- Letter
- Open Access

# Methods of analysis of geomagnetic field variations and cosmic ray data

- Oksana V Mandrikova
^{1, 2, 3}Email author, - Igor S Solovev
^{1, 2, 3}and - Timur L Zalyaev
^{1}

**66**:148

https://doi.org/10.1186/s40623-014-0148-0

© Mandrikova et al.; licensee Springer. 2014

**Received:**31 March 2014**Accepted:**29 October 2014**Published:**21 November 2014

## Abstract

In the present paper, we propose a wavelet-based method of describing variations in the Earth’s magnetic field, such as the horizontal component of the geomagnetic field, in addition to methods for evaluating changes in the energy characteristics of the field and for isolating the periods of increased geomagnetic activity. Based on a combination of multiresolution wavelet decompositions with neural networks, we propose a method of approximation of the cosmic ray time course and the allocation of anomalous variations (Forbush effects) that occur during periods of high solar activity. During the realization of the method, an algorithm was created for selecting the level of the wavelet decomposition and adaptive construction of the neural network. By using the proposed methods, we performed a joint analysis of the geomagnetic field and cosmic rays during periods of strong magnetic storms. The strongest geomagnetic field perturbations were observed in periods of abnormal changes in cosmic ray level. Assessment of the intensity of geomagnetic disturbances on the eve of and during magnetic storm development allowed us to highlight local increases in intensity of the geomagnetic field occurring at different frequency ranges prior to the development of the storm’s main phase. Implementation of the proposed method with theoretical tools in combination with other methods will improve the estimation accuracy of the geomagnetic field state during space weather forecasting.

## Keywords

- Geomagnetic field
- Cosmic rays
- Wavelet transform
- Neural networks
- Magnetic storms

## Findings

### Introduction

The present study examines the processes that occur in circumterrestrial space during magnetic perturbations by creating new algorithms and techniques for recognition, analysis, and interpretation of data. During perturbed periods, parameters determined by special equipment include a complex non-stationary structure that contains non-smooth local features arising at random time points that carry information about the processes under study. A lack of theoretical basis for providing adequate presentation of data for analysis leads to inevitable loss and distortion of information and requires the application of contemporary techniques such as pattern recognition and digital signal processing (Nayar et al. [2006]; Hafez et al. [2013]; Xu et al. [2008]; Jach et al. [2006]; Paschalis et al. [2013]; Macpherson et al. [2001]; Woolley et al. [2010]; Soloviev et al. [2012]; Rotanova et al. [2004]).

During periods of magnetic storms in the recorded geomagnetic data, variations occur among frequency ranges. The emerging local structures are determined by field perturbations and reveal the intensity and nature of the development of a magnetic storm. The complex structure of geomagnetic data limits the abilities of spectral analysis methods by failing to provide information on the local changes occurring in the physical process and their scale characteristics.

The disadvantages of these methods also include limitations in identifying and interpreting hidden patterns in the behavior of the data. In the present study, wavelet transform is suggested for analysis of geomagnetic data because such methods allow detection of several interesting deterministic and more stochastic features in the time series of solar activity indicators (Lundstedt et al. [2005]). Wavelet transform is the underlying mathematical tool used for analyzing local features occurring in the geomagnetic field during intense solar flares (Ivanov et al. [2001]; Rotanova et al. [2004]; Nayar et al. [2006]) and for developing algorithms for automatic determination of the onset of a magnetic storm (Hafez et al. [2013]). Furthermore, the wavelet transform is a powerful tool for eliminating noise and excluding the periodic component caused by the Earth’s rotation (Xu et al. [2008]; Jach et al. [2006]). A method used for allocation of anomalies in geomagnetic data was developed on the basis of the wavelet transform (Zaourar et al. [2013]). The authors of the present paper created technology for automatic extraction of the unperturbed level of the horizontal component of the geomagnetic field based for the first time on wavelet transform (Mandrikova et al. [2013]). This method has significantly reduced error in automatic calculation of the K-index in comparison to the adaptative smoothing method (KASm) recommended by the International Real-Time Magnetic Observatory Network (Intermagnet) and currently used by Paratunka Observatory, Kamchatka Region, Institute of Cosmophysical Researches and Radiowave Propagation, Far Eastern Branch of the Russian Academy of Sciences (IKIR FEB RAS), and Yakutsk Observatory, Yakutsk, Institute of Cosmophysical Research and Aeronomy, Siberian Branch, Russian Academy of Sciences (IKFIA SB RAS). In the present paper, the authors suggest a new technique for determining variation in the geomagnetic field by using the H-component and present related methods of extracting geomagnetic perturbations, estimating their intensity, and determining periods of increased geomagnetic activity. The suggested theoretical tools can be implemented in the automatic mode, which is close to the real-time mode and can be adapted to various magnetic observatories.

