Solar activity influence on vertical ozone redistribution over Antarctica
Study of dynamics of vertical ozone distribution above Antarctic and, for comparison, equatorial zones during complete 11-year's cycle of solar activity was made. Satellite profile ozone data from Nimbus 7 were used. Strong vertical redistribution of an ozone amounts during ozone hole is shown....
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| Цитувати: | Solar activity influence on vertical ozone redistribution over Antarctica / V.V. Lozitsky // Український антарктичний журнал. — 2004. — № 2. — С. 99-104. — Бібліогр.: 6 назв. — англ. |
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nasplib_isofts_kiev_ua-123456789-1281532025-02-09T22:37:19Z Solar activity influence on vertical ozone redistribution over Antarctica Влияние солнечной активности на вертикальное перераспределение озона над Антарктидой Вплив сонячної активності на вертикальний перерозподіл озону над Антарктидою Lozitsky, V.V. Фізика атмосфери. Геохімія Study of dynamics of vertical ozone distribution above Antarctic and, for comparison, equatorial zones during complete 11-year's cycle of solar activity was made. Satellite profile ozone data from Nimbus 7 were used. Strong vertical redistribution of an ozone amounts during ozone hole is shown. Correlations analysis between ozone vertical profile data and several solar activity indices was made. An absence of ozone layer response on solar proton events and finding out significant decrease of correlation coefficients at upper stratosphere heights are the main results of the work. Исследуется динамика высотных профилей озона над Антарктическим регионом в сравнении с экваториальной зоной. Использовались спутниковые данные, полученные с космической платформы Nimbus 7. Показано наличие сильное (по сравнению с экватором) вертикальное перераспределение содержания озона в присутствии озоновой дыры. Анализируется влияние солнечной активности на высотное перераспределение озона. Выявлены такие главные особенности, как отсутствие отклика озонового слоя на солнечные протонные вспышки та существенное уменьшение коэффициентов корреляции между содержанием озона и исследовавшимися факторами солнечной активности на высотах верхней стратосферы (по сравнению с другими высотами). Досліджується динаміка висотних профілів озону над Антарктичним регіоном у порівнянні з екваторіальною зоною. Для вивчення були взяті супутникові дані, отримані з космічної платформи Nimbus 7. Показано наявність сильних (порівняно з екватором) вертикальних перерозподілів вмісту озону під час наявності озонової діри. Аналізується вплив чинників сонячної активності на висотний перерозподіл озону. Виявлено такі головні особливості, як відсутність відгуку озонового шару на сонячні протонні спалахи та суттєве зменшення кофіцієнтів кореляцій між вмістом озону та дослідженими факторами сонячної активності на висотах верхньої стратосфери (порівняно з іншими висотами). 2004 Article Solar activity influence on vertical ozone redistribution over Antarctica / V.V. Lozitsky // Український антарктичний журнал. — 2004. — № 2. — С. 99-104. — Бібліогр.: 6 назв. — англ. 1727-7485 https://nasplib.isofts.kiev.ua/handle/123456789/128153 551.510.534 en application/pdf Національний антарктичний науковий центр МОН України |
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Фізика атмосфери. Геохімія Фізика атмосфери. Геохімія |
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Фізика атмосфери. Геохімія Фізика атмосфери. Геохімія Lozitsky, V.V. Solar activity influence on vertical ozone redistribution over Antarctica |
| description |
Study of dynamics of vertical ozone distribution above Antarctic and, for comparison, equatorial zones during complete 11-year's cycle of solar activity was made. Satellite profile ozone data from Nimbus 7 were used. Strong vertical redistribution of an ozone amounts during ozone hole is shown. Correlations analysis between ozone vertical profile data and several solar activity indices was made. An absence of ozone layer response on solar proton events and finding out significant decrease of correlation coefficients at upper stratosphere heights are the main results of the work. |
| format |
Article |
| author |
Lozitsky, V.V. |
| author_facet |
Lozitsky, V.V. |
| author_sort |
Lozitsky, V.V. |
| title |
Solar activity influence on vertical ozone redistribution over Antarctica |
| title_short |
Solar activity influence on vertical ozone redistribution over Antarctica |
| title_full |
Solar activity influence on vertical ozone redistribution over Antarctica |
| title_fullStr |
Solar activity influence on vertical ozone redistribution over Antarctica |
| title_full_unstemmed |
Solar activity influence on vertical ozone redistribution over Antarctica |
| title_sort |
solar activity influence on vertical ozone redistribution over antarctica |
| publisher |
Національний антарктичний науковий центр МОН України |
| publishDate |
2004 |
| topic_facet |
Фізика атмосфери. Геохімія |
| url |
https://nasplib.isofts.kiev.ua/handle/123456789/128153 |
| citation_txt |
Solar activity influence on vertical ozone redistribution over Antarctica / V.V. Lozitsky // Український антарктичний журнал. — 2004. — № 2. — С. 99-104. — Бібліогр.: 6 назв. — англ. |
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2025-12-01T11:27:36Z |
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| fulltext |
УКРАЇНСЬКИЙ АНТАРКТИЧНИЙ
ЖУРНАЛ
УАЖ, №2, 99-104, (2004)
99
УДК 551.510.534
SOLAR ACTIVITY INFLUENCE ON VERTICAL OZONE REDISTRIBUTION OVER
ANTARCTICA
V. V. Lozitsky
Ukrainian Antarctic Center, T. Shevchenka blvd., 16, Kyiv 01601. E-mail: uac@uac.gov.ua
Abstract. Study of dynamics of vertical ozone distribution above Antarctic and, for comparison, equatorial zones during
complete 11-year's cycle of solar activity was made. Satellite profile ozone data from Nimbus 7 were used. Strong vertical
redistribution of an ozone amounts during ozone hole is shown. Correlations analysis between ozone vertical profile data and
several solar activity indices was made. An absence of ozone layer response on solar proton events and finding out significant
decrease of correlation coefficients at upper stratosphere heights are the main results of the work.
