Interactive comment on “ Energetic particle induced interannual variability of ozone inside the Antarctic polar vortex observed in satellite data ” by T

Introduction Conclusions References


Introduction
Energetic particles (∼ keV-∼ MeV), mainly originating from the sun but also from the Earth's magnetospheric radiation belts and the aurora region, penetrate the atmosphere down to mesospheric and stratospheric regions, depending on their energy.The particles are guided by the Earth's magnetic field lines and therefore mostly precipitate at auroral and radiation belt areas (∼ 55-70 • geomagnetic latitudes), depositing energy and directly influencing the chemical composition of the stratosphere and mesosphere.Due to the air compounds, precipitating particles mainly produce large abundances of O + 2 as well as N( 2 D) and N + 2 .N( 2 D) and N + 2 lead to increased concentrations of odd 31250 Introduction

Conclusions References
Tables Figures

Back Close
Full nitrogen (NO x = N + NO + NO 2 ) through a number of reactions, including dissociative recombination of N + 2 and ion-neutral chemistry with species of the oxygen family (e.g.Rusch et al., 1981).Additionally, O + 2 and water vapour initialise chain reactions associated with water cluster ion formation and accompanied recombination reactions, which eventually lead to the production of odd hydrogen (HO x = H + OH + HO 2 ; e.g.Solomon et al., 1981).
Both HO x and NO x play an important role in destroying O 3 in the mesosphere and stratosphere (e.g.Lary, 1997).However, HO x is short-lived (∼ seconds-hours) and therefore more important near its source region in the mesosphere, while NO x has a relatively long life time (∼ days-months), at least during night-time conditions.Consequently, NO x can be transported downwards inside the polar vortex (e.g.Solomon et al., 1982) from the upper mesosphere/lower thermosphere down to the stratosphere, resulting in stratospheric O 3 depletion through catalytic chemical reactions in combination with solar radiation.Thus, energetic particle precipitation (EPP) indirectly affects O 3 during polar winter.Since O 3 is the major radiative heating source in the stratosphere, variations of this gas will also influence the stratospheric temperature field and eventually lead to altered atmospheric dynamics.However, the atmospheric response to EPP is not fully understood so far.The current knowledge is discussed in more detail by Sinnhuber et al. (2012).
Observations of the EPP indirect effect on stratospheric polar O 3 are relatively rare, at least compared to other latitudes, due to a lack of long-term O 3 measurements in these regions.However, a hint for this mechanism was presented by Randall et al. (1998) which analysed the Polar Ozone and Aerosol Measurement instrument data, revealing a close anticorrelation between NO 2 and O 3 mixing ratios in winter/spring from 1994-1996 in the Antarctic stratosphere (∼ 25-35 km).They suggested that the relationship cannot originate from downwards transported O 3 -deficient air but is due to photochemical destruction of O 3 by NO 2 .Further observations from several satellite instruments from 1992-2005 show, that, the stratospheric NO x enhancement in the Southern Hemisphere is caused by EPP (Randall et al., 2007).More recent Introduction

Conclusions References
Tables Figures

Back Close
Full satellite observations from 2002-2012 reported by Funke et al. (2014) reveal that particle induced NO x is indeed transported downwards to the middle stratosphere at polar latitudes, while further model studies suggest that the subsiding of NO x leads to strongly reduced stratospheric O 3 concentrations (∼ 30%) down to altitudes ∼ 30 km (e.g.Reddmann et al., 2010).Thus, it appears promising to search for a link between EPP and O 3 in actual data sets, because the downwards propagating signal of the EPP indirect effect on stratospheric and mesospheric O 3 throughout the polar winter has not been explicitly observed so far.Note that, NO x can be only transported downwards inside a stable large-scale dynamical structure, which provides sufficient subsidence and prevents NO x removal/dilution by horizontal transport.These conditions are found primarily inside the Antarctic polar vortex, because the Arctic vortex is strongly disrupted by planetary waves, leading to its weakening or temporary breakdown.and the relation to a number of solar and geomagnetic indices, namely the F10.7 cm solar radio flux, the Ap index, and the ≥ 2 MeV electron flux is analysed.

