The relationship between the yearly variations of cosmic ray intensity and ozone in the atmosphere, and the ozone disturbance initiated by the Forbush decrease of 1965-1976 is analyzed. The data on cosmic ray intensity were selected from the records of the super neutron monitor at Deep River station and the ionization chamber at Beijing station. Ozone data were taken from Resolute (Canada), Bismark (N. Dakota, USA), Kagoshima (Japan), and Kodaikanal (India). The statistical results show that ozone is prominently modulated and disturbed by the 11 year variation and the Forbush decrease in the galactic cosmic ray

Wang, L.

Xue, S.

Ye, Z.

English

NASA Technical Reports Server

S21 SH I0.I-I
THE INFLUENCES OF THE GALAOTIC COSMIC RAY
ON THE ATMOSPHERIC OZONE
Ye Zonghal Xue Shunsheng
(Institute of Space Physics, Academia Sinlca,
P.O.Box 5112, 1_ljlng, China)
Wang Lian ying
(Institute of Atmospheric £hyslcs, Academia Sinlca,
P.O.I_x 2718, Beljlng, China)
I. Introduction. Warneck [I_ and Nicolet et al. [21 first
put forward that cosmic ray is a suurce of NO production in
the atmosphere. The Nicolet et al. [3,4,5] proved that each
ion pair producted by cosmic ray forms about I-1.5 NO molecul-
es becsuse of the ionization and the dissociation processes.
Because of the reaction between NO and 0 in the atmosphere
NO will dlspapear in part, so the change of _NO_ will direct-
lly influence [0_] in the atmosphere. The observational res-
ults proved that the solar cosmic ray events will cause the
large decrease of[O_] in the polar stratosphere [61 • Ruderman
et al.[7] proved thatLO_] has the law of 11 years variation.
This paper has analysed the relationship between yearly
variation of cosmic ray intensity and [0_], and[05] disturbance
initiated by Forbush decrease for 1965-1976. The data of cos-
mic ray intensity were selected from the records of the sup-
erneutron monitor at Deep River station and the ionization
chamber at Beljlng statlon;_O3]data were selected from Reso-
lute (74.4ON, 94.6ow), Canada. Bismarck (46 4ON, IOO.5ow), I°Amerlcs, Kagoshima (31.4oN, 130.4°E), Japan_ Kodaikanal (10.
N, 77.3°E), India. The statistical results show that [0_]
prominently is modulated and disturbed by 11 years variation
and Forbush decrease of the galactic cosmic ray.
II. The modulation of 11 years variation of cosmic raE inten-
_it.y on the ozone. Fig. Ic is the curves of yearly variation
of cosmic ray intensity. The solid line is the data of the
superneutron monitor at Deep River. The dashed line indlcats
meson component recorded by the ionization chamber at
Beljing. It can be seen that there is the maximum of cosmic
" ray intensity during the solar activity minimum (1964-1965),
there is the minimum of cosmic ray intensity during the solar
activity maximum (1969-1970). Fig. I _,b are the correspond-
. ing content of O3 at four variant latitudes. Used [O3]data
is selected from "Ozone data for the world" published by
Canada,8] . The analysis results show that except Resolute
Station at high latitude 11 years variation of [03] is very
evident. The ozone content decreases when cosmic ray inten-
sity increases, The ozone content increases whe cosmic ray
intensity decreases. This means the relationship between the
ozone variation and cosmic ray intensity variation is the na-
getive correlation.
It is seen from fig. 1 that 11 years variation of [O3]has
evident latitude effect. From maximum year of cosmic ray in-
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SH i0.I-I
522
_,oCo%_, tensity to minimum year[O_] increased
by 7.8% and 5.8% at Kodaikanal and
49 Kagoshima respectively. The increase
47 of [0_] decreasedWlth the increase of
the latitudes, [03] only increased by
45 o 4.8% at Bismarck.But 11 years varia-
43 _/_marck tion of [03] become indistinct at Re-
_, ' solute in the polar region.Co3_ _e'6547 e'e z, T3 75 7_
_,oo36 _ III. The disturbance of Forbush decr-
35 AJ Ko0o. ease on [033• I. Data analysis. In
34 order to study the disturbance stage
33 _0_=_.o, b of Forbush decrease for variant ampli-
32 / __ tudes on [03], Forbush decrease ev-ents are divided >1%, >2/0, >3% and3 >5% four importances based on their
1965 67 69 ?1 73 7_5 77
n , amplitudes. The disturbance analysis
x 105 "40
"\_\' fk// of the solar flare and Forbush decr-
ZSZ ',_°ijing .,8o ease on vorticity arear index (VAI)
" -,2o showed that the disturbances of VAI
24o _ /\ / ° have evident seasonal property [9].
Z34 _ / O,,p RiAzer 440
,^ ,--., So the time occurred Forbush decrease
zz, ,v,LX-''_'" -8o is also divided hhe winter (10-3 mon-
zz_,_ _7 69 7 73 _ _ 24o ths) and the summer (4-9 months).
Fig.1 _Is modulation of According to the seasons and impor-
11 years variation of tances occurred Forbush decrease, th-
eir variant combination is analysed.
cosmic ray intensity There were 234 Forbush decrease ev-
on the ozone ents during 1965-1976. The distri-
bution of various Forbush decrease events as table I shown.
Table I The distribution of Forbush decrease events
_j_rtanee I" -'_ ...... >2% >3% >5%
winter I 119 ...... 49 22 4
summer ] 115 48 28 4
total I.234 97 50 8
The method of the statistical study has used the super-
pose d epoch method. The day of the minimum of Forbush dec-
rease Is considered as the zero day. The abscissa denotes
the time in>:days for all of the figures in this section. The
