The Road to Recovery: Is the Ozone Layer Finally Healing?

Image of the earth and the highlighted region of the Antarctic region

Editor's Introduction

Emergence of healing in the Antarctic ozone layer

annotated by

What happens when humans across the globe unite to save the Earth? More than 30 years ago, the world took action to heal the hole in the Antarctic ozone layer. The Montreal Protocol phased out the use of chemicals responsible for the hole, but, after all these years, are there any signs that the hole is actually closing? And if so, is this a response to human action? Or can it be explained by natural causes? Scientists use observational data and simulations to determine whether our collective action to save the ozone layer is finally paying off.

Paper Details

Original title
Emergence of healing in the Antarctic ozone layer
Original publication date
Vol. 353, Issue 6296, pp. 269-274
Issue name


Industrial chlorofluorocarbons that cause ozone depletion have been phased out under the Montreal Protocol. A chemically driven increase in polar ozone (or “healing”) is expected in response to this historic agreement. Observations and model calculations together indicate that healing of the Antarctic ozone layer has now begun to occur during the month of September. Fingerprints of September healing since 2000 include (i) increases in ozone column amounts, (ii) changes in the vertical profile of ozone concentration, and (iii) decreases in the areal extent of the ozone hole. Along with chemistry, dynamical and temperature changes have contributed to the healing but could represent feedbacks to chemistry. Volcanic eruptions have episodically interfered with healing, particularly during 2015, when a record October ozone hole occurred after the Calbuco eruption.


Antarctic ozone depletion has been a focus of attention by scientists, policy-makers, and the public for three decades (1). The Antarctic ozone hole opens up in austral spring of each year and is measured both by its depth (typically a loss of about half of the total integrated column amount) and its extent (often more than 20 million km2 by October). Ozone losses have also been documented in the Arctic and at mid-latitudes in both hemispheres (2). Concern about ozone depletion prompted a worldwide phaseout of the production of anthropogenic halocarbons containing chlorine and bromine, which are known to be the primary sources of reactive halogens responsible for the depletion (2). The ozone layer is expected to recover in response, albeit very slowly, mainly because of the long atmospheric residence time of the halocarbons (2).

Ozone recovery involves multiple stages, starting with (i) a reduced rate of decline, followed by (ii) a leveling off of the depletion and (iii) an identifiable ozone increase that can be linked to halocarbon reductions (23). For simplicity, we refer to the third stage of recovery as “healing.” All three stages of recovery have been documented in the upper stratosphere in mid- and low latitudes, albeit with uncertainties (246). Some studies provide evidence for all three recovery stages in ozone columns at mid-latitudes, despite dynamical variability (7). Although the first and second stages of recovery have also been well documented in the Arctic and Antarctica (810), a recent scientific assessment concluded that the emergence of the third stage had not been established by previous studies of the polar regions (2). Further, in October of 2015, the Antarctic ozone hole reached a record size (11), heightening questions about whether any signs of healing can be identified in either polar region.

Controls on polar ozone

Polar ozone depletion is driven by chlorine and bromine chemistry linked to anthropogenic halocarbon emissions (212). But ozone is not expected to heal in a monotonic fashion as halocarbon concentrations decrease because of confounding factors (such as meteorological changes) that induce variability from one year to another and could influence trends (21314).

The exceptionally large ozone depletion in the polar regions compared with lower latitudes is related to polar stratospheric cloud (PSC) particles that form under cold conditions. These clouds drive heterogeneous chlorine and bromine chemistry that is sensitive to small changes in temperature (and hence to meteorological variability). A second related factor is change in the transport of ozone and other chemicals caused by circulation or mixing changes (2). Further, some PSCs, as well as aerosol particles capable of driving similar chemistry, are increased in abundance when volcanic eruptions increase stratospheric sulfur. Volcanically driven increases in Antarctic ozone depletion were documented in the early 1990s after the 1991 eruption of Mount Pinatubo and are well simulated by models (1516). Since about 2005, a series of smaller-magnitude volcanic eruptions has increased stratospheric particle abundances (1718), but the impact of these on polar ozone recovery has not previously been estimated.

