Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements
The high atmosphere of Mars ( z > 30 km) has been observed from Phobos 2, using the solar occultation technique. Due to a major error in the pointing system, resulting from a wrong orientation of the spacecraft in the pointing software, the lower atmosphere is never observed in ultraviolet (220–3...
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| Veröffentlicht in: | Planetary and space science 1991, Vol.39 (1), p.175-187 |
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| creator | Blamont, J.E. Chassefiere, E. Goutail, J.P. Mege, B. Nunes-Pinharanda, M. Souchon, G. Krasnopolsky, V.A. Krysko, A.A. Moroz, V.I. |
| description | The high atmosphere of Mars (
z > 30 km) has been observed from
Phobos 2, using the solar occultation technique. Due to a major error in the pointing system, resulting from a wrong orientation of the spacecraft in the pointing software, the lower atmosphere is never observed in ultraviolet (220–330 nm) and high resolution near-infrared (760 nm, 936 nm) channels. Pointing data sometimes provide useful information on the visible opacity below 30 km. showing that the scale height of dust decreases from ≅ 8 km below 20 km to ≅ 4 km above. Among 32 occultations, four show the presence of a water ice cloud high in the atmosphere (
z = 50 km), with a maximum tangential optical thickness varying from ≅ 0.05 to ≅ 2 and a vertical extent in the range from 5 to 15 km. Indications on the particles size (
r ≫ 0.01
μm) are obtained using spectral information. From a simple cloud model, where eddy diffusion and sedimentation processes are taken into account, an upper limit of 10
7 cm
2 s
−1 is derived for the eddy diffusion coefficient. Similarly, the absence of ozone in detectable amounts above 30 km is interpreted as the signature of a rather weak value of
K. Using a simple stationary photochemical model, a value of
K as low as 10
6 cm
2 s
−1 seems to be required. |
| doi_str_mv | 10.1016/0032-0633(91)90140-6 |
| format | Article |
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z > 30 km) has been observed from
Phobos 2, using the solar occultation technique. Due to a major error in the pointing system, resulting from a wrong orientation of the spacecraft in the pointing software, the lower atmosphere is never observed in ultraviolet (220–330 nm) and high resolution near-infrared (760 nm, 936 nm) channels. Pointing data sometimes provide useful information on the visible opacity below 30 km. showing that the scale height of dust decreases from ≅ 8 km below 20 km to ≅ 4 km above. Among 32 occultations, four show the presence of a water ice cloud high in the atmosphere (
z = 50 km), with a maximum tangential optical thickness varying from ≅ 0.05 to ≅ 2 and a vertical extent in the range from 5 to 15 km. Indications on the particles size (
r ≫ 0.01
μm) are obtained using spectral information. From a simple cloud model, where eddy diffusion and sedimentation processes are taken into account, an upper limit of 10
7 cm
2 s
−1 is derived for the eddy diffusion coefficient. Similarly, the absence of ozone in detectable amounts above 30 km is interpreted as the signature of a rather weak value of
K. Using a simple stationary photochemical model, a value of
K as low as 10
6 cm
2 s
