Variation of Total Ozone during 24 August 2005 Magnetic Storm: A Case Study

doi:10.4236/acs.2013.34049

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Atmospheric and Climate Sciences, 2013, 3, 475-480

http://dx.doi.org/10.4236/acs.2013.34049 Published Online October 2013 (http://www.scirp.org/journal/acs)

Variation of Total Ozone during 24 August 2005

Magnetic Storm: A Case Study

Gustavo A. Mansilla1,2

1Departamento de Física, Facultad de Ciencias Exactas y Tecnología, Universidad Nacional de Tucumán,

San Miguel de Tucumán, Argentina

2Consejo Nacional de Investigaciones Científicas y Técnicas, Buenos Aires, Argentina

Email: [email protected]

Received June 11, 2013; revised July 13, 2013; accepted July 21, 2013

which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

ABSTRACT

This paper presents the longitudinal distribution of total ozone along several latitudinal circles from both hemispheres

during a strong geomagnetic storm that occurred on 24 August 2005 after a solar proton event (the maximum flux of

protons with energy > 10 MeV was 1.70 × 107 protons cm−2·day−1·sr−1 on 23 August). For that, we use average daily

values of total ozone observations (=column ozone amount) in Dobson units for the period 18-25 August 2005 (ob-

tained from the Total Ozone Mapping Spectrometer, TOMS). The considered storm occurred after a relatively quiet

geomagnetic period and it is not superposed by another perturbation, which permit us to identify clearly the effects of

the geomagnetic storm on total ozone. The results show statistically significant decreases in ozone along the latitudinal

circles 70˚N and 70˚S (summer and winter), no statistically significant effects at middle latitudes (40˚S) and sparse sta-

tistically significant increases at low latitudes (20˚S). The role of some mechanisms to explain the features observed is

considered.

Keywords: Solar Proton Event; Geomagnetic Storm; Ozone; Hemispheres

1. Introduction

Solar Proton Events (SPEs) occur when protons with

very high energy are emitted by the Sun during solar

flares or coronal mass ejections (CME), sometimes to-

ward the Earth. High energy solar protons can penetrate

the Earth’s magnetic field near the poles. These protons

penetrate into the atmosphere, typically to the 40 to 80

km height. Only 12 - 15 events per solar cycle can be

recorded at the ground level [1]. In this way, they pro-

vide a direct connection between the Sun and the Earth’s

middle atmosphere [2]. Geomagnetic storms (temporary

disturbances of the Earth’s magnetic field) can be ex-

pected during solar flares and CMEs but not because of

the increase of charged particles into the Earth’s magne-

tosphere. They can occur when the interplanetary mag-

netic field (IMF) is southward and the solar wind crosses

the Earth for long duration of time or in shorter more

energetic bursts (flares/CMEs). When the IMF is south-

ward, a magnetic reconnection of the dayside magneto-

pause is produced, rapidly injecting magnetic and parti-

cle energy into the Earth’s magnetosphere.

Geomagnetic storms cause large disturbances in the

upper atmosphere (ionosphere and thermosphere) includ-

ing also the middle atmosphere and the troposphere [3,4].

Solar energetic particles which reach middle atmosphere

cause ionization of air molecules. As the ionized mole-

cules recombine, they produce nitrogen and hydrogen

oxides which can affect ozone through odd nitrogen NOy

and odd hydrogen HOx catalytic reactions (see e.g., [5]

for details). Decreases of ozone in the middle atmosphere

after large solar proton events have been predicted by

atmospheric models (e.g., Whole Atmosphere Commu-

nity Climate Model WACCM3), and also observed by

satellite measurements [6-8]. The stratospheric ozone

effects were caused by the odd nitrogen. Very large NOy

enhancements lasted for months in the middle and lower

stratosphere after some largest SPEs. Using a two-dimen-

sional chemistry and transport atmosphere model, [9]

compute the effects of gigantic SPEs in the stratosphere.

They obtained upper stratospheric ozone depletions >

10% to last for a few months after the SPEs. Moreover,

during the October-November 2003 series of solar proton

events, ozone depletion varying from 20% at 40 km alti-

tude to more than 95% at 78 km was found [10].