The topology of the geomagnetic field during magnetic storms is characterized by variability of cosmic rays on the Earth’s surface (Kozlov and Markov [2007]), which present an integral result of various solar, heliospheric, and atmospheric phenomena with a complex structure. The most substantial changes in cosmic ray parameter are caused by emissions of the corona substance and subsequent changes in parameters of the interplanetary field and solar wind (Vecchio et al. [2012]). The current study of the dynamics of cosmic ray flux includes methods of adaptive approximation, wavelet transform, and neural networks. Using neural networks for the primary processing of neutron monitor data have led to greater efficiency in the noise reduction procedure compared with median methods (Paschalis et al. [2013]). Neural networks also can be used to detect abnormal features in complex functions. For example, the method of automatic detection of sudden commencement is based on neural networks (Segarra and Curto [2013]). Based on a combination of wavelet transform and empirical mode decomposition, the dominant temporal scales of long-term temporal variation of cosmic rays were highlighted for periods of 11, 22, and 6 years and biennial oscillation, and their physical nature was determined (Vecchio et al. [2012]). In the present study, the authors combine multiscale wavelet transforms and neural networks to develop a technique for approximating the time variation of cosmic rays and discovering anomalous changes connected with increased solar activity.

This method enables noise suppression to distinguish characteristic variations and to examine the details of their structures.

On the basis of the proposed methods, we have performed joint analysis of the geomagnetic field and cosmic rays during periods of strong magnetic storms on 5 to 7 April 2010 and 5 September 2012. During the analysis, we used 1-min geomagnetic field data from Intermagnet (www.intermagnet.org) and 1-min neutron monitor data obtained within the framework of the Real-time Neutron Monitor Database (NMDB) (www.nmdb.eu/) project.

## Description of methods

### Decomposition of time series into components based on wavelet transform

*f*

_{ j }(i.e., values of the function at the grid with a resolution of 2

^{−j}), we can consider the following subspace as the sampling space:

where *V*_{
j
} is generated by translation and dilation of *the scaling function ϕ* (Daubechies [1992]; Chui [1992]; Mallat [1999]), and *L*^{2}(*R*) is the Lebesgue space.

*f*

_{ j }into spaces

*V*

_{j −1}and

*W*

_{j −1}, we obtain (Daubechies [1992]; Chui [1992]; Mallat [1999])

where ⊕ denotes the orthogonal sum. The set of functions (wavelets) *Ψ*_{j,n} =2^{j/2}*Ψ*(2^{
j
}*t* − *n*), *n* ∈ *Z* form the basis of the space *W*_{
j
}.

*f*

_{ j }as time series. On the basis of Equation 2, the time series can be represented as:

Each component of the series ${f}_{j-1}\left(t\right)={\displaystyle \sum _{n}}{c}_{n}^{j-1}{\Psi}_{j-1,n}\left(t\right)$ and ${g}_{j-1}\left(t\right)={\displaystyle \sum _{n}}{d}_{n}^{j-1}{\Psi}_{j-1,n}\left(t\right)$ in Equation 3 is uniquely defined by the sequence of coefficients ${\overline{c}}^{j}={\left\{{c}_{j,n}\right\}}_{n\in Z}\in {V}_{j}$ and ${\overline{d}}^{j}={\left\{{d}_{j,n}\right\}}_{n\in Z}\in {W}_{j}$: *c*_{j,n} = 〈*f*, *ϕ*_{j,n}〉, *d*_{j,n} = 〈*f*, *Ψ*_{j,n}〉.