Observations and model test cases

We examined healing using balloon ozone data from the Syowa and South Pole stations. We also used total ozone column measurements from the South Pole station and the Solar Backscatter Ultra-Violet satellite (SBUV; we averaged SBUV data over the region from 63°S to the polar edge of coverage). The SBUV record has been carefully calibrated and compared with suborbital data (19). We also used the Total Ozone Mapping Spectrometer/Ozone Monitoring Instrument (TOMS/OMI) merged data set for analysis of the horizontal area of the ozone hole (20). Calibrated SBUV data are currently only available up to 2014, whereas the other records are available through 2015 (affecting the time intervals evaluated here). Model calculations were carried out with the Community Earth System Model 1 (CESM1) Whole Atmosphere Community Climate Model (WACCM), which is a fully coupled state-of-the-art interactive chemistry climate model (21). We used the specified dynamics option, SD-WACCM, in which meteorological fields including temperature and winds are derived from observations (2223). The analysis fields allow the time-varying temperature-dependent chemistry that is important in polar ozone depletion to be simulated in detail. The model’s ability to accurately represent polar ozone chemistry has recently been documented (2324). Aerosol properties were based on the Chemistry and Climate Model Intercomparison (CCMI) recommendation (25) or derived inline from a version of WACCM that uses a modal aerosol submodel (2326). The modal submodel calculates variations in stratospheric aerosols from volcanic sources (using an observational database of volcanic SO2 emissions and plume altitudes; table S1) and nonvolcanic sulfur sources (particularly OCS, anthropogenic SO2, and dimethyl sulfide). The injection heights and volcanic inputs are similar to those of previous studies (1827), and the calculated aerosol distributions capture the timing of post-2005 eruptions observed in several low-, mid-, and high-latitude lidar data sets and satellite climatologies (26). Based on comparisons with lidar data for several eruptions and regions (26), our modeled post-2005 total stratospheric volcanic aerosol optical depths are estimated to be accurate to within ±40% (supplementary materials). Differences between the CCMI aerosol climatology and our calculated modal aerosol submodel results can be large, especially in the lower stratosphere (26), and can affect ozone abundances.

The concentrations of halogenated gases capable of depleting ozone stopped rising in the polar stratosphere around the late 1990s as a result of the Montreal Protocol and are slowly declining (228). We analyze what role these decreases in halogens play, along with other drivers of variability and change, in polar ozone trends since 2000. The year 2002 was anomalous in terms of meteorological behavior in the Antarctic (29), and it is excluded from all trend analyses throughout this paper.

Three different model simulations, all using full chlorine and bromine chemistry, were used to examine drivers of polar ozone changes since 2000: (i) a simulation encompassing observed time-varying changes in temperature and winds from meteorological analyses, with calculated background and volcanic stratospheric particles as well as other types of PSCs (chem-dyn-vol); (ii) a volcanically clean simulation (vol-clean), considering only background sources of stratospheric sulfur; and (iii) a chemistry-only simulation, in which annual changes in all meteorological factors (including the temperatures that drive chemistry) were suppressed by repeating conditions for 1999 throughout, and volcanically clean aerosols were imposed (chem-only). The Antarctic stratosphere in austral spring of 1999 was relatively cold and was deliberately chosen for the third simulation for its large chemical ozone losses. A longer run using full chemistry and CCMI aerosols illustrates the model’s simulation of ozone loss since 1979. Further information on statistical approaches, methods, data sets, and the model are provided in the supplementary materials.

Our chem-only simulation probably represents a conservative estimate of chemical effects because it does not include radiatively driven temperature changes that are expected to occur as a result of changes in ozone (30) or the feedbacks of those temperature changes to chemical processes. Temperature and ozone are coupled because absorption of sunlight by ozone heats the stratosphere. If ozone increases as a result of reductions in halogens, then temperatures will increase, which feeds back to the chemistry (for example, by reducing the rate of temperature-dependent heterogeneous reactions that deplete ozone), further increasing ozone. Such effects have not been separated here from other changes in temperature or winds (due to dynamical variability or forcings such as greenhouse gases).

