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# Analysis of temporal–longitudinal–latitudinal characteristics in the global ionosphere based on tensor rank-1 decomposition

- Shikun Lu
^{1, 2}View ORCID ID profile, - Hao Zhang
^{1}Email author, - Xihai Li
^{2}, - Yihong Li
^{2}, - Chao Niu
^{2}, - Xiaoyun Yang
^{2}and - Daizhi Liu
^{2}

**Received:**17 October 2017**Accepted:**23 February 2018**Published:**14 March 2018

## Abstract

## Keywords

- Large-scale ionospheric characteristics
- Tensor rank-1 decomposition
- Time lags
- Geomagnetic north–south asymmetry

## Introduction

Known as the ‘space weather display,’ the ionosphere is an important part of the Sun–Earth system. Ionospheric characteristics can reflect both variations in the solar-terrestrial environment and solid Earth and atmosphere (Afraimovich et al. 2006; Yoshikawa et al. 1999). With advances in information technology, radio waves have become a significant carrier for information. Due to the ionospheric influence on radio wave propagation, the impact of the ionosphere on people’s lives is increasing. Both national security, e.g., space-borne synthetic-aperture radar system (Tsynkov 2009) and over-the-horizon radar (Hu et al. 2016), and people’s lives, e.g., GPS position and high-voltage networks (Liu et al. 2013), are closely related to the ionosphere. As a result, ionospheric research is of great value for both theory and application.

Extensive research has been conducted regarding ionospheric spatial and temporal characteristics. With the help of the space technology, especially GPS, researchers have gained insight into the shape and behavior of the ionosphere. However, conventional research usually focuses on temporal and spatial variations separately. Ren et al. (2008) examined the electron temperature and total ion density in the sunset equatorial topside ionosphere and found clear seasonal dependence and significant anti-correlation using the longitudinal variations in ionosphere. Mu et al. (2010) analyzed the correlation between ionospheric longitudinal harmonic components (WN3 and WN4) and upper atmospheric tides. They found that atmospheric tidal DE2 and DE3 patterns were important factors in the ionospheric WN3 and WN4 structures. Kil and Paxton (2011) reviewed the causal link between longitudinal plasma density structure, vertical plasma drifts, and atmospheric tides. These previous studies only focused on longitudinal variations. Xu et al. (2013) investigated the influence of declination and thermospheric wind on longitude differences in midlatitude ionospheric total electron content (TEC) by analyzing the data distributed on both sides of the longitudes with zero declination. Wang et al. (2015) and Wang and Zhang (2017) studied the longitudinal and diurnal differences in midlatitudinal electron density from a global perspective using the global ionosphere–thermosphere model. They quantified the effects from in-situ physical processes and atmospheric tides from the low atmosphere. These researchers studied spatial variations in the ionosphere, ignoring temporal variations by fixing or removing them. Other studies have only focused on the temporal variation of the ionosphere, such as the seasonal and diurnal changes (Liu et al. 2009; Lee et al. 2011; Coyne and Belrose 1972; Wright 1962). Roughly compressing the data in one certain dimension results in loss of information in other dimensions or coupling between dimensions. Identical to matrix analysis, compared to eigenvectors obtained from the singular value decomposition, one column or row contains much less information than the matrix.

Some research has been made to jointly analyze temporal and spatial variations. Wen et al. (2007) investigated ionospheric temporal and spatial variations during the August 18, 2003, storm over China to reveal ionospheric storm evolution processes using time series ionospheric electron density maps. Yao et al. (2013) conducted research on temporal and spatial variations in ionospheric electron density profiles over South Africa during strong geomagnetic storms using the 3D structure of ionospheric electron density and its response to geomagnetic storms. Essentially, both research groups tried to analyze the spatiotemporal variations with a time series of spatial variation results. However, spatial and temporal variations of the ionosphere are correlated (Talaat and Zhu 2016). Therefore, this strategy cannot provide deep insight into spatiotemporal variations in the ionosphere. By formulating statistics using separate bins, Araujo-Pradere et al. (2005) determined that ionospheric variability for quiet and disturbed conditions is a function of local time, geomagnetic activity, season, and geomagnetic latitude. In their research, the data were divided into different bins that disregarded the coupling between factors. For example, for seasonal dependence, the data were simply divided into five seasonal bins, regardless of spatiotemporal coupling. Afraimovich et al. (2008) found that Global Electron Content (GEC) well reflected Sun dynamics. However, GEC is calculated by the summation of the global TEC, removing spatial information. Lean et al. (2016) studied the distinctive spatial patterns of TEC response to solar, seasonal, diurnal, and geomagnetic influences using a new statistical model based on the linear summation of different influences, but this also neglects the coupling between them. Consequently, the strategy, separately analyzing or roughly compressing the spatial and temporal characteristics, may destroy the spatiotemporal coupling. However, research has been conducted to address this issue. Chen et al. (2015) illustrated the importance of different types of spatial-temporal variations to the TEC over North America using the empirical orthogonal function (EOF). Talaat and Zhu (2016) analyzed the spatial and temporal variation of total electron content revealed by principal component analysis (PCA). Although these studies can separate spatial and temporal variations, they cannot separately provide detailed spatial information on variations in longitude and latitude. Generally, previous research on ionospheric spatiotemporal variations has not decoupled correlations in time, longitude, and latitude and has not truly combined analyses of these three modes simultaneously.

