scholarly journals Impact of January 2005 solar proton events on chlorine species

2012 ◽  
Vol 12 (9) ◽  
pp. 4159-4179 ◽  
Author(s):  
A. Damiani ◽  
B. Funke ◽  
D. R. Marsh ◽  
M. López-Puertas ◽  
M. L. Santee ◽  
...  
Keyword(s):  
Geographic Distribution ◽  
Climate Model ◽  
Temporal Evolution ◽  
Michelson Interferometer ◽  
Solar Proton ◽  
Active Chlorine ◽  
High Latitudes ◽  
Polar Night ◽  
Solar Proton Events ◽  
Terminator Region

Abstract. Sudden changes in stratospheric chlorine species in the polar northern atmosphere, caused by the Solar Proton Events (SPEs) of 17 and 20 January 2005, have been investigated and compared with version 4 of the Whole Atmosphere Community Climate Model (WACCM4). We used Aura Microwave Limb Sounder (MLS) measurements to monitor the variability of ClO, HCl, HOCl and Michelson Interferometer for Passive Atmospheric Sounder (MIPAS) on ENVISAT to retrieve ClONO2. SPE-induced chlorine activation has been identified. HCl decrease occurred at nearly all the investigated altitudes (i.e., 10–0.5 hPa) with the strongest decrease (of about 0.25 ppbv) on 21 January. HOCl was found to be the main active chlorine species under nighttime conditions (with increases of more than 0.2 ppbv) whereas both HOCl and ClO enhancements (about 0.1 ppbv) have been observed at the polar night terminator. Further, small ClO decreases (of less than 0.1 ppbv) and ClONO2 enhancements (about 0.2 ppbv) have been observed at higher latitudes (i.e., at nighttime) roughly above 2 hPa. While WACCM4 reproduces most of the SPE-induced variability in the chlorine species fairly well, in some particular regions discrepancies between the modeled and measured temporal evolution of the abundances of chlorine species were found. HOCl changes are modelled very well with respect to both magnitude and geographic distribution. ClO decreases are reproduced at high latitudes, whereas ClO enhancements in the terminator region are underestimated and attributed to background variations. WACCM4 also reproduces the HCl depletion in the mesosphere but it does not show the observed decrease below about 2 hPa. Finally, WACCM4 simulations indicate that the observed ClONO2 increase is dominated by background variability, although SPE-induced production might contribute by 0.1 ppbv.

scholarly journals Impact of January 2005 solar proton events on chlorine species

2012 ◽  
Vol 12 (1) ◽  
pp. 1935-1978 ◽  
Author(s):  
A. Damiani ◽  
B. Funke ◽  
D. R. Marsh ◽  
M. López-Puertas ◽  
M. L. Santee ◽  
...  
Keyword(s):  
Geographic Distribution ◽  
Climate Model ◽  
Temporal Evolution ◽  
Michelson Interferometer ◽  
Solar Proton ◽  
Active Chlorine ◽  
High Latitudes ◽  
Polar Night ◽  
Solar Proton Events ◽  
Terminator Region

Abstract. Sudden changes in stratospheric chlorine species in the polar northern atmosphere, caused by the Solar Proton Events (SPEs) of 17 and 20 January 2005, have been investigated and compared with version 4 of the Whole Atmosphere Community Climate Model (WACCM4). We used Aura Microwave Limb Sounder (MLS) measurements to monitor the variability of ClO, HCl, HOCl and Michelson Interferometer for Passive Atmospheric Sounder (MIPAS) on ENVISAT to retrieve ClONO2. SPE-induced chlorine activation has been identified. HCl decrease occurred at nearly all the investigated altitudes with the lowest values (of less than 0.25 ppbv) on 21 January. HOCl was found to be the main active chlorine species under nighttime conditions (with increases of more than 0.2 ppbv) whereas both HOCl and ClO enhancements (about 0.1 ppbv) have been observed at the polar night terminator. Further, small ClO decreases (of less than 0.1 ppbv) and ClONO2 enhancements (about 0.2 ppbv) have been observed at higher latitudes (i.e., at nighttime) roughly above 2 hPa. While WACCM4 reproduces most of the SPE-induced variability in the chlorine species fairly well, in some particular regions discrepancies between the modeled and measured temporal evolution of the abundances of chlorine species were found. HOCl changes are modelled very well with respect to both magnitude and geographic distribution. ClO decreases are reproduced at high latitudes, whereas ClO enhancements in the terminator region are underestimated and attributed to background variations. WACCM4 also reproduces the HCl depletion in the mesosphere but it does not show the observed decrease below about 2 hPa. Finally, WACCM4 simulations indicate that the observed ClONO2 increase is dominated by background variability, although SPE-induced production might contribute by 0.1 ppbv.