Key words. Antarctica, ozone profiles, ozone hole, solar ultraviolet, cosmic rays.
Вплив сонячної активності на вертикальний перерозподіл озону над Антарктидою. В.В. Лозицький
Реферат. Досліджується динаміка висотних профілів озону над Антарктичним регіоном у порівнянні з екваторіальною
зоною. Для вивчення були взяті супутникові дані, отримані з космічної платформи Nimbus 7. Показано наявність
сильних (порівняно з екватором) вертикальних перерозподілів вмісту озону під час наявності озонової діри.
Аналізується вплив чинників сонячної активності на висотний перерозподіл озону. Виявлено такі головні особливості,
як відсутність відгуку озонового шару на сонячні протонні спалахи та суттєве зменшення кофіцієнтів кореляцій між
вмістом озону та дослідженими факторами сонячної активності на висотах верхньої стратосфери (порівняно з іншими
висотами).
Влияние солнечной активности на вертикальное перераспределение озона над Антарктидой. В.В. Лозицкий
Реферат. Исследуется динамика высотных профилей озона над Антарктическим регионом в сравнении с
экваториальной зоной. Использовались спутниковые данные, полученные с космической платформы Nimbus 7.
Показано наличие сильное (по сравнению с экватором) вертикальное перераспределение содержания озона в
присутствии озоновой дыры. Анализируется влияние солнечной активности на высотное перераспределение озона.
Выявлены такие главные особенности, как отсутствие отклика озонового слоя на солнечные протонные вспышки та
существенное уменьшение коэффициентов корреляции между содержанием озона и исследовавшимися факторами
солнечной активности на высотах верхней стратосферы (по сравнению с другими высотами).
1. Introduction
The first empirical evidences of the solar activity influence on the total ozone content (TOC)
were found at the middle of the last century by different researchers independently (Логинов и др.,
1980). Solar ultraviolet variability influence was explored and other mechanisms of influence were
proposed. In (Krivolutsky, 2002) the impact of solar proton events on the ozone content is examined.
Short-term impact of the solar protons in the atmosphere can generate huge amounts of the NOx at
mesospheric heights. The model calculations predict that observed variations in TOC may be
explained by this scheme. In (Reiter, 1979) the flux on the wavelength 10.7 cm was taken for the solar
activity index. Its variations were compared with monthly average change in TOC with eliminated
seasonal and quasibiennial trends and running averaging through the six months for 1970–1975 were
made. The correlation coefficient of +0.94 was obtained. The total ozone content decrease for that
period up to the level of 15 DU due to the decay of solar activity was discussed.
The influence of the cosmic rays on the ozone content at different heights has been estimated
in (Логинов и др., 1980). The 11-years variation of the cosmic ray flux can modulate ionization
intensity at the stratospheric heights. This modulates the 11-year variation of NOx generation rate,
which affects ozone directly. Investigation and prediction of the long-term trends of the global ozone
was made in (Hansen et al, 2002). On the basis of ozone data analysis and model calculations, authors
came to conclusion that starting from 1998, the global decreasing trend of TOC finished and should be
close to zero for the nearest future.
V.V. Lozitsky: SOLAR ACTIVITY INFLUENCE ON VERTICAL OZONE REDISTRIBUTION …
100
In this work author used correlation analysis applied to several solar activity factors and
ozone profile data in order to determine the most probable mechanism of solar activity influence on
the layer ozone amounts.