Approximation of the Antarctic polar vortex
The position and the extension of the Antarctic polar vortex were estimated by using the gradient of the potential vorticity (PV) on isentropic surfaces (Nash et al., 1996).Introduction

Conclusions References
Tables Figures

Back Close
Full Assuming a dry atmosphere at altitudes ≥ 20 km, the PV was calculated from temperature, pressure, relative vorticity, and the corresponding latitude taken from ERA-Interim (https://ecaccess.ecmwf.int/ecmwf), the latest version of global atmospheric reanalysis data produced by the European Centre for Medium-Range Weather Forecasts (ECWMF).The reference pressure was set to 1000 hPa and the gravitational constant was considered to be dependent on latitude and height.The PV was calculated for all height intervals between 20 and 70 km which were adapted from the MIPAS retrieval grid (see Sect. 2.2.1).As an example, Fig. 1 shows the PV, depending on time and equivalent latitude (EQL), during the Antarctic winter 2011 at ∼ 40 km.The EQLs assigned to an individual PV isoline enclose the same area as the geographical latitudes of equivalent values.However, this area is located around an estimate of the vortex centre position, rather than around the geographical pole.In general, the EQL of the strongest PV gradient indicates the estimated location of the vortex edge, however, in most cases, there are at least two locations revealing gradients of similar magnitude.Therefore, Nash et al. (1996) also considered the zonal wind to locate the real vortex edge, but here we added a visual analysis instead of the zonal wind to divide the Southern Hemisphere into three non-overlapping zones: deep inside the Antarctic polar vortex (CORE) and the corresponding outermost edge (EDGE), covering all EQLs poleward the respective borders, as well as an area not influenced by the vortex (OUT-SIDE), which extends from the equator to the respective OUTSIDE border.In this study we will consider the EDGE region as the Antarctic vortex area, but the CORE and OUT-SIDE region are still necessary to determine whether the observed features inside the EDGE zone are actually originating from the vortex itself.The limits of the three regions of each height interval revealed no strong variation from 2002-2011, therefore holding for every winter (Table 1).Note that the ECMWF ERA-Interim data only covers heights up to ∼ 63 km.However, considering the behaviour of the Antarctic vortex at altitudes between 60 and 70 km (Preusse et al., 2009, their Fig. 2a), it seems reasonable to assume that the estimated limits of the three regions at ∼ 63 km are also valid up to 70 km.et al. (2003, 2009) and Glatthor et al. (2006).Note that the number of tangent heights is constant during P1 (17) and P2 (23), and that the actually available altitudes (cloud contaminated observations are disregarded) only slightly differ from day to day.The corresponding vertical resolution becomes coarser at higher altitudes (independent of the geographical location), increasing from 3.5 to 8 km (Steck et al., 2007) and from 2.5 to 5 km (Eckert et al., 2014) in P1 and P2, respectively.However, the retrieval grid in all MIPAS O 3 data versions used here (V3O_O3_9, V5R_O3_220, V5R_O3_221) is independent of the tangent heights, with a grid width of 1 km below 44 and 2 km above.
During P1/P2 O 3 was measured at two different wavelength intervals, ranging from 9.0-9.4µm/9.6-9.7 µm and 12.5-13.5µm/12.7-13.2µm in particular.However, not the full spectral ranges were used, but sub-intervals (microwindows).These were selected to minimise the computing time and to optimize the relation between the measurement-Introduction

Conclusions References
Tables Figures

Back Close
Full noise induced random error and other errors.These other errors originate, among further error sources, from spectral contributions of further atmospheric constituents of unknown abundances.It should also be noted that there is a bias in MIPAS O 3 data between the two periods, which was estimated using a multi-linear parametric trend model (Eckert et al., 2014).To accept an O 3 data point, the recommended filter criteria for MIPAS O 3 data were applied by using an averaging kernel diagonal value > 0.03 as well as the visibility flag = 1 which indicates spectral available data.At least 10 accepted data points inside the Antarctic polar vortex at a certain grid level were required to calculate the arithmetic average of one day, while at least 13 days were arithmetically averaged to a 26 day running mean from 1 April-1 November, repeating this algorithm for each height interval and all years from 2002-2011.The time interval of 26 days was chosen to minimise a possible influence of the 27 day cycle of the sun, also ensuring that each time interval includes only one 27 day solar rotation maximum at most.The analysis was repeated for NO 2 (V5R_NO2_220, V5R_NO2_221) and the corresponding retrieval is described in Funke et al. (2005Funke et al. ( , 2011)).