Some studies show that during intense geomagnetic

G. A. MANSILLA

476

storms the total ozone presents a pattern which is statis-

tically significant at the northern higher middle latitudes

only under very limited conditions [11]: in winter and

under the high solar activity and the East phase of the

QBO conditions. At around 50˚N latitudinal circle, but

not around 40˚N and 60˚N, the effect appears to be basi-

cally re-distribution of ozone (in the North Atlantic-

European it means an increase of the total ozone), neither

its loss, nor its production.

This short paper shows the short-term latitudinal dis-

turbances in the total ozone content as consequence of an

isolated geomagnetic storm occurred during the descen-

ding phase of solar cycle 23 (solar flux on storm day:

100.7). Since this storm came after a relatively quiet so-

lar/magnetic period and it is not superposed upon by an-

other perturbation, it is reasonable to assume that the

variations on total ozone during the considered storm

period are caused by the geomagnetic storm. In fact, the

selected geomagnetic storm was characterized by an SSC

(storm sudden commencement), which was preceded by

quiet days and without the arrival of a new solar rapid

flow during its phase of recovery, that is, a new storm is

not superimposed. Moreover, with the results obtained

here we can check the pattern of total ozone variation

during geomagnetic storm obtained by [11].

Case studies which consider several latitudes from

both hemispheres are rare but they are important for a

view of global space weather and also to know and/or

check the role of possible physical mechanisms. In addi-

tion, the ozone response to geomagnetic storms has not

been given adequate attention over Southern latitudes

[12].

We will first describe the datasets used for quantifying

the total ozone response to the geomagnetic storm. After

that, present our observations. Finally, a discussion and

the conclusion are given in Section 4.

2. Data

The database used in this study consists of average daily

values of total ozone observations (=column ozone

amount) in Dobson units for the period 18-25 August

2005, which were obtained from the Total Ozone Map-

ping Spectrometer (TOMS) (http://jwocky.gsfc.nasa.gov/

ozone/ozone.html). We considered the measurements

obtained each 10˚ of geographic longitude, between

–180˚ and +180˚ (37 observations) at different latitu-

dinal circles of the Norhtern Hemisphere (NH) and the

Southern Hemisphere (SH): 20˚, 40˚, 60˚ and 70˚.

The Earth Probe EP-TOMS instrument measures back-

scattered ultraviolet radiance from Earth at wavelength

bands centered at 308.6, 313.5, 317.5, 322.3 331.2 and

360.4 nm. One significant difference in the EP-TOMS

series from the previous Nimbus-7 and Meteor 3 TOMS

is a change is the wavelength selection for the 6 channels

of the three new instruments. Four of the nominal band

center wavelengths remain the same on all TOMS. Chan-

nels measuring at 340 nm and 380 nm have been elimi-

nated in favor of 309 nm and 322 nm on the new TOMS.

Ozone retrieval at 309 nm is advantageous because of the

relative insensitivity to calibration errors, though retriev-

als are limited to equatorial regions. Ozone retrievals at

high latitudes are improved because 322 nm is a better

choice for the optical paths encountered there [13]. Total

column ozone is inferred from the differential absorption

of scattered sunlight in the ultraviolet using the ratio of

two wavelengths, 312 nm and 331 nm for instance,

where one wavelength is strongly absorbed by ozone

while the other is weakly absorbed. TOMS is subject to

errors and random uncertainties. Some of these errors

come from the instrument and others from environmental

phenomenon. Aside from some known problems at spe-

cific times and locations, accuracy is believed to be

within 3% - 4% of actual ozone levels.

The magnetic activity as represented by the geomag-

netic index Dst. The hourly values of Dst were obtained

from the world Data Center at the University of Kyoto

database (http://swdc.kugi.kyoto-u.ac.jp/dstdir).

3. Results

In August 2005, the Sun released a solar flare (M5/1N)

associated with a CME (Halo/22 1730). Consequently

the flux of particles toward the Earth’s atmosphere was

greatly enhanced. A solar proton event began on 22 Au-

gust 2005 at 2040 UT, reaching a maximum on the fol-

lowing day at 1045 UT. Figure 1 shows the daily meas-

urements of the proton fluence taken by the GOES-11

satellite during August 2005 (http://www.swpc.noaa.gov/

ftpmenu/warehouse/2005.html. For the more important

proton event occurred during August 2005 it can be seen

that the protons with different energies are increased by

several orders of magnitude. The flux of the protons with

energy > 10 MeV was about 1.60 × 104 protons cm−2·

day−1·sr−1 prior to the solar flare, and reached a maximum

of 1.70 × 107 protons cm−2·day−1·sr−1 on 23 August.