Antarctic ozone trends, variability, and fingerprints of healing

Most analyses of Antarctic ozone recovery to date consider October or September-to-November averages (7910). The historic discovery of the Antarctic ozone hole was based on observations taken in October (1), and healing cannot be considered complete until the ozone hole ceases to occur in that month, which is expected around mid-century (228). However, October need not be the month when the onset of the healing process occurs. A first step in understanding whether a signal of the onset of healing can be identified is examining trends and their statistical significance relative to the noise of interannual variability.

October has the deepest ozone depletion of any month in the Antarctic. However, it is subject to large variability due to seasonal fluctuations in temperature and transport, as well as to volcanic aerosol chemistry. Figure 1shows the time series of measured Antarctic total ozone in October obtained from SBUV and South Pole station data, along with the model calculations; tables S2 and S3 provide the associated post-2000 trends and 90% confidence intervals. SD-WACCM reproduces the observed October variability from year to year when all factors are considered (chem-dyn-vol) (Fig. 1). However, the October total ozone trends are not yet positive with 90% certainty in the observational data or in the model. In contrast, other months with lower depletion and variability (particularly September; Fig. 1, fig. S1, and tables S2 and S3) reveal positive ozone trends from 2000 to 2014 that are statistically significant at 90% confidence in SBUV and South Pole station measurements. Arctic ozone has long been known to be more variable than Antarctic ozone (2), and no Arctic month yet reveals a significant positive trend in either the chem-dyn-vol simulation or the SBUV observations when examined in the same manner (table S2).

Figure 1

Fig. 1. Monthly averaged Antarctic total ozone column for October and September, from SBUV and South Pole station observations and a series of model calculations. Total ozone data measured at the geographic South Pole are from Dobson observations (filled circles) for October (Top) and balloon sondes (open circles) for September (Bottom), when there is not sufficient sunlight for the Dobson. SBUV data for each month are compared with model runs averaged over the polar cap latitude band that is accessible by the instrument; South Pole station data are compared with simulations for 85°S to 90°S.

Dobson Units (DU)

A Dobson Unit (DU) is a standard unit for measuring the amount of atmospheric ozone. A DU is equivalent to the amount of pure ozone that could be squeezed into a 0.01-mm-thick layer at 1 atmosphere of pressure and 0 degrees Celsius. On average, the atmosphere has 300 DUs of ozone.

Note that the "Dobson Unit" or "DU" is a standard unit of total ozone amount regardless of which instrument was used for the measurement.

Read more here at

Dobson Observations

The South Pole Dobson observations (represented by filled circles) were measured using a Dobson Ozone Spectrophotometer. Since the ozone layer prevents certain types of ultraviolet (UV) radiation from reaching Earth's surface, this instrument measures the amount and type of UV radiation on the ground to determine the abundance of atmospheric ozone.

Read more here at

See video below. 

September vs October

Total ozone column amounts are less variable in September, which makes that month better suited for tracking trends in ozone over the years.

Dobson Units (DU)

Why do the "Chem-Only" simulated data points show less variation than the other simulation data?


The "Chem-Only" simulation only accounts for chemistry in the atmosphere and does not include variations due to volcanic aerosols or variations in atmospheric temperature.

The September profile of balloon ozone trends is a key test of process understanding. Figure 2 shows measured balloon profile trends for the South Pole and Syowa stations for 2000–2015, together with SD-WACCM model simulations. The large ozone losses measured at Syowa as the ozone hole developed from 1980 to 2000 are also shown for comparison. Antarctic station data need to be interpreted with caution because of an observed long-term shift in the position of the Antarctic vortex that affects Syowa in particular in October; the South Pole station is, however, less influenced by this effect (31). The ozonesonde data sets suggest clear increases since 2000 between about 100 and 50 hPa (10). The chem-only simulation reproduces about half of the observed healing, with the remainder in this month being accounted for by dynamics and temperature. The simulations also suggest a negative contribution (offset to healing) due to volcanic enhancements of the ozone depletion chemistry between about 70 and 200 hPa (fig. S2 shows similar effects in other months in this sensitive height range). The comparisons of the modeled trend profiles in Fig. 2 provide an important fingerprint of the onset of healing of the Antarctic ozone layer in September. This is consistent with the basic understanding that reductions in ozone-depleting substances in the troposphere will lead to a healing of polar ozone that emerges over time, with lags due to the transport time from the troposphere to the stratosphere, along with the time required for chemically driven trends to become significant relative to dynamical and volcanic variability.

