Stratospheric effects of energetic particle precipitation in 2003–2004

Authors


Abstract

[1] Upper stratospheric enhancements in NOx (NO and NO2) were observed at high northern latitudes from March through at least July of 2004. Multi-satellite data analysis is used to examine the temporal evolution of the enhancements, to place them in historical context, and to investigate their origin. The enhancements were a factor of 4 higher than nominal at some locations, and are unprecedented in the northern hemisphere since at least 1985. They were accompanied by reductions in O3 of more than 60% in some cases. The analysis suggests that energetic particle precipitation led to substantial NOx production in the upper atmosphere beginning with the remarkable solar storms in late October 2003 and possibly persisting through January. Downward transport of the excess NOx, facilitated by unique meteorological conditions in 2004 that led to an unusually strong upper stratospheric vortex from late January through March, caused the enhancements.

1. Introduction

[2] Through dissociation and ionization processes, energetic particle precipitation (EPP) leads to routine production of odd nitrogen in the mesosphere and thermosphere, and to sporadic production in the stratosphere when very highly energetic particles are involved. EPP also indirectly affects the stratosphere via descent of EPP-produced mesospheric NOx (NO + NO2) to the stratosphere during polar winter and spring, where it plays a major role in ozone chemistry. EPP coupling of the upper and lower atmosphere was first examined more than two decades ago [Solomon et al., 1982], and observational evidence for its occurrence is prevalent [e.g., Russell et al., 1984; Jackman et al., 1995; Rinsland et al., 1996; Randall et al., 1998, 2001a; Siskind et al., 2000; Callis et al., 2001; Natarajan et al., 2004 (hereinafter referred to as N04)]. EPP occurs throughout the polar night, but the stratospheric response depends strongly on the energy and number of precipitating particles (i.e., the altitude and intensity of the source), and on the efficiency of vertical transport across the stratopause.

[3] In Nov and Dec 2003, enhancements in northern hemisphere (NH) upper stratospheric HNO3 and NO2 were measured by the MIPAS (Michelson Interferometer for Passive Atmospheric Sounding) instrument [Orsolini et al., 2005] (hereinafter referred to as O05), and enhancements in NO2 were measured by the GOMOS (Global Ozone Monitoring by Occultation of Stars) instrument [Seppälä et al., 2004]. These authors attributed the enhancements to NOx produced by EPP during the unusually powerful solar storms and associated solar proton events (SPEs) of Oct–Nov 2003 (see special section on Violent Sun-Earth Connection Events of October–November 2003, Geophysical Research Letters, 32, 3, 2005). In Apr 2004, unprecedented enhancements in NH upper stratospheric NOx, accompanied by significant reductions in ozone, were observed by the Halogen Occultation Experiment (HALOE). The enhancements were tentatively ascribed to indirect effects (mesospheric production followed by descent) of the Oct–Nov solar storms (N04). In this paper we describe measurements from numerous satellite instruments to provide a more comprehensive picture of EPP effects in 2003–2004 on the stratosphere. Included are data from the POAM (Polar Ozone and Aerosol Measurement) II & III, SAGE (Stratospheric Aerosol and Gas Experiment) II & III, HALOE, MIPAS, and OSIRIS (Optical Spectrograph and InfraRed Imager System) instruments. We examine the time dependence of NO, NO2, and O3 from Nov 2003 through Jul 2004, place the observations in historical context, and investigate the origin of observed NOx enhancements.

2. Stratospheric NOx Enhancements and O3 Reductions in 2003–2004

[4] Figure 1 compares 2004 measurements of NO2 (or NOx in the case of HALOE) and O3 at 40 km to data in previous years from four solar occultation instruments: HALOE (1991–present), SAGE II (1984–present) and POAM II & III (1994–1996 and 1998–present). Because of their mid-inclination orbits, the HALOE and SAGE II measurement latitudes vary rapidly in time, generally reaching polar latitudes for several days each month, but at different times each year (see Randall et al. [2001b] for representative latitude sampling of HALOE and SAGE II). Thus every individual NH measurement with error less than 30% is depicted, including local sunrise (SR) and sunset (SS) data. POAM measurement latitudes repeat annually, varying only slowly in time between 54° and 71° in the NH, so 7-day running averages are shown; only local SS measurements are acquired by POAM in the NH. NOx (or NO2) enhancements and O3 reductions in Apr 2004 are unmistakable in these data sets: NOx mixing ratios are up to a factor of 4 higher than ever observed previously, and O3 is reduced by more than 60% in some cases. Further analysis (not shown) reveals that the anomalies are confined to latitudes poleward of ∼40°N, and that enhancements of 10–50% persist through July (the last month of the analysis) in all three data sets above 40 km. N04 show the photochemical consistency of the NOx enhancements and O3 reductions in Apr HALOE data. Figure 1 gives a more complete picture of the time dependence and places the observations into the context of measurements dating back to 1984.