The described computational procedure is known as a wavelet decomposition algorithm, which can be applied to any resolution (scale) *j* of the signal (Daubechies [1992]; Chui [1992]; Mallat [1999]).

*f*

_{ j }(

*t*)

*m*times, we obtain the following form of the decomposition of the space

*V*

_{ j }:

*f*

_{ j }(

*t*) can be represented as the sum of the components listed below:

Component *g*_{
j
} is known as a *detailed (high-frequency)* component of the time series; component *f*_{j − m} is known as the smoothed component of the time series.

In the wavelet transform theory, decomposition of the form in Equation 5 is known as *multiresolution wavelet decomposition to the level m* (Chui [1992]; Mallat [1999]).

*W*

_{ j }, we obtain a partition of the high-frequency components, which allows us to identify different types of time-frequency structures. In the wavelet transform theory, decomposition of

*f*

_{ j }based on recursive splitting of the spaces

*V*

_{ j }and

*W*

_{ j }is known as

*the wavelet packet*decomposition. Graphic representation of wavelet packet decomposition of the time series

*f*

_{ j }is shown in Figure 1.

### Description of geomagnetic field variations on the basis of wavelets

*f*

_{ j }(

*t*), we could consider the time variation of the horizontal component of the geomagnetic field. Without loss of generality, we assume that

*j*= 0, i.e., the space of initial data is ${V}_{0}={\mathrm{clos}}_{{L}^{2}\left(R\right)}\left(\varphi \left({2}^{0}t-n\right)\right)$. Based on the wavelet packet decomposition, we obtain the following representation of

*f*

_{0}(

*t*):

where *I* is a set of indices.

*g*

_{ j }(

*t*) on the scale

*j*(Mandrikova et al. [2013]; Mandrikova and Solovev [2013]). We used the following criteria to determine the set of indices

*I*(Mandrikova et al. [2013]):

where *m* is the sample mean, *v* is the index of disturbed field variation, *k* is the index of calm field variation, and *ε* is a positive number.

Assuming that variable *A*_{
j
}^{
k
} is normally distributed with some mean *μ*^{
k
} and variance *σ*^{2,k}, it is possible to estimate *ε* as $\widehat{\epsilon}={x}_{\frac{1-\alpha}{2}}\sqrt{{\sigma}^{2,k}}$, where ${x}_{\frac{1-\alpha}{2}}$ is the $\frac{1-\alpha}{2}$ quantile of standard normal distribution.

Estimation of the set of indices *I*, particularly for the station Paratunka (Kamchatka Region), was performed using geomagnetic data for 2002, 2005, and 2008, containing 63 disturbed field variations and 64 calm field variations.

Let us consider three possible states of the geomagnetic field: state *h*_{0}: calm field; state *h*_{1}: weakly perturbed field; state *h*_{2}: perturbed field. According to the proposed field states, we introduce the following states of the coefficients *d*_{j,n} on the scale *j*:

*h*_{
j
}^{0}: calm coefficient

*h*_{
j
}^{1}: weakly perturbed coefficient

*h*_{
j
}^{2}: perturbed coefficient.

*a measure of magnetic disturbance*of the coefficient, it is logical to determine its amplitude. Then, in accordance with the introduced states of the coefficients from Equation 6, we obtain the following representation of geomagnetic field variations:

where component ${g}_{1}\left(t\right)={\displaystyle \sum _{j,n}}{F}_{1}\left({d}_{j,n}\right){\Psi}_{j,n}\left(t\right)$ describes weak geomagnetic perturbations, where the coefficients of *g*_{1}(*t*) are in a weakly perturbed state; component ${g}_{2}\left(t\right)={\displaystyle \sum _{j,n}}{F}_{2}\left({d}_{j,n}\right){\Psi}_{j,n}\left(t\right)$ describes strong geomagnetic perturbations, where the coefficients of *g*_{2}(*t*) and *T*_{j,1} > *T*_{j,2} are in a perturbed state; and coefficients *d*_{j,n}, where |*d*_{j,n}| ≤ *T*_{j,1} is considered as quiet.