Our dataset, a time series of global ionospheric maps, constitutes a data cube, represented by a third-order tensor. As an efficient method to analyze multidimensional arrays, tensor rank decomposition can be used to address multilinear algebra problems, e.g., combined analyses of time, longitude, and latitude, which would be intractable for classical techniques (Grasedyck et al. 2013). In addition, similar to the widely used methods for spatiotemporal analysis, PCA and EOF, tensor rank decomposition can also analyze different scaled features in data tensors (Filisbino et al. 2013). Notably, rank-1 decompositions can extract large-scale characteristics of time, longitude, and latitude simultaneously. In this study, we utilize GPS-derived VTEC data supplied by CODE from 2011 to 2013. We combine an in-depth investigation on the global spatial features with temporal variations in the ionosphere based on tensor rank-1 decomposition. "Description of data and methods" section provides a description of the data information and methods. The resulting ionospheric temporal–longitudinal–latitudinal characteristics are presented in "Results and discussion" section, followed by conclusions in "Conclusions" section.

## Description of data and methods

### VTEC data source

Carrying abundant information about climatological variations of the ionosphere (Ercha et al. 2015), VTEC has been extensively used to investigate the ionosphere. CODE, as one of the IGS (International Global Navigation Satellite System Service) laboratories, can supply global VTEC data with 2-h time resolution (Wei et al. 2009). The laboratory uses dual-frequency code and phase GPS data from more than 200 stations worldwide (Hernández-Pajares et al. 2009; Rao and Dutt 2014). In the current research, a global ionospheric map (GIM) is the result of VTEC data derived from CODE. The selected dataset is named after CODE (ftp://ftp.unibe.ch/aiub/CODE). The VTEC in CODE is modeled using a spherical harmonics expansion up to order 15. Simultaneously, 3328 parameters are used to represent the global VTEC distribution. As a result, the CODE dataset can provide abundant detailed ionospheric variations in both space and time.

The spatial extent of GIM ranges from \(180^{\circ }\)W to \(180^{\circ }\)E in longitude and from \(87.5^{\circ }\)S to \(87.5^{\circ }\)N in latitude. The size of a GIM cell is \(5^{\circ }\) in longitude and \(2.5^{\circ }\) in latitude. The time-varying GIMs for VTEC, 2D spatial maps, can constitute a third-order tensor by the arrangement with time.

### Tensor rank decomposition

The widespread application of multi-sensor technology and the emergence of high-dimensional datasets have highlighted the limitations of traditional flat-view matrix methods and shown the necessity of moving toward more versatile tools. High-order statistics for multivariate stochastic variables promote the development of multilinear algebra, which is the algebra of higher-order tensors. The range of applications for tensor techniques has expanded widely in signal processing and data analysis, e.g., computational tasks in electronic structure calculations and solution to stochastic and parametric partial differential equations (Grasedyck et al. 2013; Khoromskaia and Khoromskij 2014; Espig et al. 2014).