Two vertical profile graphs showing trends in the Southern Hemisphere polar cap ozone.

Fig. 2. Trends in Southern Hemisphere (SH) polar cap ozone profiles in September. Ozone data from balloons at the Syowa (69°S, 39.58°E) (Left) and South Pole (Right) stations, along with model simulations averaged over the polar cap and over 85°S to 90°S, respectively, are shown versus pressure. The shading represents the uncertainties on the trends at the 90% statistical confidence interval.

90% Confidence Intervals

The confidence interval indicates that there is a 90% probability that the true value lies within the specified range of values. A larger interval shows that there is more uncertainty associated with the data.

Unit of Pressure

A pascal (Pa) is a unit of pressure in which 101,325 Pa corresponds to Earth's atmospheric pressure at sea level.  The prefix hecto (h) means 100. Thus, one hectopascal (hPa) equals 100 pascals (Pa).

Pressure with altitude

In these plots, lower pressure corresponds to a higher altitude above Earth's surface.

Ozone Trends vs. Time

A negative value on the horizontal axis means ozone is decreasing with time, and a positive value means it is increasing with time. In the left panel, the negative 1980-2000 trend becomes positive from 2000-2015. 

The seasonal cycle of monthly total ozone trends from the SBUV satellite observations is shown in Fig. 3, along with model calculations for various cases. The contributions to the modeled trends that are due to volcanic inputs (difference between chem-dyn-vol and vol-clean simulations), chemistry alone (chem-only simulations), and dynamics and temperature (difference between vol-clean and chem-only simulations) are shown in the lower panel. Although it is not possible to be certain that the SBUV observations vary for the same reasons that the model calculations do, the broad agreement between them on the seasonal cycle of total trends supports this interpretation. Less dynamical variability in September compared with October (as shown by smaller error bars on the “dynamics/temperature” term in Fig. 3, bottom panel), along with strong chemical recovery, make September the month when the Antarctic ozone layer has undergone the largest amount of healing since 2000. The data suggest September increases (at 90% confidence) of 2.5 ± 1.6 DU per year over the latitudes sampled by SBUV and 2.5 ± 1.5 DU per year from the South Pole sondes. These values are consistent with the chem-dyn-vol model values of 2.8 ± 1.6 and 1.9 ± 1.5 DU per year, respectively. Because the model reproduces much of the observed year-to-year variability in September total ozone from both the South Pole station and SBUV observations, confidence is increased that there is a significant chemical contribution to the trends (Fig. 1). As a best estimate, the model results suggest that roughly half of the September column healing is chemical, and half is due to dynamics and temperature, though the dynamics and temperature effects are highly variable. The modeled total September healing trend has been reduced by about 10% as a result of the chemical effects of increased volcanic activity in the latter part of 2000–2014.

Figure 3 shows a total ozone abundance by month in bar graph form.

Fig. 3. Trends in total ozone abundance (TOZ) by month from 2000 to 2014. (Top) Monthly and polar cap–averaged SBUV satellite observations, together with model simulations masked to the satellite coverage. Error bars denote 90% statistical confidence intervals. (Bottom) Contributions to the simulated monthly trends in total ozone abundance driven by dynamics and temperature (vol-clean minus chem-only), chemistry only (chem-only), and volcanoes (chem-dyn-vol minus vol-clean). In austral winter, SBUV measurements do not extend to 63°S; therefore, the model averages for those months cover 63°S to 90°S (open bars).

Top Panel

The average monthly ozone trends are positive (increasing over time) for all months, but the 90% confidence intervals extend to negative values for some months.  This indicates that there is more statistical uncertainty associated with the positive ozone trends in those months. However, the confidence intervals only include positive values in September, and this shows that there is a 90% probability that the total September ozone is increasing.