Threshold functions *F*_{0}(*x*), *F*_{1}(*x*), and *F*_{2}(*x*) in Equation 9 determine rules for decision-making of coefficient state.

Threshold *T*_{j,1} and *T*_{j,2} divide the space of coefficients *X* into three disjoint regions *X*_{0}, *X*_{1}, and *X*_{2}. Then, the rule of decision-making establishes a correspondence between decisions of the state of coefficients and regions.

*h*

_{ j }

^{ i }, the average value of the loss can be defined as (Levin [1963])

where *Π*_{
il
} if loss function, $P\left\{x\in {X}_{l}/{h}_{{j}_{\mathrm{dist}},i}\right\}$ is the conditional probability that the sample falls into the area *X*_{
l
} if the real state is *h*_{
j
}^{
i
}, *i* ≠ *l i. l* is the state of indices, where sign ‘/’ means conditional probability.

*h*

_{ j }

^{ i },

*i*= 0, 1, 2, we obtain average risk (Levin [1963]):

where *p*_{
i
} is the a priori probability of the state *h*_{
j
}^{
i
}.

The best rule is the one for which the average risk is smallest (Levin [1963]).

Since we did not know the a priori distribution of states *p*_{
i
}, we used a posteriori risk for choosing the best decision rule (Levin [1963]). Posterior probabilities *P*{*h*_{
j
}^{
i
}/*x*}, *i* = 0, 1, 2, represent the most complete characterization of the states *h*_{
j
}^{
i
} with available priori data.

*J*

_{ l }(

*x*) is

In this case, the criterion of the quality of decision-making is the criterion of the lowest error rate.

Thresholds *T*_{j,1} and *T*_{j,2} are determined by best decision rule of the decision-making, ensuring the lowest value of the posterior risk *J*_{
l
}(*x*).

*J*

_{ l }(

*x*), we determine thresholds

*T*

_{j,1}and

*T*

_{j,2},

*j*∈

*I*for regions of Kamchatka and Yakutsk (Mandrikova et al. [2013]; Mandrikova and Solovev [2013]). The criterion of assessment of the coefficients is the K-index (Bartels et al. [1939]). The following assessments were considered:

- 1)
Coefficient belongs to area

*X*_{0}(i.e., they are in a quiescent state) if the current value of the K-index is 0 or 1; - 2)
Coefficient belongs to area

*X*_{1}(i.e., they are in a weakly perturbed state) if the current value of the K-index is 2, 3, or 4; - 3)
Coefficient belongs to area

*X*_{2}(i.e., they are in a perturbed state) if the current value of the K-index is more than 4.

The introduced states of coefficients describe the states of the geomagnetic field and their assessment based on the obtained rule for decision-making, which allows us to register moments of increasing geomagnetic activity. In our previous paper (Mandrikova et al. [2013]), we developed an automatic algorithm to construct the Sq-curve and to calculate the K-index on the basis of this representation of geomagnetic field variations (shown in Equation 8), and we demonstrated that its application for stations Paratunka and Yakutsk significantly reduced the error of K-index computation in the automatic mode, in comparison with the methodology used in the Intermagnet network stations. In the present work (‘Assessment of changes of energy characteristics of the field and the allocation of periods of increased geomagnetic activity’ subsection), we used this approach to suggest computational solutions for estimating changes in the energy characteristics of the field and the allocation of periods of increased geomagnetic activity. To obtain more detailed information on the state of the geomagnetic field, we used continuous wavelet transform.

### Assessment of changes of energy characteristics of the field and the allocation of periods of increased geomagnetic activity

Since wavelet *Ψ* has a zero mean, coefficients (*W*_{
Ψ
}*f*) (*b*, *a*) describe the properties of the function *f* in the neighborhood *b* when the scale *a* tends to be zero. This property of the continuous wavelet transform allows us to obtain detailed information on the local properties of the function *f*.

