The main features of solar cycle 23, sun enters a period of intermediate and weak solar activity in terms of sunspot number. Based on the observation from Omniweb data centre for solar- interplanetary data , geomagnetic activity and monthly mean count rate of cosmic ray intensity (CRI) variation data from Oulu / Moscow/ Keil neutron monitors (Rc=0.80 GV , Rc=2.42 GV and Rc=2.29 GV,) during solar activity cycle 23 . The phase of minimum solar activity began in May 2005 and lasted for 4.5 years the unprecedented duration of the relative sunspot numbers falls. It is observed that the strength of the interplanetary magnetic field has been falling off to new low levels, and reduces the GCR entering inner- heliosphere and it is also found that SSN positive correlated with Kp and Ap and sunspot number, 10.7 cm solar radio flux, were inverse correlated with monthly mean count rate of cosmic ray intensity.

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Solar Interplanetary and Geomagnetic Activity in Solar Cycle 23
B. K. Tiwari1
B. R. Ghormar2
1,2
Department of Physics
1
A.P.S.University Rewa, Madhya Pradesh 2
Rewa Engineering College Rewa Madhya Pradesh
Abstract— The main features of solar cycle 23,
sun enters a
period of intermediate and weak solar activity in terms of
sunspot number. Based on the observation from Omniweb
data centre for solar- interplanetary data , geomagnetic
activity and monthly mean count rate of cosmic ray
intensity (CRI) variation data from Oulu / Moscow/ Keil
neutron monitors (Rc=0.80 GV , Rc=2.42 GV and Rc=2.29
GV,) during solar activity cycle 23 . The phase of
minimum solar activity began in May 2005 and lasted for
4.5 years the unprecedented duration of the relative sunspot
numbers falls. It is observed that the strength of the
interplanetary magnetic field has been falling off to new low
levels, and reduces the GCR entering inner- heliosphere and
it is also found that SSN positive correlated with Kp and Ap
and sunspot number, 10.7 cm solar radio flux, were inverse
correlated with monthly mean count rate of cosmic ray
intensity.
Keywords: Galactic Cosmic ray(GCR), Interplanetary
magnetic field(IMF), Solar magnetic field, sunspot
number(SSN)
I. INTRODUCTION
Solar cycle 23(of 12.5 years) have the most specific feature
and revealed its properties of evolution, which is entered in
the family of the intermediate-magnitude of solar activity, it
is farmally started in May 1996 reached its maximum in
term of relative sunspot numbers in April 2000 and
maximum 10.7cm solar radio flux observed in Feb 2002 i.e.,
the maxima of the two main indices were separated in time
as in the case of previous solar activity cycle. The complete
polarity reversal of solar magnetic field for solar structure at
(70ᵒ N and 70ᵒ S) occurred during July-December 2000. The
secondary maximum of solar cycle relative to sunspot
number, was observed in Nov 2001 .This solar cycle was
different other cycle is term of the number of active regions
before declining phase and stable (non flare) active regions,
which may be weaker circulation in the solar convection
zone during this cycle as compared to previous solar cycles
(Tiwari,B.K., et al.,2014). The total number of active region
in 23rd
solar cycle still behind previous solar cycle in term
of number of optical solar flare and major x-ray flare and the
last flare region with high flare appeared in the beginning of
December 2006 (after 6.6 years of maximum). The cycle is
characterized by abrupt decrease of the fluences (total daily
fluxes) before the decrease phase (July 2002), the decrease
in the flare activity reconnected in a considerable increase in
the number of days with quiet geomagnetic conditions.
In the extended solar minimum observed in 2009-
2010 counts of highly elevated fluxes of GCRs, this results
may be found considering the reduction in the total
heliospheric magnetic flux observed by interplanetary
spacecrafts, reduction in the magnetic flux comes during a
solar minimum, when the heliospheric magnetic field allows
better access to the inner heliospheric through gradient and
curvature drift of cosmic rays.(Jokipii et al 1977., Heber et
al 2009., Tiwari, et. al.,2014)
In a magnetic epoch like at present, when the
larged-scale solar magnetic fields are directed inward in the
north, we expect a more peaked time- profile for positive
charged GCRs. In contrast we expect a wider peak in the
time profile of positive charged GCRs in epochs when the
larged-scale solar magnetic field are directed outward is
north ( similar as 1970s &1990s). The reduction in
heliospheric flux and GCR drift patterns have caused the
extended solar minimum to be both elevated in dose rate &
prolonged compared to previous solar minimum this
provides optional conditions for the measurements of GCR(
Schwadron et. al.,2010, Zhao et. al.,2011 )
II. METHODLOGY
Data from three neutron monitor have been used for analysis
together with solar, IMF, solar wind, geomagnetic data from
internet sources (htpp://www.sec.noaa.gov/ace/)and
(ftp://ftp.ngdcnoaa.gov/stp/geomagnetic.data/). All results
on cosmic ray variation are obtained and analysis based on
the original sophisticated method.