SABER
The SABER instrument on board the TIMED Satellite has been nearly continuously operating since January 2002, measuring vertical profiles of several atmospheric parameters and minor constituents (e.g.O 3 ) from the surface up to altitudes > 100 km.The SABER measurements are governed by a periodic quasi 60 day cycle, each time changing from the Southern Hemisphere mode (83 • S-52 • N) to the Northern Hemisphere mode ( 52• S-83 • N) and vice versa.Note that the "switching day" is only varying and the measurements of both versions were restricted to values < 20 ppm to exclude outliers.Comparisons with the results of an increased threshold to < 100 ppm revealed only minor differences (not shown here).The investigated height interval, ranging from 20 to 70 km, is divided in 38 non-overlapping subintervals and binned at the same altitudes as MIPAS data.The algorithm used to calculate the running means is also identical to the one applied for the "accepted" MIPAS data points.However, SABER needs approximately 60 days to cover all local times, leading to a quasi 60 day wave like oscillation in O 3 if 26 day running means are used.This behaviour becomes evident at altitudes > 50 km, where the averaging interval was consequently extended from 26 to 60 days.Note that the calculation of the 60 day running means required at least 30 days.

SMR
The Odin satellite mission started in February 2001 and is a joint project between Sweden, Canada, France and Finland (Murtagh et al., 2002).Odin was launched into a sun-synchronous polar orbit, carrying the SMR instrument and nominally covering the latitude range from 82.5 • S-82.5 • N. The SMR makes vertical profile measurements during both day and night, while passing the equator at ∼ 6:00/18:00 LT in the descending/ascending node.The O 3 data were extracted from the Odin/SMR Level 2 data product, version 2.0 (http://odin.rss.chalmers.se/,Urban et al., 2005), only using measurements of the frequency band centred around ∼ 544.6 GHz, providing vertical O 3 profiles in the ∼ 15-70 km altitude range.The filtering criterion used for SMR is the measurement response, which corresponds to the sum of the rows of the averaging kernel matrix.The profiles characterized by a measurement response lower than 0.9 are not reliable enough, and are therefore excluded.The algorithm to calculate the 26 day running means is identical to the one applied to MIPAS data.Note that Odin/SMR was a two-discipline satellite until April 2007, switching between atmospheric (aeronomy mode) and astronomy observations, and is entirely dedicated to aeronomy since this date.Additionally, measurements in the relevant mode are only Introduction

Conclusions References
Tables Figures

Back Close
Full performed every day, consequently only covering about one day out of three before April 2007 and every other day afterwards.However, the calculation of the 26 day running means is still possible because the data gaps occur in a regular way, so they do not essentially worsen the 26 day averages.The vertical resolution of the data version used here is better than 3 below 45 km, but increases to 5-6 km (50-60 km) and 7-10 km (60-70 km), leading to noisy results at altitudes > 50 km compared to the other two instruments.

Solar data and geomagnetic indices
The data of the indices were obtained from two different websites provided by the National Geophysical Data Center.In detail the flux of the 10.7 cm radio emission from the sun (F10.7) and the geomagnetic Ap index (Ap), commonly used proxies for solar variation and geomagnetic activity, respectively, were downloaded from http://spidr.ngdc.noaa.gov/spidr/.The ≥ 2 MeV electron flux (2 MeV), including the flux of all electrons with energy levels above 2 MeV, was used here as an indicator of the influence from the magnetosphere.The corresponding time series were measured by the Geostationary Operational Environmental Satellites and downloaded from ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SATELLITE_ENVIRONMENT/Daily_Fluences/.Note that the 2 MeV data set also considers contamination effects on the electron detectors on the spacecrafts due to protons > 32 MeV.The time series of all data sets are based on daily values, which were arithmetically averaged to 26 day means centred at 1 April, 1 May, and 1 June.The means were separately calculated for each index for the individual years from 2002-2011, however, 2 MeV data are only available until 2010.