*t*=

*b*on the scale

*a*. This intensity can be written as:

*e*

_{b,a}, we can estimate the state of the coefficients and allocate time-frequency intervals containing weak and strong geomagnetic disturbances on the analyzed scale

*a*:

where the threshold *T*_{a,1} allows to us allocate weak and strong perturbations, and the threshold *T*_{a,2} indicates strong perturbations.

*t*=

*b*is

*T*

_{a,1}and

*T*

_{a,2}by minimizing a posteriori risk, in accordance with rule of decision-making introduced in ‘Description of geomagnetic field variations on the basis of wavelets’ subsection.

*K-index was the criterion of estimation of the state of coefficients*, where the data used was from stations Paratunka, Yakutsk, and Novosibirsk. Analysis of Figure 3 shows the complex multiscale nature of the process. The results of processing of the data allow us to allocate its general features. Prior to the beginning of the storm, from about 09:00 to 10:40 UT and 21:30 to 23:30 UT on 23 June and from 02:00 to 03:30 UT on 24 June, local increases in the intensity of geomagnetic disturbances were observed at all analyzed stations, and periods of weak geomagnetic activity had been formed. Simultaneous occurrence of disturbances at different stations eliminates the influence of the noise factor and confirms their solar nature. The strongest field perturbations observed from 4:57 to 06:43 UT coincide with the moments of the main phase of the storm.

### Method of approximation of the time variation of cosmic rays and allocation of anomalous changes in its dynamic on the basis of combination of multiresolution wavelet decompositions and neural networks

We consider the time variation of cosmic rays as *f*_{
j
}(*t*). Let us assume that the initial data space is ${V}_{0}={\mathrm{clos}}_{{L}^{2}\left(R\right)}\left(\varphi \left({2}^{0}t-n\right)\right)$ (i.e., *j* = 0).

*f*

_{0}(

*t*) to the level

*m*, we obtain its representation in the following form (see Equation 5):

where the upper index (−*m*) corresponds to the resolution of the component before the operation of the wavelet reconstruction.

To construct the mapping, we used a feedforward neural network with variable structure, which is a network in which the structure is determined by minimizing the error on the training set. The training set is formed from the data registered during quiet periods. In this case, the trained neural network reproduced regular variations of the data being approximated, which is typical for quiet conditions. Network training was performed on the basis of the back error propagation algorithm (Haykin [1999]).

If in constructed mapping, ${\widehat{f}}_{0}^{*\left(-m\right)}$ is the actual output of the network and *f*_{0}^{*(−m)} is desired, then *f*_{0}^{*(−m)} = *y*(*f*_{0}^{(−m)}) is an unknown function, and ${\widehat{f}}_{0}^{*\left(-m\right)}$ is its approximation, which is reproduced by the neural network. The advantage of the neural network representation of the approximated function is greater flexibility of the basic functions and their ability to adapt (Haykin [1999]). When the input of the trained network is the function values from the interval [*t*_{
n
} − *Q* +1, *t*_{
n
}], the network is able to calculate the preemption of its value in the time interval [*t*_{
n
} +1, *t*_{
n
} + *I*], where *t*_{
n
} is the current discrete time, and *I* is the length of the preemption interval.

*Network error*(approximation error) at time moment

*t*

_{ n }is determined as the difference between the desired

*f*

_{0}

^{*(−m)}and actual ${\widehat{f}}_{0}^{*\left(-m\right)}$ output values of the function:

where *i* is the step of the feedforward network of the data, and square brackets denote the discrete time.

The algorithm for constructing the network and choosing the level of the wavelet decomposition, based on minimization of the approximation error, is listed below.

where *U* is the length of the observation window, and *T* is a preassigned threshold.

### Algorithm for constructing a neural network and choosing the level wavelet decomposition

Step 1. We obtain representation of a smoothed component of the series in the form${f}_{0}^{\left(-m\right)}\left(t\right)={\displaystyle \sum _{n}}{c}_{0,n}^{\left(-m\right)}{\varphi}_{0,n}\left(t\right)$, where *m* = 1.