Bottom Panel

Notice that the error bars are largest for dynamics and temperature, indicating that they contribute the most to the statistical uncertainty. To the contrary, the error bars are the smallest for the chemistry component of the simulation, adding more statistical certainty to the trend of increasing ozone with time. 

Ozone Depletion Chemistry

See this animation of ozone depletion due to chemicals in the atmosphere: 

Map of Ozone-Depleting Chemical 

See this movie which maps the concentration of an ozone-depleting chemical, ClO, over the Antarctic from August to October of 2004:   

Volcanic eruptions affect polar ozone depletion because injections of sulfur increase the surface areas of liquid PSCs and aerosol particles (32). Higher-latitude eruptions directly influence the polar stratosphere, but tropical eruptions also can increase polar aerosols via transport. The model indicates that numerous moderate eruptions since about 2005 have affected polar ozone in both hemispheres (table S1 gives eruptions, dates, and latitudes), particularly at pressures from about 70 to 300 hPa (Fig. 4). At pressures above about 100 hPa, temperatures are generally too warm for many PSCs to form, but there is sufficient water that effective heterogeneous chemistry can take place under cold polar conditions (12). Our simulations indicate peak volcanic losses locally as large as 30 and 55% for the Antarctic in 2011 and 2015, mainly due to the Chilean eruptions of Puyehue-Cordón Caulle and Calbuco, respectively; contributions to depletions that are attributable to tropical eruptions are also evident in several earlier years. At these pressures, contributions to the total column are small but significant: The integrated additional Antarctic ozone column losses, averaged over the polar cap, are between 5 and 13 DU after the eruptions shown in Fig. 4.

Figure 4 Model-calculated percentage changes in local concentrations of ozone due to a series of moderate volcanic eruptions over the last 18 years.

Fig. 4. Model-calculated percentage changes in local concentrations of ozone due to a series of moderate volcanic eruptions. The results (chem-dyn-vol minus vol-clean simulations) are averaged over the Antarctic polar cap as a function of pressure and month. Volcanic eruptions that have dominated the changes are indicated, with tropical eruptions at the bottom and higher-latitude eruptions at the top. An, Anatahan; Ca, Calbuco; Ch, Chaiten; Ke, Kelut; Ll, Llaima; Ma, Manam; Me, Merapi; Na, Nabro; NS, Negra Sierra; PC, Puyehue-Cordón Caulle; PF, Piton de la Fournaise; Ra, Rabaul (also referred to as Tavurvur); Ru, Ruang; Rv, Reventador; SA, Sangeang Api; SH, Soufriere Hills.


The higher-latitude eruptions (listed at the top) are closer to Earth's polar regions. While the volcanic eruptions occurred at various latitudes, the simulations represent the impact of these eruptions on the Antarctic region (63-90 degrees south).

The Calbuco Eruption

The 2015 eruption in Calbuco, Chile, had the largest impact on ozone concentrations over the 2000 to 2015 time period. This is indicated by the darker coloring in the plot. 


In 2011, volcanic eruptions occurred at Nabro (Na), Eritrea, and at Puyehue-Cordón Caulle (PC), Chile. Which eruption is driving the 2011 volcanic-induced Antarctic ozone reduction?


The 2011 volcanic-induced ozone reduction was primarily due to the higher-latitude eruption at Puyehue-Cordón Caulle (PC), Chile.  