Numerical modelling
The three-dimensional chemistry and transport model (3dCTM; Sinnhuber et al., 2012, appendix 1) used here is based on the Bremen 3dCTM (e.g.Wissing et al., 2010), extending on 47 pressure levels from the tropopause up to the lower thermosphere Introduction

Conclusions References
Tables Figures

Back Close
Full (∼ 10-140 km) with a latitude/longitude resolution of 2.5 • × 3.75 • .The model was recently updated with a variable H 2 and O 2 distribution, leading to proper HO x and consequently night time O 3 values at altitudes > 60 km (see Sect. 1).The 3dCTM is driven by meteorological data obtained from simulations of the three-dimensional dynamical model LIMA (Berger, 2008) and the advection is calculated by applying the second-order moments scheme reported by Prather (1986).In the stratosphere, a family approach for the chemical families: O In this study the 3dCTM was used to investigate the impact of precipitating particles on O 3 inside the Antarctic polar vortex at altitudes from 20-70 km.After a multiyear two-dimensional model spin-up, two simulations from 2003-2009 were performed.The first run (base run) does not consider any energetic particles, while the second run (EP run) includes ionisation effects by both protons and electrons, using the ionisation rates provided by the Atmospheric Ionisation Module Osnabrück (AIMOS; Wissing and Kallenrode, 2009).The resulting NO x production per created ion pair includes various ionic and neutral reactions depending on the atmospheric background state (Nieder et al., 2014).Simple parameterisations are used for the production of HO x (Solomon et al., 1981) and O (Porter et al., 1976).Note that heterogeneous chemistry was not included, which only becomes important during spring in the lower stratosphere.Both model runs considered constant solar minimum conditions (F10.first builds up in April.Therefore the focus is set on the O 3 response to indices centred around 1 April.The O 3 amplitude was calculated for the all three regions (CORE, EDGE, and OUTSDIE) which were introduced in Sect.2.1.The corresponding results reveal that the pattern found inside the EDGE region are fairly similar and less noisy compared to the features observed in the CORE area (not shown here).In contrast the O 3 amplitudes outside the Antarctic polar vortex are fundamentally different.An example for the O 3 response associated to 1 April Ap in the EDGE and the OUTSIDE region derived from MIPAS measurements is presented in Fig. 2, showing considerably disagreeing structures and essentially weaker amplitudes, especially below 50 km.Thus comparison between the individual regions of the Southern Hemisphere ensures, that, the pattern found in the EDGE region are actually originating from the Antarctic polar vortex.
Figure 3 displays the corresponding results of the O 3 amplitude from 2002-2011, but only for values above the significance level of 95 % while shaded areas show regions between the significance level of 95 and 99 %.The significance was calculated according to a Student's t test, based on the error of the mean of the 26 day running O 3 means and assuming the worst case scenario of absolute error propagation.The MIPAS O 3 measurements (left column) reveal a high negative response to Ap (upper row) in early Antarctic winter > 60 km, on average ranging around −10 %.Further striking negative O 3 amplitudes occur in July between 30 and 40 km as well as around 1 October at ∼ 30 km, at least weakly indicating the downward transport of the Ap signal in stratospheric O 3 due to NO x predicted by model studies (e.g.Reddmann et al., 2010).In contrast, a positive O 3 amplitude is found at the beginning of the winter between ∼ 25 and ∼ 55 km (∼ 10-20 %), as well as at altitudes < 30 km throughout the winter (up to ∼ 20% in October at ∼ 20 km) and above the indicated subsiding layer of negative amplitudes.But considering that most of these features drop below the significance level of 95 % by combining the data of all three instruments (right column), a more detailed investigation of these pattern is not reasonable.However, the results of the merged data set show a well pronounced subsiding negative Ap signal from ∼ 50 km in June Introduction

