Microwave observations of stratospheric ozone variations during a solar eclipse

During solar eclipses the ozone layer of the Earth is exposed to variable action of an ozone active radiation of the Sun (wavelengths 200-400 nm). The variations of magnitude and spectral structure of a solar ultraviolet radiation flow can cause both variability of total ozone content (TOC), and its...

Ausführliche Beschreibung

Gespeichert in:
Bibliographische Detailangaben
Hauptverfasser: Fedoseev, L.I., Krasilnikov, A.A., Kulikov, Yu.Yu, Ryskin, V.G.
Format: Tagungsbericht
Sprache:eng
Schlagworte:
Online-Zugang:Volltext bestellen
Tags: Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
container_end_page 890 Vol.2
container_issue
container_start_page 889
container_title
container_volume 2
creator Fedoseev, L.I.
Krasilnikov, A.A.
Kulikov, Yu.Yu
Ryskin, V.G.
description During solar eclipses the ozone layer of the Earth is exposed to variable action of an ozone active radiation of the Sun (wavelengths 200-400 nm). The variations of magnitude and spectral structure of a solar ultraviolet radiation flow can cause both variability of total ozone content (TOC), and its vertical distribution. It is obvious, that the ozone variability should happen in the upper part of a layer (above than 40 km), where time of O/sub 3/ relaxation it is a little (photochemical time of life - about one minute). The ozone layer at altitudes of 40-80 km reacts most rapidly to variations of the Sun radiation, which are stimulated by rotation of the Earth (sunrise and sunset) and by solar eclipses. During eclipses the observations of TOC variations are carry out usually. The data of such observations represent rather inconsistent information about behavior of TOC to a phase of solar eclipses. It, most likely, is connected to that the full amount of ozone on heights exceeding 40 km, makes up only small part TOC. As to modifications of vertical distribution ozone density during eclipses, the information about them is not enough. The realization of similar observations has become possible due to emerging and development, perhaps, most approaching tool for research of the response of the upper atmosphere ozone on a rather rapid modification of the solar radiation - microwave radiometry with a high temporal and spectral resolution. We briefly present a method of research of ozone variations during a partial solar eclipse of May 31, 2003 (maximum phase about 70%), and discuss the used equipment and obtained outcomes.
doi_str_mv 10.1109/MSMW.2004.1346227
format Conference Proceeding
fullrecord <record><control><sourceid>ieee_6IE</sourceid><recordid>TN_cdi_ieee_primary_1346227</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><ieee_id>1346227</ieee_id><sourcerecordid>1346227</sourcerecordid><originalsourceid>FETCH-LOGICAL-i175t-e4d8b23168e20c3d8883c59e91c0beb6e30ae84e6a9dd19e25864a2f8bdec8993</originalsourceid><addsrcrecordid>eNotj81KxDAURgMiqOM8gLjJC0zNX9ubpQz-wZRZqLgcbpNbjdSmJLWiT69gv83ZHA58jF1IUUgp7FXz2LwUSghTSG0qpeojdiZqEBqMlPqErXN-F38zpRGgTtm-CS7FL5yJxzZTmnEKccg8djxPCaeYxzdKwfH4EwfiM6awGP4zheGVI8-xx8TJ9WHMdM6OO-wzrReu2PPtzdP2frPb3z1sr3ebIOty2pDx0CotKyAlnPYAoF1pyUonWmor0gIJDFVovZeWVAmVQdVB68mBtXrFLv-7gYgOYwofmL4Py2f9C_R_TsM</addsrcrecordid><sourcetype>Publisher</sourcetype><iscdi>true</iscdi><recordtype>conference_proceeding</recordtype></control><display><type>conference_proceeding</type><title>Microwave observations of stratospheric ozone variations during a solar eclipse</title><source>IEEE Electronic Library (IEL) Conference Proceedings</source><creator>Fedoseev, L.I. ; Krasilnikov, A.A. ; Kulikov, Yu.Yu ; Ryskin, V.G.