Geophysical Research Letters

Modeling atmospheric effects of the September 1859 solar flare

Authors


Abstract

[1] We have modeled atmospheric effects, especially ozone depletion, due to a solar proton event which probably accompanied the extreme magnetic storm of 1–2 September 1859. We use an inferred proton fluence for this event as estimated from nitrate levels in Greenland ice cores. We present results showing production of odd nitrogen compounds and their impact on ozone. We also compute rainout of nitrate in our model and compare to values from ice core data.

1. Introduction

[2] Atmospheric ozone effects by solar proton events (SPEs) associated with solar eruptive events have been studied since the 1970's. Ozone depletion occurs following the production of odd hydrogen- and nitrogen-oxides. Production of HOx (e.g., H, OH, HO2) and NOy (e.g., N, NO, NO2, NO3) and depletion of O3 by solar proton events has been studied through both satellite observations and computational modeling [e.g., Crutzen et al., 1975; Heath et al., 1977; Reagan et al., 1981; Jackman and McPeters, 1985; Jackman et al., 2000, 2001]. Jackman and McPeters [2004] review much of the work in this area.

[3] The solar flare of 1 September 1859 was one of the most intense white-light flares ever observed [Tsurutani et al., 2003; Clauer and Siscoe, 2006]. The flare itself was observed independently by Carrington [1860] and Hodgson [1860] and lasted approximately 5 minutes. The flare was followed about 17 hours later by a magnetic storm at the Earth which lasted about 2 hours [Carrington, 1860; Tsurutani et al., 2003]. The storm was of such intensity that in the United States and Europe fires were started after arcing from induced currents in telegraph wires [Loomis, 1861]. The storm was likely caused by energetic charged particles accelerated by one or several highly energetic coronal mass ejections (CME) from the Sun at the time of the flare. The geomagnetic activity associated with the accelerated particles lasted several days at least [Chapman and Bartels, 1940]. Studies of very energetic events associated with solar activity are important in understanding how such activity impacts various Earth-based systems. An event as energetic as the 1859 one has not been modeled in this way before, and it may be that events of this magnitude and larger are not uncommon over the long term [Schaefer et al., 2000; Smith and Scalo, 2007].

2. Methods

[4] Our modeling was performed using the Goddard Space Flight Center two-dimensional atmospheric model that has been used previously for modeling SPEs [Jackman et al., 1990, 2000, 2001, 2005a, 2005b], as well as much higher energy events such as gamma-ray bursts [Thomas et al., 2005]. We briefly describe the model here. More detail on the version of the model used and its reliability for high fluence events is given by the appendix of Thomas et al. [2005].

[5] The model's two spatial dimensions are altitude and latitude. The latitude range is divided into 18 equal bands and extends from pole to pole. The altitude range includes 58 evenly spaced logarithmic pressure levels (approximately 2 km spacing) from the ground to approximately 116 km. The model computes 65 constituents with photochemical reactions, solar radiation variations, and transport (including winds and small scale mixing) as described by Thomas et al. [2005] and Fleming et al. [1999]. A photolytic source term is computed from a lookup table and used in calculations of photodissociation rates of atmospheric constituents by sunlight [Jackman et al., 1996].

[6] We have employed two versions of the atmospheric model. One is intended for long term runs (many years) and includes all transport mechanisms (e.g., winds and diffusion); it has a time step of one day and computes daily averaged constituent values. The second is used for short term runs (a few days) and calculates constituent values throughout the day and night, but does not include full transport. This version has a time step of 225 seconds.

[7] No direct measurements of the proton fluence are available from 1859, but an estimate of the fluence of this event based on measurements of nitrate enhancement in Greenland ice cores is given by McCracken et al. [2001a, 2001b]. They use nitrate enhancements associated with events of known proton fluence (e.g. the 1972 and 1989 flares) to determine a scale factor between fluence and nitrate enhancement. This allows an estimate of fluence given a measured nitrate enhancement, with a range based on possible scale factor variation.

[8] We assume a fluence of protons with energies greater than 30 MeV of 27.4 × 109 cm−2 for the 1859 event, corresponding to the middle of the range of estimated values of McCracken et al. [2001a, 2001b]. Given the known fluence of the October 1989 event (4.2 × 109 cm−2 [McCracken et al., 2001a]) the 1859 event was 6.5 times more energetic in protons. We use this value to scale up the computed atmospheric ionization profiles that were used by Jackman et al. [1995] to study effects of the October 1989 event for use in this study. This scaling is, of course, uncertain, since there is no way to know the specific proton spectrum for the 1859 event since this sort of data was not available before about 1955 [Svestka and Simon, 1975], but it is a “best guess” approach. A linear scaling seems appropriate, given that it has been shown for photon events of large fluence (which have similar atmospheric effects) that the production of nitrogen oxides (NOy) scales linearly with fluence, and the deposition of nitrate is directly dependent upon the NOy production [Ejzak et al., 2007; Thomas et al., 2005]. While x-rays from the flare would be important in the upper atmosphere (above about 70 km), they do not penetrate to the stratosphere and so have little or no impact on ozone [Barth et al., 1999; Hines et al., 1965]. We have therefore neglected any effects of x-rays.