Conclusions References
Tables Figures

Back Close
Full down to ∼ 25 km in October, which is disrupted in August, while the generally positive structures below 30 km are also still present.
The O 3 response to 2 MeV (middle row) derived from MIPAS observations also indicates a downwelling of negative O 3 amplitudes, descending from ∼ 60 km in June down to ∼ 30 km in late August.Additionally, the MIPAS O 3 response to 2 MeV in early winter is reversed compared to the corresponding influence from Ap on O 3 , which does not originate from missing 2 MeV data from 2011.Strong positive O 3 amplitudes are generally observed throughout the winter below 30 km, exceeding values of ∼ 20% in April and October, as well as during October between 30 and 50 km where the maximum amplitude is lower (∼ 10%).The positive features can be validated with the composite results even if they are damped in the region below 30 km.However, this is not the case for the negative response, except for a small area in June in the lower mesosphere.
The O 3 response to F10.7 (lowermost row) is fairly similar between MIPAS and the merged measurements, and both also agree with the respective pattern observed for Ap, including the indicated downwelling of negative O 3 amplitudes during midwinter from 50 to 25 km.The composite O 3 shows strong positive amplitudes in May > 55 km which originate from SMR measurements and are most likely due to the low vertical resolution of the SMR instrument at these altitudes (see Sect. 2.2.3).The high agreement between the results of Ap/O 3 and F10.7/O 3 might originate from the coupling of both indices during solar maximum years (Gray et al., 2010, their Fig. 1).In order to investigate a possible cross-correlation between solar radiation and geomagnetic disturbances, the analysis was repeated for years of moderate solar activity, only including 2005-2010 (Fig. 4).Similar analyses to extract a more distinct solar signal during times of approximately constant geomagnetic activity were not reasonable, because the respective years of nearly constant Ap values (2002,2005,2006,2008,2010) do not provide a sufficient amount of data in MIPAS and SMR measurements.Introduction

Conclusions References
Tables Figures

Back Close
Full below 50 km and propagating downwards to ∼ 25 km throughout the winter.However, the middle part of the downwelling between late July and late September is below the significance level of 95 % and therefore not shown here.Furthermore, the hinted subsidence is closely surrounded by well pronounced positive O 3 amplitudes, especially below ∼ 30 km which maximise in September (> 20%).There is also a negative structure centred at 1 June at ∼ 60 km, which cannot be caused by NO x but most likely results from HO x formation (see Sect. 1).Considering the composite results, the downwelling Ap signal in O 3 becomes apparent and robust but slightly weaker (∼ −10 %) while the positive features are also damped but still present.The mesospheric response is generally weak and the high positive O 3 amplitudes in May are again caused by the SMR measurements.
The 2 MeV impact on MIPAS O 3 shows generally agreeing features with the influence of the geomagnetic activity and is also of similar magnitude, however, the downwelling negative signal is hinted to already start in late May at ∼ 55 km.In contrast to the O 3 response to Ap, the downwards propagating 2 MeV signal is less robust and can be only guessed in the composite O 3 amplitude, while the positive structures (∼ 10-15 %) in August below 30 km and in September between 30 and 50 km are still present.In general, the 2 MeV features are less obvious in the O 3 composite, except for the positive O 3 amplitudes above the hinted downward transport.Nevertheless, the agreement between Ap and 2 MeV pattern is quite strong, in MIPAS observations in particular, although both parameters are only indirectly related to O 3 .However, the O 3 feedback to both indices is far too similar and additionally found in all three instruments to be Introduction