The ozone hole typically begins to open in August of each year and reaches its maximum areal extent in October. Decreases in the areal extent of the October hole are expected to occur in the 21st century as chemical destruction slows, but they cannot yet be observed against the backdrop of interannual variability, in part because of the extremely large hole in 2015 (fig. S3). However, monthly averaged observations for September show a shrinkage of 4.5 ± 4.1 million km2 between 2000 and 2015 (Fig. 5, left panel). The model underestimates the observed September hole size by about 15% on average, but it yields variability (Fig. 5) and trends (4.9 ± 4.7 million km2) that are similar to the observations. The right panel of Fig. 5 shows that the observed and modeled day of the year when the ozone hole exceeds a threshold value of 12 million km2 has been occurring later in recent years, indicating that early September holes are becoming smaller (Fig. 6). This result is robust to the specific choice of threshold value and implies that the hole is opening more slowly as the ozone layer heals. The chem-only simulation results in Fig. 5show that if temperatures, dynamical conditions, and volcanic inputs had remained the same as they were in 1999 until now, the September ozone hole would have shrunk by about 3.5 ± 0.3 million km2 as a result of reduced chlorine and bromine; thus, the reduction of these chemicals dominates the total shrinkage over this period.

Figure 5 has two line graphs. The graph on the left just shows trends in September, whereas the line graph on the right shows annual days that the ozone hole exceeds a specific limit.

Fig. 5. September size of the ozone hole and day of year when the hole exceeds 12 million km2. (Left) Annual size of the September monthly averaged ozone hole, (defined as the region where the total ozone amount is less than 220 DU,) from TOMS/OMI satellite observations and model simulations. Trends in the TOMS/OMI observations (heavy dashed black line) and the chem-dyn-vol model calculations (heavy dashed red line) from 2000 to 2015 are also indicated. (Right) Annual day of the year when the size of the ozone hole exceeds 12 million km2 (and remains above that value for at least 3 days) in the TOMS/OMI observations and model simulations.

Left Panel

The 2000 to 2015 data show that the ozone hole area is still much larger compared to 1980. However, the trend shows that the hole has started to shrink since 2000. The chemistry-only (chem-only) model shows that the reduction in ozone-depleting substances is driving this shrinkage.

Right Panel

The ozone hole reached the 12 million square km threshold later in the year from 2000 to 2015. This delay in reaching the threshold is a sign of ozone hole healing.  The chemistry-only (chem-only) simulation shows that the reduction in ozone-depleting substances is driving this trend.  

September Ozone Over the Years

View this video which maps the September Antarctic ozone hole from 1979 to 2020 at

October Ozone Over the Years

View this video which maps the October Antarctic ozone hole from 1979 to 2020 at  

Figure 6 three line graphs displaying daily size of the ozone hole.

Fig. 6. Daily size of the ozone hole. Daily measurements (Top) and model calculations (Middle and Bottom) of the size of the Antarctic ozone hole versus day of year for different time intervals, with 2015 shown in black. The dashed black line in the top panel denotes the 2015 TOMS/OMI data after the period covered by the model runs.

Top Panel

The large growth in the average size of the ozone hole from the 1979-1988 period to the 1989-1998 period shows the effects of human-made chemicals. Once those chemical levels began to decline, the average ozone hole stopped growing in size over the 2009-2014 period.

Middle Panel

The simulation which includes chemistry, temperature/dynamic, and volcanic effects shows that the opening of the ozone hole occurs later in the year. It also reproduces the extraordinarily large holes in 2011 and 2015. This indicates that the volcanic eruptions in 2011 and 2015 likely produced the unusually large holes observed in those years.

Bottom Panel

The chemistry-only simulation shows that the ozone hole would have been steadily shrinking from 2000 to 2015 if the volcanic eruptions and temperature variations had not occurred.

Volcanic eruptions caused the modeled areas of the September-averaged ozone holes to expand substantially in several recent years. Our results, as shown in Fig. 5 (left panel), indicate that much of the statistical uncertainty in the observed September trend is not random, but rather is due to the expected chemical impacts of these geophysical events. In 2006, 2007, and 2008, model calculations suggest that the September ozone holes were volcanically enlarged by about 1 million km2. The sizes of the September ozone holes in 2011 and 2015 are estimated to have been, respectively, about 1.0 million and 4.4 million km2 larger because of volcanic eruptions (especially Puyehue-Cordón Caulle in 2011 and Calbuco in 2015) than they would otherwise have been, substantially offsetting the chemical healing in those years.