We focused the analysis on the geomagnetic storm that

took place two days after SPE. Figure 2 shows the geo-

magnetic index Dst for August 2005. It can be clearly

seen the only intense geomagnetic storm occurred that

month: the magnetic storm started on 24 August (kp =

46; Ap = 102) with a sudden commencement at 0613 UT.

An abrupt decrease is observed at about 11 - 12 UT that

day when Dst reached its minimum of –216 nT after

which started a relatively rapid recovery.

We selected ten magnetically quiet days of the month

of the storm to obtain an average pre-storm quiet level of

total ozone and calculate the average value and σ sepa-

rately for each latitudinal circle. The storm effect in the

G. A. MANSILLA 477

August-2005

1,E+03

1,E+04

1,E+05

1,E+06

1,E+07

1,E+08

1,E+09

1611 1621 26 31

Day

protons/cm2-day-sr

> 1MeV> 10 M eV> 100 M eV

Figure 1. Daily values of proton fluence (protons/cm2/day/

sr) for August 2005, measured by GOES-11 satellite. Three

curves indicate protons with energies above 1, 10 and 100

MeV.

August-2005

-250

-200

-150

-100

-50

12345678910 11 12 13 14 15 16 17 1819 20 21 22 23 24 25 26 27 28 29 30 31

Day

Dst (n T )

Figure 2. Hourly variation of the geomagnetic index Dst for

August 2005. It can be observed the only intense storm oc-

curred that month.

total ozone may be considered as significant if the devia-

tion in individual storm days exceeds 2σ. This is the

usual criterion normally used to demonstrate the exis-

tence of a storm effect in variations of any geophysical

parameter [12]. Some cases with statistically significant

deviation (>2σ) and no statistically significant deviation

are shown in this paper.

Figures 3 and 4 display the longitudinal variation of

the total ozone at the latitudes 70˚N and 70˚S (summer

and winter hemispheres, respectively) for the storm pe-

riod 22-25 August together with ±2σ (thin curves). It can

be seen that the behavior of total ozone differs substan-

tially in the individual days and does not reveal any per-

sistent pattern. Statistically significant decreases in total

ozone are observed in the 30˚ - 120˚ longitude sector

(Northern Europe) on the storm day (24 August), and in

the longitude range −70˚ to −30˚ and −150˚ to −120˚ in

the Southern Hemisphere on 23 and 24 August. It can be

seen that individual days differ substantially and do not

reveal any persistent pattern.

Figure 5 shows the variation in total ozone at 60˚S

(winter). One can observe that the variations of total

ozone in the individual days show a similar trend. The

higher values of total ozone are observed in the east sec-

tor (about 60˚ - 120˚ longitude). Statistically significant

increases in total ozone are observed at longitudes be-

tween −120˚ and −60˚ and between +60˚ and +120˚ on

24-25 August, and statistically significant decreases at

higher longitudes (~ 150˚ - 180˚) in the west and the east

Latitude: + 70 degrees

200

250

300

350

400

1801501209060300-30-60-90-120-150-180

Longit ude (degree s)

T otal ozone ( DU)

(22)

(23)

(24)

(25)

+2sigma

-2sig ma

Figure 3. Longitudinal variation of total ozone on 22-25

August 2005 along the latitudinal circle 70˚N for the geo-

magnetic storm occurred on 24 August. Thin curves indi-

cate +/−2σ uncertainty.

Latitude: - 70 degrees

100

150

200

250

300

350

1801501209060300-30-60-90-120-150-180

Longit u de ( deg re es)

T otal o z one (DU)

(22)

(23)

(24)

(25)

+2sigma

-2sig ma

Figure 4. Same as Figure 3 but for the latitudinal circle

70˚S.

Latitude: - 60 degrees

100

150

200

250

300

350

400

450

500

18015 01209060300-30-60-9 0-120-150-180

Longitude ( degr e es)

Total ozone (DU)

(22)

(23)

(24)

(25)

+2sigma

-2sigma

Figure 5. Same as Figure 3 but for the latitudinal circle

60˚S.

sectors. The total ozone at 60˚N in the summer hemi-

sphere (not shown here) reveals similar behavior that the

winter hemisphere.