Conclusions References
Tables Figures

Back Close
Full a coincidence, even if the descending O 3 response to 2 MeV is weaker.That strongly indicates a related source mechanism, suggesting solar wind variability.
Considering the entire process, that energetic particles produce NO x which eventually destroys stratospheric O 3 , the Ap impact observed in O 3 (see Fig. 5) is expected to be reversed in NO x , at least in the stratosphere.In order to investigate this in more detail, the analysis was repeated for 1 April Ap and NO x .Here NO x , is represented only by NO 2 from MIPAS observations, because the respective NO measurements are quite noisy compared to NO 2 , especially below 30 km.This is still reasonable because NO is converted to NO 2 during night and therefore NO 2 is the major fraction of NO x inside the Antarctic polar vortex.The corresponding results include the years 2005-2010 and are displayed in Fig. 6, supporting that the stratospheric O 3 depletion can be indeed associated to the catalytic NO x /O 3 cycle.The Ap signal in NO 2 is stronger by the factor of 2-5, compared to the respective O 3 amplitudes.The sharp gradient in mid July originates from 2005 NO 2 data, which are not available afterwards.However, the general structure of the subsiding Ap signal in NO 2 is still similar with and without 2005 observations.Note that the essentially smaller NO 2 amplitudes in October below the significance level of 95 % are not in conflict with the respective well pronounced negative O 3 response, because the latter one results from an accumulation effect from the NO 2 above.Furthermore, large negative NO 2 amplitudes throughout the entire winter below ∼ 30 km are observed, matching the high positive O 3 feedbacks to Ap.A possible reason for this behaviour might be that NO 2 is stored in reservoir species, like ClONO 2 and HNO 3 , due to reactions with ClO and OH, respectively (López-Puertas et al., 2005, their reactions 1 and 12).This eventually leads to lower NO x concentrations and consequently slows down the catalytic O 3 depletion.Based on the corresponding MIPAS climatologies (not shown here), HNO 3 is more important until mid July, while ClONO 2 is dominating afterwards and its influence becomes essentially crucial in spring due to heterogeneous chemistry which has taken place before.Furthermore, the positive O 3 amplitudes below ∼ 30 km could be also partly explained by the self healing effect of O 3 (Jackman and McPeters, 1985).Altitude regions of reduced O 3 will lead to increased Introduction

Conclusions References
Tables Figures

Back Close
Full solar UV radiation in the layers directly below.This is accompanied by a higher production of atomic oxygen and would consequently increase the formation of O 3 .However, this proposed mechanism would only have an additional effect, contributing to the formation of O 3 in the atmospheric layer right below the subsidence, but cannot account for the entire region.Note that this layer is also present throughout the entire winter, and thus an influence from the vortex above is unlikely but any further investigations are beyond the scope of this study.Additionally, the area of high positive Ap/O 3 structure between 35 and 50 km from August-September cannot be explained by the NO x /O 3 cycle.However, the respective Ap influence of NO 2 is below the 95 % significance level and is therefore at least not in conflict with a higher O 3 response.Furthermore, this positive Ap impact on O 3 is essentially less visible in the composite results than in MI-PAS data, and a corresponding composite analysis for Ap/NO 2 is necessary for a more detailed investigation.But this is not possible due to non-existing NO 2 measurements from SABER and SMR.

Comparison with 3dCTM
The simulated O 3 amplitude between the EP run and base run, representing high and low geomagnetic activity, respectively, is displayed in Fig. 7.Note that the modelled O 3 amplitude is also referred to as O 3 amplitude here, which is justified because "observed" and "modelled" O 3 amplitude still hold the same physical meaning, even if the calculation algorithm is slightly different.It is reasonable to investigate the complete The qualitative agreement between model results and observations in the stratosphere suggests that the subsiding Ap signal found in O 3 is actually originating from particle precipitation.However, the simulated downwelling starts at altitudes > 60 km while observations reveal no obvious structures in the mesosphere, possibly caused by satellite sampling.As already stated in Sect 3.1.2,the mesospheric behaviour cannot be caused by NO x , because the NO x /O 3 cycle is not efficiently working at these altitudes.Thus the O 3 depletion > 50 km could be accounted to OH production, which is most likely overestimated in the model and consequently leads to an increased O 3 depletion not observed by the satellite instruments.