Figure 1.

Mixing ratios at 40 km for (top left) HALOE NOx, (top middle) SAGE II NO2, (top right) POAM NO2 and (bottom) O3 for the respective instruments. POAM III NO2 has been scaled as described by Randall et al. [2001a]. Tick marks on the horizontal axis denote the first day of each month.

[5] The polar-orbiting MIPAS instrument senses infrared emission, and is thus capable of measuring atmospheric constituents globally during night and day. Figure 2 shows MIPAS NO2 and CH4 data plotted as a function of equivalent latitude (EqLat, the latitude that would enclose the same area between it and the pole as a given potential vorticity (PV) contour) and potential temperature, for several 4-day periods in Mar 2004 (MIPAS has not been operating since late Mar 2004). NO2 mixing ratios typically decrease with increasing altitude and EqLat in the upper stratosphere, due to less production from N2O oxidation, destruction by atomic nitrogen, and descending NOx-poor air. In 2004, however, NO2 enhancements above 40 km appear in early Mar at high EqLat, reaching values of over 150 ppbv by mid-Mar before declining slightly in late Mar. Corresponding CH4 plots indicate that the NO2 enhancements occur in air that descends slowly throughout Mar; CH4 mixing ratios of 0.1–0.2 ppmv signify air of mesospheric origin, consistent with the Apr enhancements shown by N04.

Figure 2.

Potential temperature/EqLat plots of MIPAS NO2 (top, solar zenith angle (SZA) > 95°) and CH4 (bottom) in 2004 for the dates shown in each column. These are similar to zonal mean contour plots but use the vortex-centered EqLat coordinate system. Contour increments are 10 ppbv for NO2 and 0.08 ppmv for CH4; white indicates missing data. The vortex edge is at ∼60° EqLat.

[6] The geographic distribution of nighttime MIPAS NO2 for 24–26 Mar at 1640 K (∼43 km) is shown in Figure 3, and reveals enhanced NO2 nearly filling the vortex. The decline in NO2 near the pole is still under investigation. The polar-orbiting OSIRIS instrument senses scattered light with near-global, daytime coverage, when diurnally-varying NO2 mixing ratios are at their smallest. OSIRIS is not sensitive above 1600 K, where the peak of the late Mar enhancements was observed by MIPAS. By mid-Apr, however, the peak enhancement had descended below 1400 K. The OSIRIS NO2 map shown in Figure 3 indicates that the enhancements at this time and altitude were still confined largely to the vortex, but with substantial inhomogeneity perhaps due to increased mixing as the vortex began to break down.

Figure 3.

(left) Orthographic map of MIPAS NO2 (ppbv, SZA > 95°) at 1640 K (∼43 km) for 24–26 Mar 2004. Latitudes range from 30°N to the pole, and 0° longitude is at the bottom. The white contour denotes 60° equivalent latitude, approximately the vortex edge. The white circle near the pole indicates missing data. (right) Same as left but for OSIRIS NO2 at 1350 K (∼40 km) for 12–13 Apr 2004; only ascending node data (local solar time 12–18 hrs) are included with SZA ranging from 72–85°.

[7] The POAM III and SAGE III solar occultation measurements have continual high-latitude coverage throughout the year, and can thus be used to follow the temporal progression of the enhancements in altitude. Contour plots of three-day running average NO2 profiles from POAM III and SAGE III are shown in Figure 4. By 1 Mar, enhanced NO2 is evident in the SAGE III data above 45 km, and both data sets show significant enhancements at 45 km by 9 Mar. The enhanced layer descends in time during Mar and Apr, with a maximum near 38–40 km by early May. The data shown in Figures 24, as well as the fact that particle activity in Mar–Apr 2004 (not shown) was insufficient to produce significant NOx directly in the stratosphere, confirm that the extraordinary spring/summer enhancements in Figure 1 arise from descent of NOx-rich air from the mesosphere prior to the beginning of Mar.

Figure 4.

Three-day running averages of (left) POAM III and (right) SAGE III SS NO2 mixing ratios (ppbv) from 1 Feb to 31 May 2004. For Feb–Apr, only data inside the vortex is included. Measurement latitudes are shown at the top of each plot.