scholarly journals Short- and medium-term atmospheric constituent effects of very large solar proton events

2008 ◽  
Vol 8 (3) ◽  
pp. 765-785 ◽  
Author(s):  
C. H. Jackman ◽  
D. R. Marsh ◽  
F. M. Vitt ◽  
R. R. Garcia ◽  
E. L. Fleming ◽  
...  
Keyword(s):  
Climate Model ◽  
Michelson Interferometer ◽  
Geomagnetic Latitude ◽  
High Energy ◽  
Solar Proton ◽  
Atmospheric Effects ◽  
Medium Term ◽  
Earth’S Atmosphere ◽  
Earth's Atmosphere ◽  
Solar Proton Events

Abstract. Solar eruptions sometimes produce protons, which impact the Earth's atmosphere. These solar proton events (SPEs) generally last a few days and produce high energy particles that precipitate into the Earth's atmosphere. The protons cause ionization and dissociation processes that ultimately lead to an enhancement of odd-hydrogen and odd-nitrogen in the polar cap regions (>60° geomagnetic latitude). We have used the Whole Atmosphere Community Climate Model (WACCM3) to study the atmospheric impact of SPEs over the period 1963–2005. The very largest SPEs were found to be the most important and caused atmospheric effects that lasted several months after the events. We present the short- and medium-term (days to a few months) atmospheric influence of the four largest SPEs in the past 45 years (August 1972; October 1989; July 2000; and October–November 2003) as computed by WACCM3 and observed by satellite instruments. Polar mesospheric NOx (NO+NO2) increased by over 50 ppbv and mesospheric ozone decreased by over 30% during these very large SPEs. Changes in HNO3, N2O5, ClONO2, HOCl, and ClO were indirectly caused by the very large SPEs in October–November 2003, were simulated by WACCM3, and previously measured by Envisat Michelson Interferometer for Passive Atmospheric Sounding (MIPAS). WACCM3 output was also represented by sampling with the MIPAS averaging kernel for a more valid comparison. Although qualitatively similar, there are discrepancies between the model and measurement with WACCM3 predicted HNO3 and ClONO2 enhancements being smaller than measured and N2O5 enhancements being larger than measured. The HOCl enhancements were fairly similar in amounts and temporal variation in WACCM3 and MIPAS. WACCM3 simulated ClO decreases below 50 km, whereas MIPAS mainly observed increases, a very perplexing difference. Upper stratospheric and lower mesospheric NOx increased by over 10 ppbv and was transported during polar night down to the middle stratosphere in several weeks past the SPE. The WACCM3 simulations confirmed the SH HALOE observations of enhanced NOx in September 2000 as a result of the July 2000 SPE and the NH SAGE II observations of enhanced NO2 in March 1990 as a result of the October 1989 SPEs.

scholarly journals Northern Hemisphere atmospheric influence of the solar proton events and ground level enhancement in January 2005

2011 ◽  
Vol 11 (3) ◽  
pp. 7715-7755 ◽  
Author(s):  
C. H. Jackman ◽  
D. R. Marsh ◽  
F. M. Vitt ◽  
R. G. Roble ◽  
C. E. Randall ◽  
...  
Keyword(s):  
Northern Hemisphere ◽  
Atmospheric Chemistry ◽  
Reasonable Agreement ◽  
Climate Model ◽  
Michelson Interferometer ◽  
Ground Level ◽  
Solar Proton ◽  
Ground Level Enhancement ◽  
Time Period ◽  
Solar Proton Events

