larger particles ( 10μm) near the ground in the lowest parts of Mars. Long-term thin high hazes should persist through much of the Martian year, perhaps clearing before perihelion. |
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