Conclusions
We ering the period of solar minimum activity from 2005-2010 we found a negative O 3 response caused by geomagnetic activity (Ap) from 1 April in all three instruments, ranging from −5 to −10 % and propagating downwards throughout the Antarctic winter from ∼ 50 down to ∼ 25 km.This subsiding negative signal in O 3 is above the significance level of 95 % and overlaps with the corresponding positive NO 2 response to 1 April Ap, supporting that NO x is indeed the cause of the O 3 depletion.We could also show that the high positive O 3 feedback below 30 km, which is present during the entire winter, is in agreement with respective negative NO 2 structures.The cause of the NO 2 behaviour is possibly related to the formation of the reservoir species ClONO 2 and HNO 3 , slowing down the catalytic destruction of O 3 by Cl.The O 3 pattern induced by the magnetosphere (2 MeV) from 1 April are similar but weaker, compared to the respective geomagnetic activity, still suggesting a related source mechanism between 2 MeV and Ap like solar wind variability.The composite observations of all three instruments are in good qualitative agreement with 3dCTM simulation, revealing similar O 3 pattern induced by the geomagnetic activity from 1 April while the simulated O 3 response is larger but still in the same order of magnitude.However, we have to point out that the validity of the subsiding O 3 depletion associated to geomagnetic activity and NO x is not ensured due to the short time series of only 6 years at most.Thus, we conclude that precipitating particles are strongly indicated as a factor contributing to stratospheric O 3 during Antarctic winter, but we cannot prove the link unambiguously.Introduction

Conclusions References
Tables Figures

a
few days from year to year.To consider both day and night O 3 observations, SABER Level 2A Ozone96 data v2.0 and v1.07 (http://saber.gats-inc.com/custom.php,Rong et al., 2009) measured at ∼ 9.6 µm are used.However, v1.07 was only used to fill v2.0 data gaps, which seemed reasonable because the data fit quite well the results of the performed analysis during the respective periods (15-31 May, 7-31 August, not shown here).Consequently, the combined data set of both versions shows no larger data gap Discussion Paper | Discussion Paper | Discussion Paper | Screen / Esc Printer-friendly Version Interactive Discussion Discussion Paper | Discussion Paper | Discussion Paper | Discussion Paper | Screen / Esc Printer-friendly Version Interactive Discussion Discussion Paper | Discussion Paper | Discussion Paper | Discussion Paper | 7 = 70 × 10 −22 W m −2 Hz −1 ) to exclude O 3 variations due to solar activity.The obtained O 3 model results of both runs were separately selected according to the vertical MIPAS retrieval grid for direct comparisons to the observations, repeating the described algorithm to calculate the 26 day running means.Finally, in order to derive the O 3 vmr variations solely originating from precipitating particles, the obtained averages of the base run were subtracted from the corresponding O 3 values of the EP run.The results were divided by the arithmetic mean of both runs and eventually multiplied by 100 %.O 3 vmr averages from 2002-2011 of each altitude-time interval (1 April-1 November, 20-70 km) were individually grouped into years of high and low index activity.For this purpose the index median of the corresponding time series of the 26 day average of an index (F10.7,Ap, 2 MeV) centred around 1 April was calculated, only including years of actually available O 3 observations.Therefore the median of an index time series works as a threshold, dividing the entire time interval from 2002-2011 in years of high (above the median) and low (below the median) index activity.Note that the classification of the years does not only depend on the chosen index, but due to data gaps also on the considered height-time interval as well as the instrument used.Afterwards the arithmetic O 3 mean of the years of low index activity was subtracted from the O 3 mean of the years of high index activity, eventually dividing this absolute O 3 difference by the arithmetic O 3 average of the entire observation period and multiplying the results by 100 % for more handy values.Thus the calculated relative O 3 difference (referred to as O 3 amplitude here) represents the impact of the respective index on the O 3 background.To reduce the measurement noise of the individual instruments, the results of all three instruments were merged by simply calculating the arithmetic average but only if the corresponding O 3 amplitude of all three instruments was available.Note that due to the major sudden stratospheric warming centred around 27 September (Azeem et al., 2010) the O 3 observations from 1 September-1 November 2002 were excluded.In contrast, the solar proton event in the end of October 2003 (Jackman et al., 2005) was neglected due to its late occurrence.The performed analyses with O 3 observations, considering the indices from 1 May and 1 June (not shown here), revealed no essential differences compared to 1 April or the structures became less obvious.Comparisons with earlier periods are not reasonable because the vortex Discussion Paper | Discussion Paper | Discussion Paper | Screen / Esc Printer-friendly Version Interactive Discussion Discussion Paper | Discussion Paper | Discussion Paper | Discussion Paper |