Abstract. Solar eruptions in early 2005 led to a substantial barrage of charged particles on the Earth's atmosphere during the 16–21 January period. Proton fluxes were greatly increased during these several days and led to the production of HOx (H, OH, HO2) and NOx (N, NO, NO2), which then caused the destruction of ozone. We focus on the Northern polar region, where satellite measurements and simulations with the Whole Atmosphere Community Climate Model (WACCM3) showed large enhancements in mesospheric HOx and NOx constituents, and associated ozone reductions, due to these solar proton events (SPEs). The WACCM3 simulations show enhanced short-lived OH throughout the mesosphere in the 60–82.5° N latitude band due to the SPEs for most days in the 16–21 January 2005 period, in reasonable agreement with the Aura Microwave Limb Sounder (MLS) measurements. Mesospheric HO2 is also predicted to be increased by the SPEs, however, the modeled HO2 results are somewhat larger than the MLS measurements. These HOx enhancements led to huge predicted and MLS-measured ozone decreases of greater than 40% throughout most of the northern polar mesosphere during the SPE period. Envisat Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) measurements of hydrogen peroxide (H2O2) show increases throughout the stratosphere with highest enhancements of about 60 pptv in the lowermost mesosphere over the 16–18 January 2005 period due to the solar protons. WACCM3 predictions indicate H2O2 enhancements over the same time period of more than twice that amount. Measurements of nitric acid (HNO3) by both MLS and MIPAS show an increase of about 1 ppbv above background levels in the upper stratosphere during 16–29 January 2005. WACCM3 simulations show only minuscule HNO3 changes in the upper stratosphere during this time period. Polar mesospheric enhancements of NOx are computed to be greater than 50 ppbv during the SPE period due to the small loss rates during winter. Computed NOx increases, which were statistically significant at the 95% level, lasted about a month past the SPEs. The SCISAT-1 Atmospheric Chemistry Experiment Fourier Transform Spectrometer NOx measurements and MIPAS NO2 measurements for the polar Northern Hemisphere are in reasonable agreement with these predictions. An extremely large ground level enhancement (GLE) occurred during the SPE period on 20 January 2005. We find that protons of energies 300 to 20 000 MeV, not normally included in our computations, led to enhanced lower stratospheric odd nitrogen concentrations of less than 0.1% as a result of this GLE.

scholarly journals Northern Hemisphere atmospheric influence of the solar proton events and ground level enhancement in January 2005

2011 ◽  
Vol 11 (13) ◽  
pp. 6153-6166 ◽  
Author(s):  
C. H. Jackman ◽  
D. R. Marsh ◽  
F. M. Vitt ◽  
R. G. Roble ◽  
C. E. Randall ◽  
...  
Keyword(s):  
Northern Hemisphere ◽  
Atmospheric Chemistry ◽  
Climate Model ◽  
Michelson Interferometer ◽  
Ground Level ◽  
Solar Proton ◽  
Ground Level Enhancement ◽  
Time Period ◽  
Nitrogen Concentrations ◽  
Solar Proton Events

Abstract. Solar eruptions in early 2005 led to a substantial barrage of charged particles on the Earth's atmosphere during the 16–21 January period. Proton fluxes were greatly increased during these several days and led to the production of HOx (H, OH, HO2) and NOx (N, NO, NO2), which then caused the destruction of ozone. We focus on the Northern polar region, where satellite measurements and simulations with the Whole Atmosphere Community Climate Model (WACCM3) showed large enhancements in mesospheric HOx and NOx constituents, and associated ozone reductions, due to these solar proton events (SPEs). The WACCM3 simulations show enhanced short-lived OH and HO2 concentrations throughout the mesosphere in the 60–82.5° N latitude band due to the SPEs for most days in the 16–21 January 2005 period, somewhat higher in abundance than those observed by the Aura Microwave Limb Sounder (MLS). These HOx enhancements led to huge predicted and MLS-measured ozone decreases of greater than 40 % throughout most of the northern polar mesosphere during the SPE period. Envisat Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) measurements of hydrogen peroxide (H2O2) show increases throughout the stratosphere with highest enhancements of about 60 pptv in the lowermost mesosphere over the 16–18 January 2005 period due to the solar protons. WACCM3 predictions indicate H2O2 enhancements over the same time period of about three times that amount. Measurements of nitric acid (HNO3) by both MLS and MIPAS show an increase of about 1 ppbv above background levels in the upper stratosphere during 16–29 January 2005. WACCM3 simulations show only minuscule HNO3 increases (<0.05 ppbv) in the upper stratosphere during this time period. Polar mesospheric enhancements of NOx are computed to be greater than 50 ppbv during the SPE period due to the small loss rates during winter. Computed NOx increases, which were statistically significant at the 95 % level, lasted about a month past the SPEs. The SCISAT-1 Atmospheric Chemistry Experiment Fourier Transform Spectrometer NOx measurements and MIPAS NO2 measurements for the polar Northern Hemisphere are in reasonable agreement with these predictions. An extremely large ground level enhancement (GLE) occurred during the SPE period on 20 January 2005. We find that protons of energies 300 to 20 000 MeV, associated with this GLE, led to very small enhanced lower stratospheric odd nitrogen concentrations of less than 0.1 % and ozone decreases of less than 0.01 %.