2. Data description and processing technique
All daily ozone vertical profile data was taken from the SBUV website
(http://code916.gsfc.nasa.gov/Public/Space_based/sbuv/sbuv.html). The program was made for
extracting from this data ozone profiles in the two latitudinal zones 65-70S and 0-5S (for comparison).
These files have an ASCII raw format with average daily ozone amounts in Dobson units for the
twelve atmosphere Umkehr layers and for five-degree latitudinal zones over the Earth. For
approximate transition to a height scale it is possible to consider the first layer to be between 0 and 10
km, the second - between 10 and 15 km, the third - between 15 and 20 km and so on (that is very
rough estimation). The following data was used for the analysis of impact of different cosmic factors
on ozone amounts: daily measurements of the cosmic rays flux, geomagnetic disturbance index Ap,
solar ultraviolet flux, solar proton events data. Correlations coefficients were calculated by statistical
processing software. The statistical criteria were used for verifying of the received results. Almost all
of graphs are based on these processed data, if other is not specified.
3. Features of vertical ozone distribution over Antarctica
Comparative analysis of ozone dynamics above the Antarctica and other latitudinal zones some
interesting features were revealed.
The ozone vertical redistribution during the ozone hole essentially differs year by year. Its solar
cycle dependence has not been observed. Daily differences in ozone amounts in Umkehr pressure
levels below and over 24 km calculated for 1988 year and subtracted from the same differences of the
1989. These differences variations are presented on the Fig. 1. Thus we obtain although not very
precise, but convenient index of vertical ozone distribution. For example, for the majority of days of
1988 year these differences are more than zero. This means that in these days ozone layer was higher
than in the same days of 1989. One can see from Fig. 1 that these differences have noise character
during the first half of the year, but in the period of ‘ozone hole’ the height of the ozone layer
significantly changes from one year to another. For other years (not shown here) strong spring
redistributions of the Antarctic ozone layer are also given.
Fig. 1. Vertical distribution index differences (1989 – 1988) variations for Antarctic and midlatitudinal zones.
V.V. Lozitsky: SOLAR ACTIVITY INFLUENCE ON VERTICAL OZONE REDISTRIBUTION …
101
4. Influence on ozone of solar proton flares
The most powerful source of disturbances of the Earth’s magnetic field and ionosphere are the
solar proton events. Existence of significant influence of such events at least on the mesospheric
ozone was specified by Krivolutsky (2002). In this work ozone profiles dynamics during the most
powerful solar proton events was studied.
Analysis of the daily satellite data has shown that any significant changes at all levels from
the troposphere up to the mesosphere during SPEs was not observed neither on equator, nor in the 65 -
70 S zone. After the very powerful flare on October 20, 1989 no significant response after SPE was
observed in the Antarctic zone (Fig. 2). In an equatorial zone (0 - 5 S) any response was not observed
as well.
Fig. 2. Stratospheric ozone amounts in Antarctic zone (1987 and 1989 years).
5. Connection between solar ultraviolet and ozone variations
Solar ultraviolet directly influences on the formation and destruction of ozone. Results of the
correlation analysis for daily UV satellite data (Mg II NASA data were used
(ftp://ftp.ngdc.noaa.gov/FTP/)) and ozone amounts in 12 pressure levels for the 1979-1989 period are
presented (Table 1).
Table 1. Correlation coefficients between daily ozone amounts at different heights and solar UV
Height, km 0-10 10-15 15-20 20-24 24-28 28-33 33-38 38-43 43-48 48-53 53-59 > 59
Antarctica .25 .33 .22 .16 .21 .09 .13 .28 .16 .15 .24 .34
Equator .13 .12 .12 .12 .11 -.12 -.02 .27 .46 .53 .46 .38
The noticeable correlation was obtained only for the large heights over the equator. The fewest
correlation coefficients both on the equator and Antarctica occurred at 30 – 40 km heights. Ultraviolet
detrended data rows were not used because trend was small. There occurred small long-term reduction
of the stratospheric ozone over Antarctica during this period. Due to the strong seasonal variations of
the layer ozone amounts, it is reasonable to analyze yearly averaged satellite data. Then considerably
higher correlation coefficients are received (Tаble 2). Fig. 3, 4 show this yearly averaged ozone
variations at 9-th Umkehr layer (approx. 45 km height) and UV for 0 – 5S and 65 – 70S zones. The
V.V. Lozitsky: SOLAR ACTIVITY INFLUENCE ON VERTICAL OZONE REDISTRIBUTION …
102
“core-to-wing ratio” is the relative UV flux intensity characteristic that is the ratio of chromospheric
MgII line emission depth to the continuum level.