Figure 6 shows the behavior in total ozone at the lati-

tude 40˚S. As at higher latitudes, the total ozone values at

mid latitudes differ each day and they do not reveal any

regular pattern. A statistically significant effect of the in-

tense geomagnetic storm in ozone is observed only be-

tween −120˚ and −100˚ of the Southern Hemisphere.

Similar result (not shown here) is observed for 40˚N.

Figure 7 presents the variation in total ozone along the

latitudinal circle 20˚S (winter). Statistically significant

increases can be observed between −60˚ and −150˚ on

24-25 August. The rest of the longitudinal sectors do not

present any evident effect of the geomagnetic storm on

total ozone.

In order to determine a possible longitudinal re-dis-

tribution of total ozone during a geomagnetic storm, we

calculated “the mean zonal total ozone” TO3-zonal. This

G. A. MANSILLA

478

parameter was defined as follows: the quotient between

the difference of the average of the measurements taken

each 10 degrees during the storm days in each longitudi-

nal circle and the average pre-storm values above men-

tioned, and the average pre-storm values (in percentage).

Figures 8 and 9 show the results for the summer and

Latitude: - 40 degrees

200

250

300

350

400

450

18015012 09060300-30-6 0-90-120-150-180

Longitude ( deg r ee s)

T otal oz on e ( DU )

(22)

(23)

(24)

(25)

+2sigma

-2sigma

Figure 6. Same as Figure 3 but for the latitudinal circle

40˚S.

Latitud e: - 20 degrees

200

250

300

1801501209060300-30-60-90-120-150-180

Longitude (degrees)

Total ozone (DU)

(22)

(23)

(24)

(25)

+2sig ma

-2sigma

Figure 7. Same as Figure 3 but for the latitudinal circle

20˚S.

Nort hern Hem isphere

-5

-4

-3

-2

-1

22 2324 25

day

TO3-zonal (%)

20 40 60 70

Figure 8. Relative variation of the zonal mean total ozone

along several latitudinal circles (20˚, 40˚, 60˚ and 70˚) for

the Northern Hemisphere during the storm period 22-25

August 2005.

Southern Hemisphere

-5

-3

-1

22 23 24 25

day

TO3-zonal (% )

-20 -40 -60 -70

Figure 9. Same as Figure 8 but for the Southern Hemi-

sphere.

winter hemispheres respectively. At the Northern Hemi-

sphere (summer), the larger decrease is produced at 60˚N

(<5%); at higher latitudes (70˚N) the decrease is lower in

association with statistically significant decreases, while

at middle and low latitudes no substantial change is ob-

served (<1%). At the Southern Hemisphere (winter) the

larger decrease occurs in the high latitude region (<5%)

also in association with statistically significant decreases,

whereas at low latitude there is a small increase. The

magnitude of the changes in both hemispheres seems to

indicate that at 60˚N in the summer hemisphere and at

higher latitudes from the winter hemisphere there is a

decrease in ozone, while at the other latitudes would oc-

cur zonal re-distribution in ozone.

4. Discussion and Conclusions

This paper reports the longitudinal variation of the total

ozone measured along different latitudinal circles at the

Northern and Southern Hemispheres during the isolated

geomagnetic storm occurred on 24 August 2005.

The main observational results can be roughly summa-

rized as follows:

 Along the latitudinal circles 70˚N and 70˚S statisti-

cally significant decreases in total ozone are observed

in the Northern Europe (30˚- 120˚ longitude sector)

on the storm day, and in the longitude range −70˚ to

−30˚ and −150˚to −120˚ in the Southern Hemisphere.

 Along the latitudinal circle 60˚S statistically signifi-

cant increases in total ozone are produced at longi-

tudes between −120˚ and −60˚ and between 60˚ and

120˚ and decreases at higher longitudes in the west

and east sectors on 24 August.

 At mid latitudes (40˚S) no statistically significant

effect of geomagnetic storm in ozone is observed,

while at low latitudes (20˚S) they are sparse.