*N*is the length of tensor in

*n*th mode. \({\hat {\mathscr{ A}}}\), whose rank is

*r*, is the approximation of \({\mathscr {A}}\), and its component \(\hat{a}_{i_1i_2i_3}\) is calculated using the sum of the outer product ‘\(\circ\)’, resulting in \(\hat{a}_{i_1i_2i_3}=\sum _{k=1}^r u^{(1)}_{ki_1}u^{(2)}_{ki_2}u^{(3)}_{ki_3}\). \(||\cdot ||_F\) is the Frobenius norm. Essentially, this decomposition tries to find a rank-

*r*tensor to approximate the data tensor, based on the condition that the Frobenius norm of error is as small as possible. Thus, rank-

*r*decomposition extracts the first

*r*principal components of the tensor. This decomposition has been applied in computer vision, graph analysis, and neuroscience (Lu et al. 2006; Kolda and Bader 2009). Based on this explanation, the tensor decomposition can jointly analyze the characteristics of each dimension in the dataset. This constrained optimization problem can be analyzed using the Lagrange multipliers technique (Lathauwer et al. 2000).

*r*, the results include more and more details of ionospheric variation. The first few components capture smooth or large-scale structures of the ionosphere, as shown in Fig. 1 for \(r=1\). In our application, to analyze large-scale ionospheric structures, we only focus on the first principal component of the time-longitude-latitude characteristics, where \(r=1\). Because we mainly focus on the large-scale characteristics of the ionosphere, the details in the results are not necessarily expected to show close correspondence with the original data. Furthermore, the two crests in the subplots, ‘\(r=1\) CODG-1’ and ‘\(r=1\) CODG-2’ in Fig. 1, indicate the variation caused by the Sun and geomagnetic field (Franke et al. 2003). Such phenomenon is called the ionospheric fountain effect, which plays an essential role in the equatorial ionization anomaly (EIA). This anomaly is especially significant during daytime, because of the ionizing effect of solar radiation. Thermospheric winds in the equatorial E region drag particles across the geomagnetic field lines

**B**, creating an eastward electric field

**E**. Due to

**E**\(\times\)

**B**forces and the influence of gravity and pressure gradient forces, particles travel along field lines to higher latitudes (Hanson and Moffett 1966). Thus, there is one crest about the VTEC appearing on each side of the equator.

## Results and discussion

### Fourier spectral analysis of \(U^{(1)}\)

Because solar energy ionizes atmospheric molecules and creates the ionosphere, the ionospheric VTEC tensor is largely controlled by the Sun (Goldberg 1966; Schunk and Nagy 2009). Even though the temporal variation in the ionosphere is also affected by variations in geomagnetic field, magnetosphere, and atmosphere excluding solar irradiation, for the timescale of this research, the temporal variations in geomagnetic field, magnetosphere, and atmosphere are derived from solar irradiation as well. Thus, as demonstrated by Afraimovich et al. (2008), the global, long-timescale characteristics of the ionosphere are determined by solar irradiation. The rank-1 decomposition primarily extracts the long periodic variations in the ionosphere. Therefore, we hypothesize that the results of rank-1 decomposition for the time mode describe the ionospheric temporal variation mainly determined by solar irradiation.

As the global VTEC supplied by CODE is given with a 2-h time resolution, one day is divided into 12 time intervals, which are UT1:(00:00–02:00),...,UT12:(22:00–24:00). We construct a 3D tensor using only one VTEC map each day from 2011 to 2013. As a result, we can achieve twelve tensors based on twelve UT intervals, and obtain twelve \(U^{(1)}\). Because the frequency spectra of the twelve \(U^{(1)}\) are almost identical, we arbitrarily select one \(U^{(1)}\) to analyze. The tensor, constructed by the global VTEC map at UT8 every day from 2011 to 2013, is selected. The frequency spectrum of \(U^{(1)}\) is shown in Fig. 2. We select the first seven primary frequency components, \(f_1,\ldots ,f_7\). The frequency spectrum and its corresponding solar periodicities are shown in Table 1, where \(T=1/f\). There are various periodic variations in the ionosphere, including 27-day, daily, and yearly variations. Those periodic variations, e.g., 27-day and daily variations, are short-term compared to 3 years. The tensor rank-1 decomposition mainly focuses on the large-scale structures. Thus, only long periodic variations are presented in Table 1. In contrast, short-periodic variations will appear in the higher-rank decomposition.