Table 2. Correlation coefficients between yearly averaged ozone amounts at different heights
and solar UV
Height, km 0-10 10-15 15-20 20-24 24-28 28-33 33-38 38-43 43-48 48-53 53-59 > 59
Antarctica .68 .74 .65 .57 .69 .54 .56 .70 .77 .76 .76 .75
Equator .39 .30 .31 .29 .43 -.05 .01 .67 .84 .78 .77 .77
Fig. 3. Yearly averaged mesospheric ozone amounts at 0 – 5S zone and UV.
Fig. 4. Yearly averaged mesospheric ozone amounts at 65 – 70S zone and UV.
V.V. Lozitsky: SOLAR ACTIVITY INFLUENCE ON VERTICAL OZONE REDISTRIBUTION …
103
There is significant correlation between layer ozone amounts and solar UV at high altitudes
in these latitudinal zones. At the heights of 30 - 40 km above the equatorial zone correlation
coefficients are much smaller possibly due to the intensive vertical dynamics processes and
appropriate high-noise behavior of ozone amounts variability at these heights. Concurrently at these
heights above the Antarctic region correlations remain relatively high, while for the middle latitudes
“intermediate” result is received (Fig 5). It is necessary to note small trend of polar ozone decreasing
at all heights in those years.
Fig. 5. Correlation coefficient vs. height.
6. Ozone variations and other solar indices
To exclude strong seasonal ozone layer amounts variations yearly averaging was used. The
vertical ozone distribution above two latitudinal zones (0 – 5S and 65 – 70S) were compared with: the
total ozone content averaged over the Earth, sunspot numbers, Mount-Wilson solar activity magnetic
index, 10.7 cм solar flux, cosmic rays intensity, interplanetary magnetic field strength, geomagnetic
disturbance index Ар. Almost all that information is taken from anonymous ftp NASA server
(ftp://ftp.ngdc.noaa.gov/FTP/). The measurements of TOC were taken from the "TOMS" (Total
Ozone Mapping Spectrometer) website. From correlation analysis it was obtained following:
• Correlations coefficients at high altitudes (above 40 km) are large in both zones and
significant for all parameters, except Ap and sunspot numbers calculated for 65 – 70S zone.
Correlations for all parameters, except CR are positive (0.6 – 0.9), for cosmic rays they are negative
(0.6 – 0.8);
• At heights about 40 km in the equatorial zone correlations coefficients of the layer ozone
amounts with all listed factors rapidly decrease and falls down to zero (or even to a negative value) at
heights about 30 km. Although correlation coefficients at heights below 30 km are larger, they still
remain insignificant (< |0.4|) at all heights till ground. At 65 – 70S zone almost all correlations at
heights below 40 km remain high and significant, though have some small decreasing also.
• Almost all of correlations obtained are less than correlations with UV for the same layers and
latitudes. Probably it means that other (non-UV) solar activity parameters variations do not influence
layer ozone amounts.
V.V. Lozitsky: SOLAR ACTIVITY INFLUENCE ON VERTICAL OZONE REDISTRIBUTION …
104
7. Conclusions
The dynamics of the vertical ozone distribution over 65-70S and 0-5S latitudinal zones during
11-year solar activity cycle was examined. The significant relation between ozone hole height and
solar activity phase was not found. In the days when ozone hole is absent ozone height distribution is
steady for every year. In equatorial zone ozone profiles are constant during the whole year.
Correlations between ozone data and solar activity factors were examined. Yearly averaged
ozone profile data was used to exclude strong seasonal oscillation of the layer ozone amounts.
Correlations of daily rows compared with solar satellite UV data were made apart. Almost for every
of compared rows it was received positive (except cosmic rays) correlations. It was discovered that in
the equatorial zone at the height of 30 – 40 km all correlation coefficients are either insignificant or
even change their sign.
The dependence of response of the ozone amounts at different heights to solar ultraviolet is
constructed. The greatest correlations coefficients have appeared at the large heights. The results
received from the analysis of influence on ozone of solar proton events and correlations analysis with
10.7 см solar flux are in the contradiction with the results of some authors.
In the first case effects of solar proton flares influence on ozone layer both in auroral and in an
equatorial zones were not revealed, including the large altitudes, that is not coordinated to conclusions
of work (Krivolutsky, 2002).
From the correlation analysis of ozone layer and 10.7 cm radiation variations is received values
not exceeding similar factors for ultra-violet radiation (0.5 - 0.8), though in work (Reiter, 1979) the
value of 0.94 for monthly data is underlined. It, probably, can be explained by too short row data, used
in work (Reiter, 1979).
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