 In general, the longitudinal distribution in total ozone

shows small loss in both hemispheres during SPE

event on 22 August 2005. At the NH the maximum

loss is observed around the 60˚N latitudinal circle

(~5%); around the longitudinal circles corresponding

at 40˚ N and 70˚ the loss is of the order 1% - 2%. At

the SH no significant production in total ozone is ob-

served at around the 20˚ longitudinal circle (~1% -

2%), almost no changes at 40˚S and 60˚S, and at 70˚

loss in the total ozone (~5%) the day of the greater

proton fluence. These results seem to suggest a redis-

tri- bution of the total ozone only in some latitudinal

cir- cles, where the relative deviation of the “zonal

total ozone” is lower than 1% - 2%. It might owe to

changes in the stratospheric storm-time circulation

which could produce redistribution of ozone along

longitudinal circles.

The results obtained here suggest that total ozone is

affected by geomagnetic disturbances. According to [11],

G. A. MANSILLA 479

the Northern Hemisphere is not under all the favourable

conditions for a significant ozone response during the

considered event because NH is in the summer season.

Analyzing 5 strong geomagnetic storms occurred in

July-August for the period 1982-1991, [12] found that

contrary to the Northern Hemisphere, detectable effects

of geomagnetic storms on total ozone do not occur at the

Southern Hemisphere higher middle latitudes. On the

contrary, we found longitudinal variations at 60˚ - 70˚ in

winter in the Southern Hemisphere.

Some total ozone column depletions are observed near

the south boundary of the Atlantic South magnetic

anomaly and close to the boreal geomagnetic pole which

suggests that geomagnetic field longitude seems to play

an important role in ozone variation. The ozone change

in the South Atlantic anomaly agrees with [14], who ob-

served mesospheric ozone depletion in that region.

There is an evident depletion of total ozone (~5%) dur-

ing the strong geomagnetic storm in the 60˚N and 70˚S

longitudinal circles. During both quiet and disturbed

conditions the Antarctic polar vortex creates ozone de-

pletion. A speculative and no verifiable explanation is

that the polar vortex plays a significant role in the loss of

ozone at high latitudes of the winter hemisphere during

the storm. However, satellite observations taken during

polar winter in the Antarctic indicate NOx enhancements,

which occur in good correlation with levels of enhanced

high-energy particle precipitation (associated with SPEs)

and/or geomagnetic activity (e.g., [6,15]).

A possible explanation of the depletion of ozone in the

Northern Hemisphere could be related with changes in

HOx and NOx. In fact, upper stratospheric enhancements

in NOx were measured at northern high latitudes during

storms [16,17]. Measurements from the UARS HALOE

and NOAA 14 SBUV/2 instruments indicate short-term

(~day) middle mesospheric ozone decreases for over

70% caused by short-lived HOx during a SPE with a

longer-term (several days) upper stratospheric ozone

depletion of up to 9% caused by longer-lived NOx.

Unfortunately no available study about the changes of

NOx in the middle atmosphere in the case of this SPE has

been found, which prevents the confirmation of that as-

sumption.

The ozone depletion observed in summer differs from

the results obtained by other authors who found that sig-

nificant effects of geomagnetic storms on total ozone

(redistribution in ozone, not ozone production or loss)

have been observed only in winter and for strong storms

(Ap > 40) and only under specific conditions [11,18,19].

Because each storm has its individual characteristics we

believe that actual patterns of response are not consistent

yet because deviations from the model pattern are ob-

served. For that reason more case studies are necessary to

obtain some common/consistent storm-time features.

In summary, we analyzed the short-term response of

the total ozone content to an isolated geomagnetic storm

along several latitudinal circles from both hemispheres

(summer and winter). The total ozone content exhibits

redistribution at middle and low latitudes (20˚ - 40˚) in

both hemispheres and decreases at higher latitudes (in

winter and summer) the days of great proton fluence.

This result is a new one and can be considered as the

main contribution of this paper to current community

knowledge on total ozone storm effects because it differs

from obtained by other authors [12]. It is clear that the

present results may be significant and could have impor-

tant implications for the study of the behavior of the at-

mosphere during geomagnetic storms, contain little sta-

tistical information. Because of the discrepancy of the

results for the different authors, it is evident that it is nec-

essary to perform further analysis of satellite measure-

ments in order to infer a statistics about the standards of

behavior of the total ozone during disturbed periods.

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