ordinate represents the ozone content. The horizontal llne
refers to the average value of the total absembly of [0_].
The dashed llne represents confidence level with probability
0.05 or the degree of confidence 95%. n is the number of
Forbush decrease events.
2. Analysis results. The stqtistical study for all Forbush
decrease events shows that the disturbance of Forbush decr-
ease on [05] is of statistical sLgnificance, and the amplitude
of [0_] disturbance increases with the increase of Forbush
decrease amplitude. The disturbance of Forbush decrease on
[03] Increases with the increase of the latitudes. But at
528 SH 10.1-1
high latitudes, the effect of the solar cosmic r_v and preci-
pitating particles on IOn]will be over Forbush decrease, so
that the ozone disturbance produced by Forbush decrease all
is covered.
The disturbance of Forbush decrease occurred in the win-
ter on [0_] is larger and more evident. Usually on the day
started Forbush decrease, i.e. about at-I day, [Os] begins
increase, and there is a larger increase after the fourth day.
The amplitudes of [03] disturbance increase with the increase
of the latitudes of the observational stations. Fig. 2 shows
the disturbance of [03]for variant latitude regions in the
winter. I_cause the data of [O3_ observed in the winter at
Resolute is a few numbers, the change of [09]can not be given.
_o_ The disturbance Forbush decrease
3_o w,,,.,> O_o,.,,_/_/ occurred in the wltner on [O_]at same
latitude increases with the increase
/ of Forbush decrease amplitudes. If
3_o the average value of [03] from the third
_,...._ ° day to the fifth day before the zero
day is considered as the undlsturbance
3% 3 o 3 5 7 , value of [0_], that the largest distur-doy
%_ bance of >1% Forbush decrease on 0
2_o_.,.,o._.,O_o..,,, was about 5.3%. The largest distur-
_._--_-=-_c_/_-___- _.... bance of >2%, >3% and >5% Forbush de-
__w crease events were 5.9%, 6.2% and280
Kago=nimo ° IO. 3% respectively.
275/r , , ' , , • , , ,5 _ o 3 5 _ 9 The disturbance of Forbush decrease
°0' occurred in the summer on [09] in low
latitudes can also be seen, but its
[%]I- disturbance is very less than in the
26o_*...,_,O_o ,:,, o winter. The disturbance of Forbush
z5__----_=-_'_c____- _----_-
25o_ _°"°"J - decrease on [03]all is covered at highlatitudes. It always is the decrease
-5 -3 _ 0 _ 3 5 7 9
,o, tendency after the solar flare, and it
Fig. 2 The disturban- lasts_ several days (see Fig.3).
ce of Forbush decrease [%1|.......'°/°.o,,5 36c_/k'_' .2o/. .:,ein the winter on [033 35 5.,
IV. Conclusions and dis- 5_ ...._ _
cussion. According to 35o[-_ ___........ 3so
the results dlscribed _i_I......... _ _45, • , 340
above, we obtain the 5 3 4o 3 5 _ _ _ _ _ o, _ _ _
following conclusions: _o_ _o_
, [O_] is modulated by _%1
I1 years variation •of __'°/° n=28 [03] ....... 5% n= 4
cosmic
ray intensity. 3_o____
34O
The relationship bet- _ v ___/_ _o_/
ween the ozone variation_ ........ _,,o
and cosmic ray intensity
variation i the n gati -3_ ,o
ve correlation. The 11 _ _oo
doy doy
years vibration of [03] Fig.3 The change of COs]duringis most evident at the
Forbush decrease in the summer at
middle and the low la- Bismarck.
524
SH 10.1-i
titudes. The law of thls variation is more indistinct at
the high latitudes. Because the influences of the solar
cosmic ray and precipitating particles on [03] are so large
that the effect caused by the long period variation of cosmic
ray intensity is covered.
The disturbance of Forbush decrease occurred in the winter
on [03] is very remarkable. The disturbance of [03] evidently
increases with the rising of the latitudes. Usually [03]
increases after Forbush decrease started, and lasts several
days. The disturbance occurs the maximum after the fourth
or the fifth day. The amplitude of [03J disturbance also
increases with the increase of Forbush decrease amplitude.
The disturbance of Forbush decrease occurred in the
summer on [03] is very interesting. The effect of Forbush
decrease on [09] is also evident at the low latitudes, but
the disturbance of [03] is Just opposite to the effect caused
by Forbush decrease at the high latitudes. Evidently, this
is not produced by Forbush decrease. It is produced by the
solar cosmic ray and precipitating particle events. As was
shown by Shah [I0] , the disturbance of the solar cosmic ray
events occurred in the summer on VAI is the most remarkable.
We discover that the larger solar cosmic ray events occur in
the summer. So the disturbance of the solar cosmic ray events=
occurred in the summer on [03] can also be the most remarkable.
References.
I. Warneck, P. (1972), J. Geophys. Res., Vol. 77, 6589
2. Nicolet, M. et al. (1972), Annals Geophys., Vol. 28, 751
3. Brasseur, G. et al. (1973, Planet. Space sci., vol. 21
939
4. Nicolet, M. (1975) Planet, Space Sci, Vol. 23, 637
5. Reagan, J. B. (198_), J. Geophys. Res._ Vol. 86, 1473
6. Donald, F. H. et al. (1977), Science, Vol. 197, 866
7. Ruderman, M. A. et al. (1975), Planet. Space Sci., Vol.
23, 247
8. Ozone data for the world, environment Canada, atmospheric
environment Service 1965-1976
9. Ye Zonghai et al. (1984), Chinese Journal of Space
Science, Vol. 4, 198
10. Shah, G. N. (1981), J. Atmos. Terres. Phys, Vol. 43, 147


The influences of the galactic cosmic ray on the atmospheric ozone

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