Fig. 1: Monthly mean sunspot number and 10.7cm solar
radio flux with monthly mean of Kp and Ap during solar
cycle 23
Fig. 2: Monthly mean count rate of CRI (Keil-red,Moscow-
violet,Oulu-Green)with Kp and Ap during solar cycle 23
0
10
20
30
40
50
0
50
100
150
200
250
300
Kp&Ap
SSN&10.7cm
Year
0
10
20
30
40
50
0
2000
4000
6000
8000
10000
12000
199619971998199920002001200220032004200520062007200820092010201120122013
Kp&Ap
CRI
(Kiel,Oulu,Moscow)
Kiel
Oulu
Moscow
Kp
Ap

2. Solar Interplanetary and Geomagnetic Activity in Solar Cycle 23
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Fig. 3: Monthly mean count rate of CRI (Keil-red,Moscow-
violet,Oulu-Green)with sunspot number and 10.7cm solar
radio flux during solar cycle 23
Fig. 4: Correlation with monthly mean sunspot number with
monthly mean of Kp and Ap during solar cycle 23
Fig. 5: Correlation with monthly mean sunspot number with
monthly mean count rate of CRI (Moscow-red,Oulu-blue)
during solar cycle 23
III. RESULT AND DISCUSSION
The cycle is characterized by an abrupt decrease of the
fluences (total daily fluxes) of energetic particles (>2Mev)
.The sun is entering a period of intermediate and small solar
activity cycles, comparatively about 5 to 6 solar cycle (60-
70 years).The decrease in the flare activity resulted in a
considerable increase in the number of days with quiet
geomagnetic conditions. A decrease in the number of active
regions may result in an increase in the number of coronal
holes and consequently, in the number of recurrent high
velocity solar wind streams, which will cause relative in the
number of recurrent minor geomagnetic disturbance in the
earth environment. A significant decrease in the number of
flare events will result in a decrease in the number of
stranger sporadic geomagnetic disturbance conditions .The
weaker solar magnetic field will result in the shrinking,
galactic cosmic rays modulation 2006 in the interplanetary
space & in a significant increased in their intensity thought
the entire solar cycle, not only during the epoch of solar
minimum.
IV. CONCLUSION
The solar cycle 23 is characterized by an abrupt decrease of
total daily fluxes of energetic particles (>2Mev) .The sun is
entering a period of intermediate and small solar activity,
comparatively about 5 to 6 solar cycles .The decrease in the
flare activity resulted in a considerable increase in the
number of days with quiet geomagnetic conditions, and a
decrease in the number of active regions may result in an
increase in the number of coronal holes and consequently in
the number of recurrent high velocity solar wind streams,
which will cause relative in the number of recurrent minor
geomagnetic disturbance in the earth environment. A
significant decrease in the number of flare events will result
in a decrease in the number of sporadic geomagnetic
disturbance conditions. The weaker solar magnetic field will
result in the shrinking, galactic cosmic rays modulation
2006 in the interplanetary space & in a significant increased
in their intensity thought the entire solar cycle, not only
during the epoch of solar minimum.
REFERENCES
[1] J.R. Jokipii, E.H.Levy and W.B.Hubbard(1977),
“Effect of particle drift on cosmic –ray transport.”
Astro Phys. J.213,861-868
[2] B.Heber, J.Kopp, J. Gieseler, R. Miiller-Mellin,
H.Fichtner, K.Scherer, M.S.Potgieter, and
S.E.Ferreira(2009) “ Modulation of galactic cosmic
ray protons and electrons during an unusual solar
minimum.” Astrophys. J., 699,1956-1963,
doc:10.1088/0004-637X/699/2/1956
[3] B.K.Tiwari., B.R.Ghormare., P.K.Shrivastava.,
D.P.Tiwari.“ Modulation in Cosmic ray During the
Declining and Minimum Solar Activity Period of
Solar Cycle 23”. Res. J. Physical Sci. Vol. 2(2), 9-12,
(2014)
[4] N.A.Schwadron., A.J.Body., K.Kozarev.,
M.Golightly., H.Spence., L.W.Townsend.,and
M.Owens.“ Galactic cosmic ray radiation hazard in
the unusual extended solar between solar 23 and 24.
Space Weather”, Vol.8, S00E04,
doi:10.1029,2010SW000567,(2010)
[5] Zhao,L.,Fisk,L., “Understant the behavior of the
heliospheric magnetic field and the solar wind
during the unusual solar minimum between cycle
23 and 24”.Solar Phys.274,379, (2011)
[6] B.K.Tiwari., B.R.Ghormare., P.K.Shrivastava.,
D.P.Tiwari.“ Study of variation in Cosmic ray
Intensity due to Solar-Interplanetary activity between
1996-2013”.Res. J. Physical Sci. Vol. 2(3), 4-8,
(2014)
[7] B.K.Tiwari., B.R.Ghormare., P.K.Shrivastava.,
D.P.Tiwari.“Dependence of the Helioshphere and
Cosmic ray (CR) Modulation on Solar activity”. Res.
J. Physical Sci. Vol. 2(5), 8-11, (2014)
0
100
200
300
0
5000
10000
15000
199619971998199920002001200220032004200520062007200820092010201120122013
SSN&10.7cm
CRI
(Kiel,Oulu,Mosc
ow)
0
20
40
60
0 100 200
Kp&Ap
SSN
Kp
Ap
Linear (Kp)
Linear (Ap)
4000
6000
8000
10000
12000
0 100 200
CRI(Oulu&
Moscow)
SSN
Oulu
Moscow
Linear (Oulu)