[9] The scaled-up ionization profiles are input to the short term version of the atmospheric model as a source of NOy and HOx which then go on to deplete ozone through catalytic cycles [Jackman and McPeters, 2004]. Several previous SPE studies have found that the proton flux is restricted to latitudes above about 60° [McPeters et al., 1981; Jackman et al., 2001, 2005b] by the Earth's magnetic field, the structure of which is modified by the SPE. We have no way of knowing the precise latitude restriction of the proton flux in the 1859 case, but we adopt the previous limit as likely.

[10] We scale the whole range of ionization rates from the October 1989 event by a factor of 6.5, including ionizations that result from protons with energies between 1 and 30 MeV. The HOx constituents, which are especially important above 50 km, are greatly impacted but have relatively short lifetimes and their effect is gone within several hours after the event is over. NOy constituents above 50 km are increased by these lower energy protons and can be transported downwards to the upper stratosphere (below 50 km) during late fall and winter [Jackman et al., 2005b]. The largest stratospheric impact will be by those protons with energies greater than 30 MeV, because the NOy produced by these high energy protons will be much deeper into the stratosphere where the lifetime of the NOy family can be quite long (months in the middle stratosphere to years in the lower stratosphere).

[11] While the main magnetic storm associated with the 1859 flare was observed to last about 2 hours, the particle event likely occurred over several days, perhaps as many as 10 days. Most SPEs have durations of several days; the 1989 SPE from which we are extrapolating lasted 12 days. We have chosen to input ionization from the 1859 SPE over 2 days in our model. This duration may be shorter than the actual event, though we note that the magnetic storm had a short duration. This is a convenient duration for practical purposes with the model we used. It is known that long term atmospheric effects (e.g. ozone depletion) from such ionization are much more strongly dependent on total fluence than on duration [Ejzak et al., 2007]. Therefore, we believe a difference in duration is not likely to yield significant changes to our conclusions. An expanded study could check this assertion in the context of proton events.

[12] The total ionization is distributed over the 2 day duration uniformly (i.e. as a step function) in the middle of a 7 day run of the short term model. Results of this run are then read in to the long term model which is run for several years to return the atmosphere to equilibrium, pre-flare conditions.

3. Results

[13] Our primary results are changes in NOy and O3 in the stratosphere. NOy is produced in the high latitude areas where the protons enter the atmosphere. Figure 1 shows the NOy generated during and shortly after the event, as the percent difference in column NOy between a run with the effect of the SPE included and one without. The maximum localized increase in column NOy is about 240%.

Figure 1.

Percent difference in column NOy between perturbed and unperturbed runs during the week in which the SPE occurs.

[14] Figures 2 and 3show the percent difference in profile NOy and O3, respectively, between a run with the effect of the SPE included and one without, as a function of altitude and latitude, two months after the event. This is the point in time when the globally averaged ozone depletion is largest. Note that the increased NOy extends primarily upward in altitude from about 30 km and is most widespread in altitude at latitudes above about 30°. Also, the O3 change is contained primarily within a band around 40 km altitude and restricted to latitudes above 30°.

Figure 2.

Percent difference in profile NOy between perturbed and unperturbed run, at two months after the event.

Figure 3.

Percent difference in profile O3 between perturbed and unperturbed run, at two months after the event.

[15] Figure 4 shows the percent difference in column NOy between a run with the effect of the SPE included and one without for four years after the event. As is apparent from this plot, NOy is transported to some degree to mid and low latitudes, but remains primarily concentrated in the high latitude regions as the atmosphere recovers to its pre-event equilibrium.

Figure 4.

Percent difference in column NOy between perturbed and unperturbed runs for the first four years after the SPE.

[16] Figure 5 shows percent difference in column O3 between a run with the effect of the SPE included and one without for four years after the event. The maximum localized decrease in O3 column density is about 14% and occurs in the high latitude areas where the NOy increase is largest.

Figure 5.

Percent difference in column O3 between perturbed and unperturbed runs for the first four years after the SPE.

[17] One may notice in Figures 15 that there is asymmetry between northern and southern hemisphere regions. This is because levels of NOy and O3 vary seasonally, especially in the polar regions, due to variations in the presence and intensity of sunlight. Photolysis reactions play a critical role in the balance of constituents here and strongly affect the total values. A detailed discussion of these effects can be found in the work by Thomas et al. [2005] for the case of a gamma-ray burst.