Figure 6 shows that the bulk of the seasonal growth of the ozone hole typically occurs between about days 230 and 250 (late August to early September). As the ozone layer heals, the growth of the hole is expected to occur later in the year (middle and bottom panels), in agreement with observations (top). The slower rates of early-season growth are key to the trend of shrinkage in the September-averaged ozone hole. For example, the rate of ozone loss depends strongly upon the ClO concentration, so that reduced chlorine concentrations lead to slower rates of ozone loss after polar sunrise. The ozone hole of 2015 was considerably larger over several weeks in October (but notably, not in September) than ever previously observed, and this behavior is well reproduced in our model only when the eruption of Calbuco is considered (figs. S3 and S4). The record-large monthly averaged ozone hole in October 2015 measured 25.3 million km2, which is 4.8 million km2 larger than the previous record year (20.6 million km2 in 2011). When volcanic aerosols are included (chem-dyn-vol simulation), our calculated monthly averaged October 2015 ozone hole is 24.6 million km2, whereas the corresponding value excluding volcanic aerosols (vol-clean simulation) is much smaller, 21.1 million km2 (fig. S3). Therefore, our calculations indicate that cold temperatures and dynamics alone made a much smaller contribution to establishing the October 2015 record than volcanic aerosols did (figs. S3 and S4), and the cold temperatures are expected to be at least partly a feedback to the volcanically increased large ozone losses. Further, the conclusion that the volcanic aerosols were the dominant cause of the record size of the October 2015 ozone hole would hold based on our calculations even if the volcanic aerosol amounts were overestimated by a factor of several (a much larger error than indicated by our comparison of our model calculations with lidar data for multiple eruptions in (26); supplementary materials).

The reasons for the contributions of dynamics and temperature to the healing of the Antarctic ozone layer are not clear. The dynamical and temperature contributions to healing estimated in Fig. 3 vary by month in a manner that mirrors the ozone depletion in spring, suggesting linkages to the seasonality of the depletion itself and hence possible dynamical feedbacks. Some models (3335) suggest that a reduction in transport of ozone to the Antarctic occurred as depletion developed in the 1980s and 1990s, which would imply a reversal of this process and hence increased healing as ozone rebounds. But others indicate that ozone depletion increased the strength of the stratospheric overturning circulation (36), and a reversal of this factor during recovery would impede healing. Although there is robust agreement across models that climate change linked to increasing greenhouse gases should act to increase the strength of the stratospheric overturning circulation, observations show mixed results (37); further, the seasonality of this effect has not been established, and the magnitude in the Antarctic is uncertain. Internal variability of the climate system linked, for example, to variations in El Niño could also affect the trends.


After accounting for dynamics, temperature, and volcanic factors, the results presented here indicate that healing of the Antarctic ozone hole is emerging. Our results underscore the combined value of balloon and satellite ozone data, volcanic aerosol measurements, and chemistry-climate models in documenting progress in the recovery of the ozone layer since the Montreal Protocol.


Materials and Methods

Figs. S1 to S4

Tables S1 to S3

References (3844)


1. J. C. Farman, B. G. Gardiner, J. D. Shanklin, Nature 315, 207–210 (1985).

2. World Meteorological Organization/United Nations Environment Programme (WMO/UNEP), Scientific Assessment of Ozone Depletion: 2014 (Global Ozone Research and Monitoring Project Report No. 55, WMO, 2014).