scholarly journals Spatio-temporal observations of tertiary ozone maximum

2009 ◽  
Vol 9 (2) ◽  
pp. 6597-6615
Author(s):  
V. F. Sofieva ◽  
E. Kyrölä ◽  
P. T. Verronen ◽  
A. Seppälä ◽  
J. Tamminen ◽  
...  
Keyword(s):  
Climate Model ◽  
Solar Proton ◽  
Mixing Ratio ◽  
Polar Night ◽  
Night Time ◽  
Subsequent Decrease ◽  
Ozone Maximum ◽  
Low Concentrations ◽  
Spatio Temporal ◽  
In The Beginning

Abstract. We present spatio-temporal distributions of tertiary ozone maximum (TOM), based on GOMOS (Global Ozone Monitoring by Occultation of Stars) ozone measurements in 2002–2006. The tertiary ozone maximum is typically observed in the high-latitude winter mesosphere at altitude ~72 km. Although the explanation for this phenomenon has been found recently – low concentrations of odd-hydrogen cause the subsequent decrease in odd-oxygen losses – models have had significant deviations from existing observations until recently. Good coverage of polar night regions by GOMOS data has allowed for the first time obtaining spatial and temporal observational distributions of night-time ozone mixing ratio in the mesosphere. The distributions obtained from GOMOS data have specific features, which are variable from year to year. In particular, due to a long lifetime of ozone in polar night conditions, the downward transport of polar air by the meridional circulation is clearly observed in the tertiary ozone maximum time series. Although the maximum tertiary ozone mixing ratio is achieved close to the polar night terminator (as predicted by the theory), TOM can be observed also at very high latitudes, not only in the beginning and at the end, but also in the middle of winter. We have compared the observational spatio-temporal distributions of tertiary ozone maximum with that obtained using WACCM (Whole Atmosphere Community Climate Model) and found that the specific features are reproduced satisfactorily by the model. Since ozone in the mesosphere is very sensitive to HOx concentrations, energetic particle precipitation can significantly modify the shape of the ozone profiles. In particular, GOMOS observations have shown that the tertiary ozone maximum was temporarily destroyed during the January 2005 and December 2006 solar proton events as a result of the HOx enhancement from the increased ionization.

scholarly journals Enhancement of N<sub>2</sub>O during the October–November 2003 solar proton events

2008 ◽  
Vol 8 (2) ◽  
pp. 4669-4691 ◽  
Author(s):  
B. Funke ◽  
M. García-Comas ◽  
M. López-Puertas ◽  
N. Glatthor ◽  
G. P. Stiller ◽  
...  
Keyword(s):  
Atmospheric Model ◽  
Solar Proton ◽  
Polar Regions ◽  
Polar Night ◽  
Present Evidence ◽  
Solar Proton Events

Abstract. In this paper we present evidence of enhanced N2O concentrations in the upper stratosphere/lower mesosphere polar regions after the solar proton events that occurred during October–November 2003. The observations were performed by the MIPAS instrument on the Envisat satellite. Simulations performed using the Canadian Middle Atmospheric Model (CMAM) show that such enhancements are most likely produced by the reaction of N(4S) with NO2, both of which species are largely enhanced just after the solar proton events in the winter polar night.

The effect of Forbush decreases on the polar-night HOx concentration

2021 ◽  
Author(s):  
Irina Mironova
Keyword(s):  
Forbush Decrease ◽  
Cosmic Ray ◽  
Solar Proton ◽  
Polar Night ◽  
Forbush Decreases ◽  
Ozone Loss ◽  
Solar Proton Events ◽  
Hydrogen Oxide ◽  
The Impact ◽  
Ionization Rates