−1 seems to be required.</description><identifier>ISSN: 0032-0633</identifier><identifier>EISSN: 1873-5088</identifier><identifier>DOI: 10.1016/0032-0633(91)90140-6</identifier><identifier>CODEN: PLSSAE</identifier><language>eng</language><publisher>Oxford: Elsevier Ltd</publisher><subject>Astronomy ; Earth, ocean, space ; Exact sciences and technology ; Mars ; Planets, their satellites and rings. Asteroids ; Solar system</subject><ispartof>Planetary and space science, 1991, Vol.39 (1), p.175-187</ispartof><rights>1991</rights><rights>1991 INIST-CNRS</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c396t-14772ff7d26b117ecfa976efcb14b4d1d96e910ed4b9bd07db495e26dfef92503</citedby><cites>FETCH-LOGICAL-c396t-14772ff7d26b117ecfa976efcb14b4d1d96e910ed4b9bd07db495e26dfef92503</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktohtml>$$Uhttps://www.sciencedirect.com/science/article/pii/0032063391901406$$EHTML$$P50$$Gelsevier$$H</linktohtml><link.rule.ids>309,310,314,776,780,785,786,3537,4010,4036,4037,23909,23910,25118,27900,27901,27902,65306</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=19637713$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Blamont, J.E.</creatorcontrib><creatorcontrib>Chassefiere, E.</creatorcontrib><creatorcontrib>Goutail, J.P.</creatorcontrib><creatorcontrib>Mege, B.</creatorcontrib><creatorcontrib>Nunes-Pinharanda, M.</creatorcontrib><creatorcontrib>Souchon, G.</creatorcontrib><creatorcontrib>Krasnopolsky, V.A.</creatorcontrib><creatorcontrib>Krysko, A.A.</creatorcontrib><creatorcontrib>Moroz, V.I.</creatorcontrib><title>Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements</title><title>Planetary and space science</title><description>The high atmosphere of Mars (
z > 30 km) has been observed from
Phobos 2, using the solar occultation technique. Due to a major error in the pointing system, resulting from a wrong orientation of the spacecraft in the pointing software, the lower atmosphere is never observed in ultraviolet (220–330 nm) and high resolution near-infrared (760 nm, 936 nm) channels. Pointing data sometimes provide useful information on the visible opacity below 30 km. showing that the scale height of dust decreases from ≅ 8 km below 20 km to ≅ 4 km above. Among 32 occultations, four show the presence of a water ice cloud high in the atmosphere (
z = 50 km), with a maximum tangential optical thickness varying from ≅ 0.05 to ≅ 2 and a vertical extent in the range from 5 to 15 km. Indications on the particles size (
r ≫ 0.01
μm) are obtained using spectral information. From a simple cloud model, where eddy diffusion and sedimentation processes are taken into account, an upper limit of 10
7 cm
2 s
−1 is derived for the eddy diffusion coefficient. Similarly, the absence of ozone in detectable amounts above 30 km is interpreted as the signature of a rather weak value of
K. Using a simple stationary photochemical model, a value of
K as low as 10
6 cm
2 s
−1 seems to be required.</description><subject>Astronomy</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Mars</subject><subject>Planets, their satellites and rings. Asteroids</subject><subject>Solar system</subject><issn>0032-0633</issn><issn>1873-5088</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1991</creationdate><recordtype>article</recordtype><recordid>eNqFkU2PFCEQholxE8dd_4EHLho9tFtANwwXE7PxK1njRb0SGoosphtGoDdZf72Ms9Gbnury1Fup5yXkKYNXDJi8BBB8ACnEC81eamAjDPIB2bG9EsME-_1DsvuDPCKPa_0OAFJytSPxG5YWnV3ooeQQF6w0B-q32qhNnuafOSGNibYbpJ9sR22itq25Hm6wIPXoN4eehpJXWvNiC83ObUuzLeZEV7R1K7hiavWCnAW7VHxyP8_J13dvv1x9GK4_v_949eZ6cELLNrBRKR6C8lzOjCl0wWolMbiZjfPomdcSNQP046xnD8rPo56QSx8waD6BOCfPT7n9oR8b1mbWWB0ui02Yt2r4NAkAPf0XZHveo4F3cDyBruRaCwZzKHG15c4wMMcCzNGuOdo1mpnfBRjZ157d59vaBYdik4v1766WQikmOvf6xGG3chuxmOoipq41FnTN-Bz_fegXNPibgg</recordid><startdate>1991</startdate><enddate>1991</enddate><creator>Blamont, J.E.</creator><creator>Chassefiere, E.</creator><creator>Goutail, J.P.</creator><creator>Mege, B.</creator><creator>Nunes-Pinharanda, M.</creator><creator>Souchon, G.</creator><creator>Krasnopolsky, V.A.</creator><creator>Krysko, A.A.</creator><creator>Moroz, V.I.