</creator><creatorcontrib>Fedoseev, L.I. ; Krasilnikov, A.A. ; Kulikov, Yu.Yu ; Ryskin, V.G.</creatorcontrib><description>During solar eclipses the ozone layer of the Earth is exposed to variable action of an ozone active radiation of the Sun (wavelengths 200-400 nm). The variations of magnitude and spectral structure of a solar ultraviolet radiation flow can cause both variability of total ozone content (TOC), and its vertical distribution. It is obvious, that the ozone variability should happen in the upper part of a layer (above than 40 km), where time of O/sub 3/ relaxation it is a little (photochemical time of life - about one minute). The ozone layer at altitudes of 40-80 km reacts most rapidly to variations of the Sun radiation, which are stimulated by rotation of the Earth (sunrise and sunset) and by solar eclipses. During eclipses the observations of TOC variations are carry out usually. The data of such observations represent rather inconsistent information about behavior of TOC to a phase of solar eclipses. It, most likely, is connected to that the full amount of ozone on heights exceeding 40 km, makes up only small part TOC. As to modifications of vertical distribution ozone density during eclipses, the information about them is not enough. The realization of similar observations has become possible due to emerging and development, perhaps, most approaching tool for research of the response of the upper atmosphere ozone on a rather rapid modification of the solar radiation - microwave radiometry with a high temporal and spectral resolution. We briefly present a method of research of ozone variations during a partial solar eclipse of May 31, 2003 (maximum phase about 70%), and discuss the used equipment and obtained outcomes.</description><identifier>ISBN: 0780384113</identifier><identifier>ISBN: 9780780384118</identifier><identifier>DOI: 10.1109/MSMW.2004.1346227</identifier><language>eng</language><publisher>IEEE</publisher><subject>Atmospheric measurements ; Bandwidth ; Earth ; Frequency ; Geoscience ; Mirrors ; Photochemistry ; Physics ; Sun ; Temperature sensors</subject><ispartof>The Fifth International Kharkov Symposium on Physics and Engineering of Microwaves, Millimeter, and Submillimeter Waves (IEEE Cat. No.04EX828), 2004, Vol.2, p.889-890 Vol.2</ispartof><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktohtml>$$Uhttps://ieeexplore.ieee.org/document/1346227$$EHTML$$P50$$Gieee$$H</linktohtml><link.rule.ids>309,310,777,781,786,787,2052,4036,4037,27906,54901</link.rule.ids><linktorsrc>$$Uhttps://ieeexplore.ieee.org/document/1346227$$EView_record_in_IEEE$$FView_record_in_$$GIEEE</linktorsrc></links><search><creatorcontrib>Fedoseev, L.I.</creatorcontrib><creatorcontrib>Krasilnikov, A.A.</creatorcontrib><creatorcontrib>Kulikov, Yu.Yu</creatorcontrib><creatorcontrib>Ryskin, V.G.</creatorcontrib><title>Microwave observations of stratospheric ozone variations during a solar eclipse</title><title>The Fifth International Kharkov Symposium on Physics and Engineering of Microwaves, Millimeter, and Submillimeter Waves (IEEE Cat. No.04EX828)</title><addtitle>MSMW</addtitle><description>During solar eclipses the ozone layer of the Earth is exposed to variable action of an ozone active radiation of the Sun (wavelengths 200-400 nm). The variations of magnitude and spectral structure of a solar ultraviolet radiation flow can cause both variability of total ozone content (TOC), and its vertical distribution. It is obvious, that the ozone variability should happen in the upper part of a layer (above than 40 km), where time of O/sub 3/ relaxation it is a little (photochemical time of life - about one minute). The ozone layer at altitudes of 40-80 km reacts most