&lt;div&gt; &lt;div&gt; &lt;div&gt; &lt;p&gt;It is well-known that energetic particle precipitations during solar proton events increase ionization rates in the middle atmosphere enhancing the production of hydrogen oxide radicals (HOx) involved in the catalytic ozone destruction cycle. There are many studies where the contribution of energetic particles to the formation of hydrogen oxide radicals and ozone loss has been widely investigated. However, until now, there was no solid evidence that the reduction in galactic cosmic ray fluxes during a magnetic storm, known as Forbush-effect, directly and noticeably affects the polar-night stratospheric chemistry.&lt;br&gt;Here, the impact of the Forbush decrease on the behaviour of hydrogen oxide radicals was explored using the chemistry-climate model SOCOL.&lt;br&gt;We found that hydrogen oxide radical lost about half of its concentration over the polar boreal night stratosphere owing to a reduction in ionization rates caused by Forbush decreases after solar proton events occurred on 17 and 20 of January 2005. A robust response in ozone was not found. There is not any statistically significant response in (NOx) on Forbush decrease events as well as over summertime in the southern polar region.&lt;br&gt;The results of this study can be used to increase the veracity of ozone loss estimation if stronger Forbush events can have a place.&lt;/p&gt; &lt;p&gt;Reference: Mironova I, Karagodin-Doyennel A and Rozanov E (2021) , The effect of Forbush decreases on the polar-night HOx concentration affecting stratospheric ozone. Front. Earth Sci. 8:618583. doi: 10.3389/feart.2020.618583&lt;/p&gt; &lt;p&gt;https://www.frontiersin.org/articles/10.3389/feart.2020.618583/full&lt;/p&gt; &lt;p&gt;The study was supported by the Russian Science Foundation grant (RSF project No. 20-67-46016).&lt;/p&gt; &lt;/div&gt; &lt;/div&gt; &lt;/div&gt;

scholarly journals Enhancement of N<sub>2</sub>O during the October–November 2003 solar proton events

2008 ◽  
Vol 8 (14) ◽  
pp. 3805-3815 ◽  
Author(s):  
B. Funke ◽  
M. García-Comas ◽  
M. López-Puertas ◽  
N. Glatthor ◽  
G. P. Stiller ◽  
...  
Keyword(s):  
Atmospheric Model ◽  
Solar Proton ◽  
Polar Regions ◽  
Polar Night ◽  
Present Evidence ◽  
Solar Proton Events

Abstract. In this paper we present evidence of enhanced N2O concentrations in the upper stratosphere/lower mesosphere polar regions after the solar proton events that occurred during October–November 2003. The observations were performed by the MIPAS instrument on the Envisat satellite. Simulations performed using the Canadian Middle Atmospheric Model (CMAM) show that such enhancements are most likely produced by the reaction of N(4S) with NO2, both of which species are largely enhanced just after the solar proton events in the winter polar night.

scholarly journals Spatio-temporal observations of the tertiary ozone maximum

2009 ◽  
Vol 9 (13) ◽  
pp. 4439-4445 ◽  
Author(s):  
V. F. Sofieva ◽  
E. Kyrölä ◽  
P. T. Verronen ◽  
A. Seppälä ◽  
J. Tamminen ◽  
...  
Keyword(s):  
Climate Model ◽  
Solar Proton ◽  
Mixing Ratio ◽  
Polar Night ◽  
Night Time ◽  
Subsequent Decrease ◽  
Ozone Maximum ◽  
Low Concentrations ◽  
Spatio Temporal ◽  
In The Beginning

Abstract. We present spatio-temporal distributions of the tertiary ozone maximum (TOM), based on GOMOS (Global Ozone Monitoring by Occultation of Stars) ozone measurements in 2002–2006. The tertiary ozone maximum is typically observed in the high-latitude winter mesosphere at an altitude of ~72 km. Although the explanation for this phenomenon has been found recently – low concentrations of odd-hydrogen cause the subsequent decrease in odd-oxygen losses – models have had significant deviations from existing observations until recently. Good coverage of polar night regions by GOMOS data has allowed for the first time to obtain spatial and temporal observational distributions of night-time ozone mixing ratio in the mesosphere. The distributions obtained from GOMOS data have specific features, which are variable from year to year. In particular, due to a long lifetime of ozone in polar night conditions, the downward transport of polar air by the meridional circulation is clearly observed in the tertiary ozone maximum time series. Although the maximum tertiary ozone mixing ratio is achieved close to the polar night terminator (as predicted by the theory), TOM can be observed also at very high latitudes, not only in the beginning and at the end, but also in the middle of winter. We have compared the observational spatio-temporal distributions of the tertiary ozone maximum with that obtained using WACCM (Whole Atmosphere Community Climate Model) and found that the specific features are reproduced satisfactorily by the model. Since ozone in the mesosphere is very sensitive to HOx concentrations, energetic particle precipitation can significantly modify the shape of the ozone profiles. In particular, GOMOS observations have shown that the tertiary ozone maximum was temporarily destroyed during the January 2005 and December 2006 solar proton events as a result of the HOx enhancement from the increased ionization.

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