As the nearest star, the Sun has an important effect on climate change and daily life on Earth. Hence, the periodicities of solar variation have been widely studied. There are various types of periodic solar activities. Significant cycles range from seconds to years (Atac et al. 2005), including the 1.3-year periodicity in solar rotation, which forms solar convection (Krivova and Solanki 2002; Guo et al. 2015; Moussas et al. 2005), 2-year periodicity (quasibiennial oscillation), and others, such as 0.9, 0.67, 0.53, 0.4, and 0.35-year (Polygiannakis et al. 2003). Furthermore, the formation of the ionosphere is primarily due to the ionization of the upper atmosphere by solar radiation. Therefore, temporal variations in the global ionosphere depends dominantly on the Sun. Table 1 shows a good corresponding relationship between the frequency spectrum of \(U^{(1)}\) and solar irradiation. \(f_{\Delta }\) corresponds to the 1.07-year period, which is missing in our results. This is probably due to the narrow interval between \(f_{\Delta }\) and \(f_{3}\), whose corresponding periods are \((1.07\pm 0.08)\) year and \((0.97\pm 0.06)\) year. Furthermore, based on Fourier Transform theory, the frequency resolution is \(1/T_w\), where \(T_w\) is the length of the series. The frequency uncertainty is \(\frac{1}{3\,{\mathrm{yr}}}\) in our research. To resolve the periodicity, \((1.07\pm 0.08)\) year, the length of the time series should be 10.4 year at least, because the frequency resolution should be larger than \(0.096 \frac{1}{\mathrm{yr}}\), which is calculated by \((\frac{1}{f_3}-\frac{1}{f_\Delta })\). Such a corresponding relationship among those periods indicates that the global ionospheric temporal variations are primarily influenced by the Sun.

Frequency label | Frequency (\(10^{-3}\) 1/day) | Periodicity (year) | Observed solar periodicity (year) | Periodicity in Mg II index (year) |
---|---|---|---|---|

\(f_1\) | 1.33 | 2.06 | 2.1 ± 0.1 | – |

\(f_2\) | 2.2 | 1.25 | 1.4 ± 0.1 | – |

\(f_{\Delta }\) | – | – | 1.07 ± 0.08 | – |

\(f_3\) | 3.08 | 0.90 | 0.97 ± 0.06 | 1 |

\(f_4\) | 4.11 | 0.67 | 0.67 ± 0.05 | – |

\(f_5\) | 5.23 | 0.52 | 0.49 ± 0.04 | 0.5 |

\(f_6\) | 6.82 | 0.40 | 0.42 ± 0.04 | – |

\(f_7\) | 8.0 | 0.34 | 0.34 ± 0.02 | – |

### Longitudinal patterns via \(U^{(2)}\)

Solar irradiation is one of the primary drivers of ionospheric variability, especially those of large scale, as the ionosphere is created by solar irradiation through ionization. Thus, if the ionospheric variations are only affected by the Sun, the VTEC amplitude would be proportional to solar irradiation. Generally, VTEC positively correlates with solar irradiation. Rama et al. (2016) found that the solar irradiation reached a maximum between 12:00–13:00 local time (LT). We mainly extract the longitude positions of the maxima of solar irradiation and ionospheric \(U^{(2)}\) in the 12 UT intervals.

Similar to the acquisition of \(U^{(1)}\), through rank-1 decomposition, 12 \(U^{(2)}\) can be achieved. Based on the conclusions in Reference Rama et al. (2016) and the 2-h time resolution, we believe the maximum of the solar irradiation on Earth is 12:00–14:00 LT. Then, we identify their central longitude position. The results are shown in Table 2 and Fig. 3. The 12 \(U^{(2)}\) represent the longitudinal wave-1 structure, i.e., single peak and trough. Because the longitude corresponds to local time, the peaks and troughs indicate variations during day and night times. The longitude differences between the positions of the maxima of \(U^{(2)}\) and solar irradiation are shown in Fig. 3 and Table 2.

The longitude position of the maxima of \(U^{(2)}\) and solar irradiation and longitude differences in each UT interval

Time interval | \(U^{(2)}\) Maximum (/\(^\circ\)) | Solar irradiation maximum (/\(^\circ\)) | Longitude difference (/\(^\circ\)) |
---|---|---|---|