Figure 5
Figure 5 displays the obtained O 3 amplitudes for solar quiet times (2005-2010) associated to 1 April Ap, again only showing values above 95 % significance level and shading the area of regions between 95 and 99 %.The MIPAS O 3 response to Ap indicates a subsiding negative signal (∼ −10 to −15 %), starting in late June slightly Screen / Esc Printer-friendly Version Interactive Discussion Discussion Paper | Discussion Paper | Discussion Paper | Discussion Paper | Screen / Esc Printer-friendly Version Interactive Discussion Discussion Paper | Discussion Paper | Discussion Paper | Discussion Paper | simulated time interval from 2003-2009, because the model runs represent solar minimum conditions similar to the years 2005-2010.The results reveal apparent negative O 3 amplitudes propagating downwards throughout the winter with maximum negative values during midwinter between 45 and 60 km.The subsidence shows larger negative O 3 amplitudes compared to the measurements and is also much broader, which might be due to the constant F10.7 and the prescribed dynamics, both reducing the inter-annual variability of O 3 .Furthermore, we performed an on/off experiment, while in reality the EEP indirect effect is a persistent feature.Below 30 km the observed high 31264 Discussion Paper | Discussion Paper | Discussion Paper |positive O 3 amplitudes associated to Ap are only indicated in the model results by essentially weaker and additionally negative amplitudes.However, the model amplitudes are at least less negative compared to the values above.The second positive region above the downwelling is completely missing.Further note that the strong positive feedback during late winter/early spring below 30 km might not be reproduced by the model due to missing heterogeneous chemistry.The proposed self healing effect of O 3 (see Sect 3.1.2)was also tested, using O 1 D as a proxy for the O 3 photolysis rate in the Lyman-alpha band and calculating the O 1 D amplitude (not shown here).However, the expected positive response directly below the downwelling is only partly visible and even below the 67 % significance level.
have investigated the O 3 behaviour inside the Antarctic polar vortex from 2002-2011, observed by three independent satellite based instruments ENVISAT/MIPAS, Odin/SMR, and TIMED/SABER.These O 3 vmr measurements, based on 26 day running means from 1 April-1 November covering altitudes from 20-70 km, were individually grouped into high and low index activity according to the 26 day averages centred around 1 April, 1 May, and 1 June of different solar and geomagnetic indices (F10.7,Ap, 2 MeV).After minimising the direct influence of the solar radiation by only consid-Discussion Paper | Discussion Paper | Discussion Paper | Screen / Esc Printer-friendly Version Interactive Discussion Discussion Paper | Discussion Paper | Discussion Paper | Discussion Paper | funded jointly by the Swedish National Space Board (SNSB), the Canadian Space Agency (CSA), the National Technology Agency of Finland (Tekes), the Centre National d'Etudes Spatiales (CNES) in France and the third party mission program of the European Space Agency (ESA).We further like to thank the ERA-Interim for free provision of data and related support.Discussion Paper | Discussion Paper | Discussion Paper | ergy Particle Precipitation in the Atmosphere (HEPPA) model versus MIPAS data intercom-

Figure 1 .Figure 2 .Figure 7 .
Figure 1.Potential vorticity (10 −6 K m 2 s −1 kg −1 , colour scale) at ∼ 40 km during the Antarctic winter 2011 as a function of time and equivalent latitude.The thresholds of the regions OUT-SIDE (dotted line), EDGE (solid line) and CORE (dashed line) are included.Potential vorticity was calculated from ECMWF Era-Interim data.