rapidly to variations of the Sun radiation, which are stimulated by rotation of the Earth (sunrise and sunset) and by solar eclipses. During eclipses the observations of TOC variations are carry out usually. The data of such observations represent rather inconsistent information about behavior of TOC to a phase of solar eclipses. It, most likely, is connected to that the full amount of ozone on heights exceeding 40 km, makes up only small part TOC. As to modifications of vertical distribution ozone density during eclipses, the information about them is not enough. The realization of similar observations has become possible due to emerging and development, perhaps, most approaching tool for research of the response of the upper atmosphere ozone on a rather rapid modification of the solar radiation - microwave radiometry with a high temporal and spectral resolution. We briefly present a method of research of ozone variations during a partial solar eclipse of May 31, 2003 (maximum phase about 70%), and discuss the used equipment and obtained outcomes.</description><subject>Atmospheric measurements</subject><subject>Bandwidth</subject><subject>Earth</subject><subject>Frequency</subject><subject>Geoscience</subject><subject>Mirrors</subject><subject>Photochemistry</subject><subject>Physics</subject><subject>Sun</subject><subject>Temperature sensors</subject><isbn>0780384113</isbn><isbn>9780780384118</isbn><fulltext>true</fulltext><rsrctype>conference_proceeding</rsrctype><creationdate>2004</creationdate><recordtype>conference_proceeding</recordtype><sourceid>6IE</sourceid><sourceid>RIE</sourceid><recordid>eNotj81KxDAURgMiqOM8gLjJC0zNX9ubpQz-wZRZqLgcbpNbjdSmJLWiT69gv83ZHA58jF1IUUgp7FXz2LwUSghTSG0qpeojdiZqEBqMlPqErXN-F38zpRGgTtm-CS7FL5yJxzZTmnEKccg8djxPCaeYxzdKwfH4EwfiM6awGP4zheGVI8-xx8TJ9WHMdM6OO-wzrReu2PPtzdP2frPb3z1sr3ebIOty2pDx0CotKyAlnPYAoF1pyUonWmor0gIJDFVovZeWVAmVQdVB68mBtXrFLv-7gYgOYwofmL4Py2f9C_R_TsM</recordid><startdate>2004</startdate><enddate>2004</enddate><creator>Fedoseev, L.I.</creator><creator>Krasilnikov, A.A.</creator><creator>Kulikov, Yu.Yu</creator><creator>Ryskin, V.G.</creator><general>IEEE</general><scope>6IE</scope><scope>6IL</scope><scope>CBEJK</scope><scope>RIE</scope><scope>RIL</scope></search><sort><creationdate>2004</creationdate><title>Microwave observations of stratospheric ozone variations during a solar eclipse</title><author>Fedoseev, L.I. ; Krasilnikov, A.A. ; Kulikov, Yu.Yu ; Ryskin, V.G.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-i175t-e4d8b23168e20c3d8883c59e91c0beb6e30ae84e6a9dd19e25864a2f8bdec8993</frbrgroupid><rsrctype>conference_proceedings</rsrctype><prefilter>conference_proceedings</prefilter><language>eng</language><creationdate>2004</creationdate><topic>Atmospheric measurements</topic><topic>Bandwidth</topic><topic>Earth</topic><topic>Frequency</topic><topic>Geoscience</topic><topic>Mirrors</topic><topic>Photochemistry</topic><topic>Physics</topic><topic>Sun</topic><topic>Temperature sensors</topic><toplevel>online_resources</toplevel><creatorcontrib>Fedoseev, L.I.</creatorcontrib><creatorcontrib>Krasilnikov, A.A.</creatorcontrib><creatorcontrib>Kulikov, Yu.Yu</creatorcontrib><creatorcontrib>Ryskin, V.G.</creatorcontrib><collection>IEEE Electronic Library (IEL) Conference Proceedings</collection><collection>IEEE Proceedings Order Plan All Online (POP All Online) 1998-present by volume</collection><collection>IEEE Xplore All Conference Proceedings</collection><collection>IEEE Electronic Library (IEL)</collection><collection>IEEE Proceedings Order Plans (POP All) 1998-Present</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Fedoseev, L.I.</au><au>Krasilnikov, A.A.