UT1 | \(-\) 150 | \(-\) 180 | 30 |

UT2 | \(-\) 175 | 150 | 35 |

UT3 | 145 | 120 | 25 |

UT4 | 115 | 90 | 25 |

UT5 | 90 | 60 | 30 |

UT6 | 65 | 30 | 35 |

UT7 | 25 | 0 | 25 |

UT8 | \(-\) 5 | \(-\) 30 | 25 |

UT9 | \(-\) 25 | \(-\) 60 | 35 |

UT10 | \(-\) 35 | \(-\) 90 | 55 |

UT11 | \(-\) 105 | \(-\) 120 | 15 |

UT12 | \(-\) 115 | \(-\) 150 | 35 |

Furthermore, we investigate the monthly variation in time lags between large-scale variations in ionosphere and solar irradiation. In each UT interval, using 1-month global ionospheric maps (GIMs) instead of 3-years, we can construct a tensor, \({\mathscr {A}}_{30\times 73\times 71}\), each month, where 30 indicates 30 days in a month. There will be 12 tensors per year for each UT interval, accordingly. There are 3 years of data from 2011 to 2013 (36 months in total). We obtain \(36\times 12\) tensors, where 36 is the number of months and 12 is the number of UT intervals. Therefore, for the 12 months from January to December, each month will have 36 samples, including 3 samples for each 12 UT range. The longitude positions of the maxima of \(U^{(2)}\) and solar irradiation are used to investigate seasonal variations in the time lags. Based on the longitude differences between the maximum \(U^{(2)}\) and solar irradiation, we calculate the time lags in each UT interval for the 12 months from January to December. As a result, 36 time lags can be obtained each month. We calculate the averages and standard deviations of the time lags, with the results shown in Fig. 4.

In Fig. 4, the average time lags exhibit substantial seasonal differences. The Lloyd seasons, D, J, and E, represent the December Solstice (January, February, November and December), June Solstice (May, June, July and August), and Equinoxes (March, April, September and October), respectively. Figure 4 indicates that, overall, the average of time lags in Lloyd J are larger than the other two, while the ones in Lloyd D season are opposite. However, the standard deviations in each month are so large that it is difficult to find any significant seasonal differences. Thus, the time lag in large-scale ionospheric responses to solar irradiation does not depend on season.

From longitude differences in the CODE dataset shown in Table 2 indicate that they range from \(15^\circ\) to \(55^\circ\). Thus, the corresponding time lags range from 1 h to 3.7 h. Some studies have already revealed that ionospheric variations are actually most correlated with the solar irradiation in the previous hours, i.e., there are time lags (Chen et al. 2015). Afraimovich et al. (2006) stated that theory predicted a time lag of around 1 h for global mean TEC variations in response to variations in solar irradiation. A 1-h time lag corresponds to a \(15^{\circ }\) longitude difference. Hocke (2008) found that the time lag between oscillations of solar extreme ultraviolet and global mean TEC were less than 3.5 h, which corresponds to a \(52.5^{\circ }\) longitude difference (Hocke 2008). While most longitude differences are below \(52.5^{\circ }\) in Table 2, we find there is a \(55^{\circ }\) longitude difference, bigger than \(52.5^{\circ }\). The difference may be due to the selection of a different dataset. Hocke (2008) selected the oscillations in solar extreme ultraviolet to represent solar radiation.

Before solar irradiation reaches the ionosphere, it should pass the magnetosphere. As the charged particles travel along geomagnetic field lines, the geomagnetic field connects the ionosphere and magnetosphere. The charged particles can travel from the magnetotail to the ionosphere. Conversely, the ionospheric charged particles can travel to the magnetosphere. Concurrently, the geomagnetic field can help propagate plasma waves. The field-aligned currents (FACs) constitute the energetic link between the magnetosphere and ionosphere. Thus, variations in the magnetosphere and ionosphere are coupled and influence each other. Moreover, the thermosphere is the ionosphere background. We speculate that the magnetosphere–ionosphere–thermosphere (M–I–T) system likely results in a time lag.