Step 2. Data array {*c*_{0,n}^{(−m)}}_{n=1}^{
N
}, where *N* is the array length and is divided into blocks of {*c*_{0,n}^{(−m)}}_{n=1}^{
Q
}, {*c*_{0,n}^{(−m)}}_{n=2}^{Q+1}, …, {*c*_{0,n}^{(−m)}}_{n=N−Q+1}^{
N
}. The block length is *Q* = 6.

Step 3. From these data blocks, we form a training matrix with the dimensions of *Q* × *V*, where *Q* is the length of the input vector of the network and *V* is the number of training vectors.

Step 4. We build a network with a variable structure.

where *ɛ*_{
i
}^{(−m)}[*l*] = *ĉ*_{0,l}^{i,(−m)} − *c*_{0,l}^{i,(−m)} is network error at a discrete moment of time *l* in *i* steps of preemption, where *c*_{0,l}^{i,(−m)} is desired; *ĉ*_{0,l}^{i,(−m)} is the actual output value of the network at a discrete moment of time *l* in *i* steps of preemption; *I* is the length of the output vector network; and *L* is the length of the array of test data.

Step 6. We estimate the difference: *Δ* = *E*_{
m
} − *E*_{m −1}. If *Δ* < = 0, then go to step 7. If *Δ* >0, then the required level of decomposition is *m** = *m* −1, and we do not perform step 7.

Step 7. If *m* ≤ log_{2}*N*, where the maximum allowable level of decomposition *M* is determined by the length of the array data *N*: *M* ≤ log_{2}*N*, we increase by 1 level of the decomposition (*m* = *m* +1) and perform steps 2 to 5. If *m* > log_{2}*N*, then *m** = *m* is the desired level of decomposition.

### Choice of wavelet

*f*

_{0}(

*t*) (Equation (18)) was performed using a wavelet from the coiflets family. Coiflets are orthogonal functions that support the smallest size with a sufficient number of zero moments in the scaling function

*ϕ*(Daubechies [1992]):

*f*belongs to

*C*

^{ r }, which is the space of

*r*times of continuously differentiable functions, in the neighborhood of 2

^{−m}

*n*with

*r*≤

*p*, then:

However, the order of approximation increases with the growth of *p*, resulting in coiflets that support size 3*p* −1.

Approximation of the data of cosmic rays with the least error was obtained by using coiflets with *p* = 3.

Based on the proposed method, we constructed neural networks for stations Novosibirsk, Athens, Apatity, and Cape Schmidt, which approximate time variations of the smoothed component of cosmic rays and uses the neutron monitor data. To train the networks, we used minute data for the period from 2005 to 2013 years. Cosmic ray variations are influenced by electromagnetic conditions in the solar system; therefore, we used geomagnetic field data as an indicator of anomalous behavior of these conditions. Thus, the training set of neural networks was formed from data registered during periods of quiet geomagnetic field (Akasofu and Chapman [1972]; Bishop [1995]; Rybàk et al. [2001]).

To consider the changes in the level of solar activity, the training of neural networks is performed separately for each year (Kóta and Somogyi [1969]; Kudela et al. [1999]; Rybàk et al. [2001]). The level of the model time series depends on the training sample. The increase in the absolute value of the error of the trained neural network indicates a change in the internal structure of the time series and the occurrence of anomalies in cosmic rays.

where *ω*_{
βn
}^{1} is the weight of neuron *β* of the input layer of the network, *ω*_{
φβ
}^{2} is the weight of the neuron *φ* of the hidden layer of the network, *ω*_{
χφ
}^{3} is the weight of a neuron *χ* of the output layer of the network, and ${\alpha}_{\beta}^{1}\left(z\right)={\alpha}_{\phi}^{2}\left(z\right)=\frac{2}{(1+exp\left(-2z\right))}-1,{\alpha}_{\chi}^{3}\left(z\right)=a\times z+b,j=-5\text{.}$

## Experimental results

The first analyzed magnetic storm was registered on Earth on 5 April 2010, at 08.26 UT, as the sudden commencement (SC) of the magnetic storm. The speed of the solar wind had increased to 750 to 900 km/s. A globally observed intense substorm emerged 30 min later in the Earth’s magnetosphere (Kleimenova et al. [2013]).