</au><au>Kulikov, Yu.Yu</au><au>Ryskin, V.G.</au><format>book</format><genre>proceeding</genre><ristype>CONF</ristype><atitle>Microwave observations of stratospheric ozone variations during a solar eclipse</atitle><btitle>The Fifth International Kharkov Symposium on Physics and Engineering of Microwaves, Millimeter, and Submillimeter Waves (IEEE Cat. No.04EX828)</btitle><stitle>MSMW</stitle><date>2004</date><risdate>2004</risdate><volume>2</volume><spage>889</spage><epage>890 Vol.2</epage><pages>889-890 Vol.2</pages><isbn>0780384113</isbn><isbn>9780780384118</isbn><abstract>During solar eclipses the ozone layer of the Earth is exposed to variable action of an ozone active radiation of the Sun (wavelengths 200-400 nm). The variations of magnitude and spectral structure of a solar ultraviolet radiation flow can cause both variability of total ozone content (TOC), and its vertical distribution. It is obvious, that the ozone variability should happen in the upper part of a layer (above than 40 km), where time of O/sub 3/ relaxation it is a little (photochemical time of life - about one minute). The ozone layer at altitudes of 40-80 km reacts most rapidly to variations of the Sun radiation, which are stimulated by rotation of the Earth (sunrise and sunset) and by solar eclipses. During eclipses the observations of TOC variations are carry out usually. The data of such observations represent rather inconsistent information about behavior of TOC to a phase of solar eclipses. It, most likely, is connected to that the full amount of ozone on heights exceeding 40 km, makes up only small part TOC. As to modifications of vertical distribution ozone density during eclipses, the information about them is not enough. The realization of similar observations has become possible due to emerging and development, perhaps, most approaching tool for research of the response of the upper atmosphere ozone on a rather rapid modification of the solar radiation - microwave radiometry with a high temporal and spectral resolution. We briefly present a method of research of ozone variations during a partial solar eclipse of May 31, 2003 (maximum phase about 70%), and discuss the used equipment and obtained outcomes.</abstract><pub>IEEE</pub><doi>10.1109/MSMW.2004.1346227</doi></addata></record>
fulltext fulltext_linktorsrc
identifier ISBN: 0780384113
ispartof The Fifth International Kharkov Symposium on Physics and Engineering of Microwaves, Millimeter, and Submillimeter Waves (IEEE Cat. No.04EX828), 2004, Vol.2, p.889-890 Vol.2
issn
language eng
recordid cdi_ieee_primary_1346227
source IEEE Electronic Library (IEL) Conference Proceedings
subjects Atmospheric measurements
Bandwidth
Earth
Frequency
Geoscience
Mirrors
Photochemistry
Physics
Sun
Temperature sensors
title Microwave observations of stratospheric ozone variations during a solar eclipse
url https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-17T22%3A23%3A23IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-ieee_6IE&rft_val_fmt=info:ofi/fmt:kev:mtx:book&rft.genre=proceeding&rft.atitle=Microwave%20observations%20of%20stratospheric%20ozone%20variations%20during%20a%20solar%20eclipse&rft.btitle=The%20Fifth%20International%20Kharkov%20Symposium%20on%20Physics%20and%20Engineering%20of%20Microwaves,%20Millimeter,%20and%20Submillimeter%20Waves%20(IEEE%20Cat.%20No.04EX828)&rft.au=Fedoseev,%20L.I.&rft.date=2004&rft.volume=2&rft.spage=889&rft.epage=890%20Vol.2&rft.pages=889-890%20Vol.2&rft.isbn=0780384113&rft.isbn_list=9780780384118&rft_id=info:doi/10.1109/MSMW.2004.1346227&rft_dat=%3Cieee_6IE%3E1346227%3C/ieee_6IE%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rft_ieee_id=1346227&rfr_iscdi=true