</creator><general>Elsevier Ltd</general><general>Pergamon Press</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>1991</creationdate><title>Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements</title><author>Blamont, J.E. ; Chassefiere, E. ; Goutail, J.P. ; Mege, B. ; Nunes-Pinharanda, M. ; Souchon, G. ; Krasnopolsky, V.A. ; Krysko, A.A. ; Moroz, V.I.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c396t-14772ff7d26b117ecfa976efcb14b4d1d96e910ed4b9bd07db495e26dfef92503</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1991</creationdate><topic>Astronomy</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Mars</topic><topic>Planets, their satellites and rings. Asteroids</topic><topic>Solar system</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Blamont, J.E.</creatorcontrib><creatorcontrib>Chassefiere, E.</creatorcontrib><creatorcontrib>Goutail, J.P.</creatorcontrib><creatorcontrib>Mege, B.</creatorcontrib><creatorcontrib>Nunes-Pinharanda, M.</creatorcontrib><creatorcontrib>Souchon, G.</creatorcontrib><creatorcontrib>Krasnopolsky, V.A.</creatorcontrib><creatorcontrib>Krysko, A.A.</creatorcontrib><creatorcontrib>Moroz, V.I.</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Planetary and space science</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Blamont, J.E.</au><au>Chassefiere, E.</au><au>Goutail, J.P.</au><au>Mege, B.</au><au>Nunes-Pinharanda, M.</au><au>Souchon, G.</au><au>Krasnopolsky, V.A.</au><au>Krysko, A.A.</au><au>Moroz, V.I.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements</atitle><jtitle>Planetary and space science</jtitle><date>1991</date><risdate>1991</risdate><volume>39</volume><issue>1</issue><spage>175</spage><epage>187</epage><pages>175-187</pages><issn>0032-0633</issn><eissn>1873-5088</eissn><coden>PLSSAE</coden><abstract>The high atmosphere of Mars (
z > 30 km) has been observed from
Phobos 2, using the solar occultation technique. Due to a major error in the pointing system, resulting from a wrong orientation of the spacecraft in the pointing software, the lower atmosphere is never observed in ultraviolet (220–330 nm) and high resolution near-infrared (760 nm, 936 nm) channels. Pointing data sometimes provide useful information on the visible opacity below 30 km. showing that the scale height of dust decreases from ≅ 8 km below 20 km to ≅ 4 km above. Among 32 occultations, four show the presence of a water ice cloud high in the atmosphere (
z = 50 km), with a maximum tangential optical thickness varying from ≅ 0.05 to ≅ 2 and a vertical extent in the range from 5 to 15 km. Indications on the particles size (
r ≫ 0.01
μm) are obtained using spectral information. From a simple cloud model, where eddy diffusion and sedimentation processes are taken into account, an upper limit of 10
7 cm
2 s
−1 is derived for the eddy diffusion coefficient. Similarly, the absence of ozone in detectable amounts above 30 km is interpreted as the signature of a rather weak value of
K. Using a simple stationary photochemical model, a value of
K as low as 10
6 cm
2 s
−1 seems to be required.</abstract><cop>Oxford</cop><cop>New York, NY</cop><pub>Elsevier Ltd</pub><doi>10.1016/0032-0633(91)90140-6</doi><tpages>13</tpages></addata></record> |
| fulltext | fulltext |
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| ispartof | Planetary and space science, 1991, Vol.39 (1), p.175-187 |
| issn | 0032-0633 1873-5088 |
| language | eng |
| recordid | cdi_proquest_miscellaneous_25530095 |
| source | Elsevier ScienceDirect Journals |
| subjects | Astronomy Earth, ocean, space Exact sciences and technology Mars Planets, their satellites and rings. Asteroids Solar system |
| title | Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements |
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