[18] Figure 6 shows the globally averaged percent difference in ozone. The maximum decrease is about 5%, which occurs two months after the event. Maximum global ozone depletion is delayed as NOy spreads and interacts with O3 over a larger area. This is quantitatively similar to the globally averaged anthropogenically-caused ozone depletion currently observed, which is predicted to diminish slowly over several decades [World Meteorological Organization, 2003]. By contrast, this naturally-caused ozone depletion from the 1859 solar flare is nearly gone in about four years.

Figure 6.

Globally averaged percent difference in column O3 between perturbed and unperturbed runs for the first four years after the SPE.

[19] Since we have estimated the intensity of the 1859 SPE using data from nitrate deposition in ice cores, a consistency check may be done by computing the nitrate rainout in the model. We have approached such a comparison in two ways.

[20] First, the maximum localized enhancement over background in the model is about 14%, while the 1859 spike in Figure 1 of McCracken et al. [2001a] is about 200% over background. This is obviously a large disagreement. However, because nitrate deposition can be spotty and takes place over a period of months, we have also computed absolute deposition values. Adding up deposition in the model over three months following the flare, within the 10° latitude band centered at 75° North, yields a value of 1360 ng cm−2. A similar computation following McCracken et al. [2001a, 2001b], using the fluence value assumed above and a value of 30 for the conversion factor between fluence and nitrate deposition [McCracken et al., 2001a], gives 822 ng cm−2, a factor of about 1.7 smaller than the model value.

[21] We note that the difference between modeled and observed absolute deposition values is opposite that of the percent enhancement over background. That is, the percent enhancement in the model is smaller than that from the ice core data, while absolute values from the ice core data are smaller than in the model. Given the many sources of uncertainty the absolute comparison is at least reasonably close, being less than a factor of two different.

[22] It is important to note that the percent enhancement comparison looks only at the height of the peak above background, while the absolute deposition value is effectively the area under that peak. A difference in how the nitrate is deposited over time could help explain this discrepancy. If in the actual event most of the nitrate was deposited in a relatively short amount of time compared to the model then the height of the peak would be greater, even if the area under that peak is less, as seen in our comparisons.

[23] Similar comparisons have been done before with this model [Jackman et al., 1990; Thomas et al., 2005]. Jackman et al. [1990] found that the model showed a smaller peak percentage enhancement of nitrates than did ice core results of Zeller et al. [1986] (around 10% from the model, compared to 400% from ice core). This discrepancy is of the same order as what we have found in this study and apparently indicates some scaling disagreement between the model computations and the observations.

4. Conclusions

[24] We find for the 1859 event an atmospheric impact appreciably larger than that of the most energetic flare in the era of satellite monitoring, that of October 1989. Localized maximum column ozone depletion (see Figure 5) is approximately 3.5 times greater than that of the 1989 event [see Jackman et al., 1995, Figure 3]. We note that this is a smaller factor than that relating the total energy of the two events (6.5). Ozone depletion has been seen in other contexts (e.g., gamma-ray burst impacts) to scale less than linearly with total energy [Thomas et al., 2005; Ejzak et al., 2007]. Causes for this weaker dependence include: increased removal of important depletion species such as NO with increased levels of NOy; production of O3 in isolated regions especially at lower altitudes which are normally shielded from solar UV which produces O3; and the “saturation” of depletion, where most of the O3 in a given region is removed and so cannot be depleted any further.

[25] Our nitrate deposition results do not show as dramatic an enhancement as the measurements by McCracken et al. [2001a]. This discrepancy does mirror a similar comparison between nitrate deposition as computed using this model and that measured in ice cores as described by Jackman et al. [1990]. This discrepancy may reflect differences in transport or deposition efficiency.

[26] Finally, while the ozone depletion seen here is limited, even small increases in UVB can be detrimental to many life forms [Rousseaux et al., 1999; Cullen et al., 1992]. Flares of significantly larger energy have been observed on Sun-like stars [Schaefer et al., 2000], and may occur from time to time through the long history of life on Earth. (See Hallam and Wignall [2003] for an overview of terrestrial extinctions.) Such events would have more dramatic effects on the biosphere. Knowledge of the impacts of such flares is important in understanding the history of life here and possibly elsewhere, in particular on terrestrial planets around stars which are more active than the Sun.

Acknowledgments

[27] This work was supported in part by the NASA Astrobiology: Exobiology and Evolutionary Biology Program under grant NNG04GM14G at the University of Kansas, by the NASA Living with a Star Targeted Research and Technology Program, and by the NASA Atmospheric Composition Data and Analysis Program.

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