3. Origin of the Spring/Summer NOx Enhancements

[8] Two requirements must be satisfied to explain the 2004 NOx enhancements: a significant source of mesospheric NOx, and efficient descent to the upper stratosphere. The anomalous nature of the 2004 enhancements suggests that one or both of these requirements was met in an extraordinary way. The Oct–Nov 2003 solar storms were certainly exceptional, but were they the ultimate source? That significant NOx was produced from the stratosphere to the thermosphere during the Oct–Nov 2003 solar storms is evident from numerous satellite observations [Jackman et al., 2005; Seppälä et al., 2004; O05]. Ideally, the descending layer of enhanced NO2 shown in Figure 4 would be traced back in time and upward in altitude to its origin, but no reliable POAM III or SAGE III NO2 data exist above the highest altitudes shown here. However, the measurement of NOx (NO + NO2) enables the examination of enhancements up into the mesosphere. Polar (>60°N) NOx data from the Atmospheric Chemistry Experiment (ACE) are available from mid-Feb to late-Mar 2004, and show an enhanced layer descending inside the vortex during this time from ∼55 to 45 km (C. P. Rinsland et al., ACE stratospheric measurements of NOx and long-lived tracers during February and March 2004, submitted to Geophysical Research Letters, 2005). Using HALOE data, N04 also show NO enhancements inside the vortex in mid-Feb above 50 km. Further analysis of HALOE data (not shown) reveals late January 2004 NO enhancements greater than 200% compared to mean values in 1992–2003; the enhancements occur between 60 and 70 km, and the HALOE measurement latitude at this time was ∼47°N. Because of the sparse latitude sampling of solar occultation instruments, these data are not definitive. At a minimum, they suggest that the anomalous springtime enhancements originated in the polar region above 60 km before the end of January. Nevertheless, there are no satellite measurements of NOx in the polar mesosphere/thermosphere from Nov through Jan that unambiguously connect the late Jan enhancements to the storms.

[9] This leads to the question of whether it is possible that the source of the springtime enhancements was EPP production of NOx after, not during, the Oct–Nov storms. A major warming resulted in a breakup of the upper stratospheric vortex in late Dec 2003; the vortex re-gained strength throughout Jan 2004, and by Feb–Mar was the strongest on record since at least 1979 [Manney et al., 2004]. Therefore, assuming meteorological conditions in the mesosphere mirrored those in the upper stratosphere, NOx produced in the Oct–Nov storms that had descended to the mesosphere by late Dec probably experienced substantial mixing to lower latitudes. Here it would have been photolyzed, reducing the probability for observing enhanced NOx in the stratosphere by Mar. On the other hand, NOx-rich air in the polar lower mesosphere in late Jan most likely experienced less transport to midlatitudes, resulting in an unusually high probability of being transported to the stratosphere. Thus, nominal EPP that occurred well after the Oct–Nov storms, together with the unique dynamical situation in 2004, could have resulted in NOx enhancements in the springtime upper stratosphere qualitatively similar to those seen in Figure 4. Determining whether NOx production after the major warming, in combination with the unprecedented vortex strength, was sufficient to explain the magnitude of the anomalous springtime enhancements is the subject of future work.

4. Summary

[10] NOx and O3 data from numerous satellite instruments have been analyzed to present a broad overview of EPP effects on the NH stratosphere from Nov 2003 through Jul 2004. EPP effects are ubiquitous in 2003–2004 satellite data, providing a unique opportunity to test our understanding of atmospheric coupling via EPP. NOx production from the upper stratosphere through the mesosphere occurred in Nov as a direct result of strong solar storms in Oct–Nov 2003. Substantially elevated mesospheric NOx was observed in Jan as well; whether this was a result of NOx-rich air descending after the initial storms, or new production from smaller SPEs and energetic electrons, is still undetermined. By late Jan, the satellite data indicate a systematic descent of NOx-rich air in the vortex that finally led to unprecedented (in the NH data sets shown here, which span 1984–present) NOx enhancements and O3 reductions in the upper stratospheric vortex from Mar–May 2004. The anomalies declined as the vortex broke up, but were still evident even in Jul. The extraordinary springtime NOx enhancements and O3 reductions are attributed to a combination of EPP and an exceptionally strong vortex from late Jan into Apr that confined NOx-rich air to the polar region, and allowed relatively unmixed descent in the polar lower mesosphere and upper stratosphere. Detailed 3-D modeling including explicit calculation of NOx production in the upper atmosphere by precipitating electrons and protons over a wide range of energies is necessary to definitively attribute, or not, the observed NOx enhancements to the powerful solar storms of Oct–Nov 2003.

Acknowledgments

[11] We thank D. Evans, C. Jackman, M. Natarajan, and C. Rinsland for helpful discussions. CER and VLH were supported by NASA grant NNG04GF39G. Work at the JPL, Cal. Tech. was done under contract with NASA. YOR was supported by EU Commission TOPOZ-III project, and ESA CAL/VAL. Occultation data are available via the NASA EOSDIS Gateway. MIPAS data used here were near-real-time provided by ESA.

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