Analysis of Figures 5 and 6 reveals that a local decrease of the level of cosmic rays occurred simultaneously with an increase of geomagnetic disturbance intensity. The error of neural networks increased fourfold at the Athens station and 2.5 times at the Novosibirsk station in comparison with the quiet period. Decreases in the level of cosmic rays at both stations were accompanied by the most severe disturbances of the geomagnetic field. However, variations of cosmic rays had different behaviors. At the Athens station, a short Forbush effect with rapid recovery peaked at 20:00 UT, in which the neural network error increased in threefold in comparison with the quiet period. At the Novosibirsk station, the Forbush effect was longer and peaked at 16:00 UT; the neural network error increased tenfold in comparison with the quiet period. The intensity of the geomagnetic field disturbances reached maximum values during 9:26 to 10:07 UT.

The second analyzed magnetic storm was recorded on Earth on 5 September 2012. The polar wind velocity reached values of 500 to 600 km/s due to the arrival of the accelerated flow from the coronal mass ejection (CME) that occurred on 2 September 2012. Detailed analysis of Figures 7 and 8 reveals that local increases in intensity of geomagnetic disturbances emerged at the analyzed stations in different frequency ranges and that periods of weak geomagnetic activity had been formed on the eve of storm (approximately 06:00 to 08:00 UT, 10:30 to 12:30 UT, and 17:00 to 18: 00 UT on 4 September and from 22:00 UT until the start of the storm). The arrival of the shock wave occurred at 1:00 UT on 5 September, and both stations simultaneously recorded the beginning of the Forbush effect; an increase in the error of the neural network was recorded at the Novosibirsk station. Maximal values of intensity field disturbances were recorded on 5 September during 6:43 to 6:48 UT, which coincides with the periods of strong geomagnetic activity. At the Novosibirsk station, the maximum of the lowering of the level of cosmic rays and neural network error had increased in ten times in comparison with the quiet period. It should be noted that the Forbush effect registered at the Athens station was short, and the cosmic ray level recovered fast, whereas the Forbush effect registered at Novosibirsk station was more extended.

## Conclusions

We proposed a model of geomagnetic field variations that allows us to describe the tranquil dynamics and disturbances occurring in periods of increased geomagnetic activity. On the basis of this model, we developed methods for assessing changes in energy characteristics of the field and allocation of periods of weak and strong geomagnetic activity. The analysis showed that in periods of increased geomagnetic activity, the developed tools allowed us to record the onset of geomagnetic disturbances and to receive quantitative estimates of the power of the geomagnetic field disturbance. Such applications allowed us to perform detailed analysis of geomagnetic field variations for different registration stations during strong magnetic storms.

A slight increase in geomagnetic activity, which is associated with the approaching storm, was observed in different frequency ranges at local moments on the eves of storms.

Moreover, we proposed methods of approximation of the time variation of cosmic ray data and allocation of anomalous changes occurring during periods of high solar activity. The methods for Novosibirsk, Athens, Cape Schmidt, and Apatity stations were built in neural networks that approximate the time variation in the smoothed component of the cosmic rays. In the training of the networks, we used data recorded in 2005 to 2013. This method allowed us to study the structure of the data of cosmic rays in detail and to allocate abnormal changes in their dynamics during periods of the Forbush effects.

Joint analysis of the data of the geomagnetic field and cosmic rays in the periods of strong magnetic storms showed that the strongest geomagnetic field perturbations were observed in periods of anomalous changes in the dynamics of cosmic rays and could be registered on the basis of the proposed applications.

Future plans include adaptation of the developed tools for a larger number of registration stations and creation of an integrated software environment that would provide the possibility of spatio-temporal data analysis in an online mode.

## Declarations

### Acknowledgements

This research is supported by a grant of Russian Academic Fund No. 14-11-00194. We thank researchers of the NMDB project (www.nmdb.eu/) for providing high-resolution neutron monitor data and those at Intermagnet (www.intermagnet.org) for promoting high standards of magnetic observatory practices.

## Authors’ Affiliations

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