3. D. J. Hofmann, S. J. Oltmans, J. M. Harris, B. J. Johnson, J. A. Lathrop, J. Geophys. Res. 102, 8931–8943 (1997).

4. M. J. Newchurch et al., J. Geophys. Res. 108, 4507 (2003).

5. N. R. P. Harris et al., Atmos. Chem. Phys. 15, 9965–9982 (2015).

6. F. Tummon et al., Atmos. Chem. Phys. 15, 3021–3043 (2015).

7. T. G. Shepherd et al., Nat. Geosci. 7, 443–449 (2014).

8. E.-S. Yang et al., J. Geophys. Res. 113, D20308 (2008).

9. M. L. Salby, E. Titova, L. Deschamps, Geophys. Res. Lett. 38, L09702 (2011).

10. J. Kuttippurath et al., Atmos. Chem. Phys. 13, 1625–1635 (2013).

11. WMO, “WMO Antarctic Ozone Bulletins: 2015,” 2015;

12. S. Solomon, Rev. Geophys. 37, 275–316 (1999).

13. J. Kuttippurath et al., Atmos. Chem. Phys. 15, 10385–10397 (2015).

14. N. J. Livesey, M. L. Santee, G. L. Manney, Atmos. Chem. Phys.15, 9945–9963 (2015).

15. D. J. Hofmann, S. J. Oltmans,  J. Geophys. Res. 98, 18555–18561 (1993).

16. R. W. Portmann et al., J. Geophys. Res. 101, 22991–23006 (1996).

17. J.-P. Vernier et al., Geophys. Res. Lett. 38, L12807 (2011).

18. C. Brühl, J. Lelieveld, H. Tost, M. Höpfner, N. Glatthor, J. Geophys. Res. Atmos. 120, 2103–2118 (2015).

19. R. D. McPeters, P. K. Bhartia, D. Haffner, G. L. Labow, L. Flynn, J. Geophys. Res. 118, 8032–8039 (2013).

20. W. Chehade, M. Weber, J. P. Burrows, Atmos. Chem. Phys. 14, 7059–7074 (2014).

21. D. R. Marsh et al., J. Clim. 26, 7372–7391 (2013).

22. A. Kunz, L. L. Pan, P. Konopka, D. E. Kinnison, S. Tilmes, J. Geophys. Res. 116, D24302 (2011).

23. Materials and methods are available as supplementary materials on Science Online.

24. S. Solomon, D. Kinnison, J. Bandoro, R. R. Garcia, J. Geophys. Res. 120, 7958–7974 (2015).

25. F. Arfeuille et al., Atmos. Chem. Phys. 13, 11221–11234 (2013).

26. M. J. Mills et al., J. Geophys. Res. 121, 2332–2348 (2016).

27. M. Höpfner et al., Atmos. Chem. Phys. 15, 7017–7037 (2015).

28. P. A. Newman, E. R. Nash, S. R. Kawa, S. A. Montzka, S. M. Schauffler, Geophys. Res. Lett. 33, L12814 (2006).

29. A. A. Scaife et al., J. Atmos. Sci. 62, 629– 639 (2005).

30. P. M. Forster, R. S. Freckleton, K. P. Shine, Clim. Dyn. 13, 547–560 (1997).

31. B. Hassler, G. E. Bodeker, S. Solomon, P. J. Young, Geophys. Res. Lett. 38, L01805 (2011).

32. A. Tabazadeh, K. Drdla, M. R. Schoeberl, P. Hamill, O. B. Toon, Proc. Natl. Acad. Sci. U.S.A. 99, 2609–2612 (2002).

33. S. Meul, S. Oberländer-Hayn, J. Abalichin, U. Langematz, Atmos. Chem. Phys. 15, 6897–6911 (2015). 

34. P. Braesicke et al., Atmos. Chem. Phys. 13, 10677–10688 (2013).

35. F. Li, J. Austin, J. Wilson, J. Clim. 21,40–57 (2008).

36. C. McLandress, T. G. Shepherd, J. Clim. 22, 1516–1540 (2009).

37. N. Butchart, Rev. Geophys. 52, 157–184 (2014).


We thank S. Tilmes (NCAR) for help with the MERRA (Modern-Era Retrospective Analysis for Research and Applications) data. D.K. and S.S. were partially supported by NSF Frontiers in Earth System Dynamics grant OCE-1338814, and D.J.I. was supported by NSF Atmospheric Chemistry grant AGS-1539972. A.S. was supported by an Academic Research Fellowship from the University of Leeds, an NCAR visiting scientist grant, and Natural Environment Research Council grant NE/N006038/1. NCAR is sponsored by NSF. WACCM is a component of CESM, which is supported by NSF and the Office of Science of the U.S. Department of Energy. We are grateful to D. Fahey, B. Hassler, W. D. McKenna, and the anonymous reviewers for helpful comments. Instructions for access to data reported in this paper are given in the supplementary materials.