When solar energy is imported into the M–I–T system, complex processes, such as Joule heating and convection and reconnection between the magnetosphere and ionosphere, likely attribute to the time lags. The response of the ionosphere to variations in ultraviolet radiation flux is determined by the time constants from ionization and the recombination of \(\sim 1\) h (Afraimovich et al. 2006; Astafyeva et al. 2008). The ionospheric response has a time delay of \(1\sim 2\) hours to the ring current variation in the magnetosphere, because of the relaxation process in the field-aligned current (Shen 1987). Fung and Shao (2008) suggested that the magnetosphere might have a memory time of a few hours, which is caused by a sequence of transitions and configuration changes associated with energy storing, dissipation, and recovery in the magnetosphere. Ionospheric electron density depends on both the ionizing solar radiation and background thermosphere. Thus, some studies attributed ionospheric time lags to thermospheric lags to the solar irradiance (Min et al. 2009; Wang et al. 2006). The correlation between the reversed *Dst* index and 3-h smoothing Joule heating indicates a delay time of 2–3 h between the Joule heating and global thermospheric response (Lu et al. 2017). Hence, we conjecture that the difference in the time lags may indicate different interactions between processes creating large-scale ionospheric variations in the M–I–T system. When the time lag is close to 1 h, ionization and recombination process may play a significant role in the M–I–T system. When the time lag is 2–3 h, Joule heating may be the primary process. Our results provide evidence for the time lag between the maxima of large-scale ionospheric variations and solar irradiation, though we cannot provide an exact explanation for its mechanism due to observational limitations.

### Hemispheric asymmetry in geomagnetic coordinates

Although many research studies on the ionosphere have been conducted based on geographic coordinates (Su et al. 2014; Chen et al. 2015; Talaat and Zhu 2016), some ionospheric characteristics, especially north–south asymmetry, are also investigated compared with geomagnetic coordinates (Geonhwa et al. 2004, 2005; Weihua and Jiaping 2015). Many geospace phenomena, including ionospheric currents, are highly organized by the Earth’s main geomagnetic field. This organization occurs because charged particles can move spirally forward along the magnetic field lines, but not across them. To provide better insight on NSA for ionospheric large-scale characteristics, we convert from geographic to geomagnetic coordinates.

To work in a reference frame that takes the geometry of the geomagnetic field into account, many geomagnetic coordinate systems are designed for different purposes and regions (Laundal and Richmond 2016). For the ionosphere, centered dipole coordinates, which represent a shift of the poles from the rotational axis to the dipole axis, are often used. However, at ionospheric altitude, the geomagnetic field deviates significantly from a centered dipole. To achieve better accuracy with respect to the geomagnetic field, we select the geomagnetic coordinates based on the geomagnetic apex (Laundal and Richmond 2016; Laundal and Gjerloev 2014). The geomagnetic apex coordinates are calculated using a Python wrapper available at GitHub.^{1} In this subsection, we mainly focus on the NSA for large-scale ionospheric variations based on geomagnetic coordinates. After coordinate conversions, the latitudinal results are shown in Fig. 5a. Using the GIMs displayed in geomagnetic coordinates, we construct new tensors whose dimensions are universal time, geomagnetic longitude, and geomagnetic latitude. To investigate the full-time variation, the tensor is constructed using all global VTEC maps every 2 h from 2011 to 2013. Through rank-1 decomposition, large-scale ionospheric variations in geomagnetic latitude, \(U^{(3)}\), are obtained.

Intuitively, a symmetrical large-scale ionospheric variation between the northern and southern hemisphere should place barycenter of the latitudinal variations on the equator. Thus, in this subsection, we preliminarily select the barycenter of geomagnetic \(U^{(3)}\) to investigate the NSA for large-scale ionospheric variations. Weighted by the distribution of mass in space, the position of the barycenter is the average position of all parts of the object. In one dimension, the position of the barycenter is usually calculated by \(\hat{x}=\frac{\sum _{i}P_{i}x(P_{i})}{\sum _{i}P_{i}}\), where \(\hat{x}\) is the position of the barycenter, and \(P_i\) and \(x(P_i)\) are the *i*th amplitude and its corresponding position, respectively. The results are shown in Fig. 5b.

In Fig. 5b, the position of the barycenter is \(1.65^\circ\) in the southern geomagnetic hemisphere. As depicted by Jee et al. (2010), the negative differences in GIM and TOPEX/Jason TEC are stronger in the southern hemisphere than in the northern hemisphere. Accordingly, due to the sparsity of GPS stations, VTEC estimates in the southern hemisphere are smaller in the CODE GIMs. As Fig. 5b shows, the position of the barycenter is in the southern hemisphere. Because the analysis is made using the CODE VTEC, which is smaller than the real value in the southern hemisphere, we hypothesize that without inhomogeneous coverage of stations, the north–south asymmetry in large-scale ionospheric variations will be clearer. Therefore, an inhomogeneous distribution of GPS stations between the northern and southern hemispheres does not cast doubt on the conclusions regarding NSA for large-scale ionospheric variations acquired from the CODE dataset. The asymmetry shown by the position of the barycenter reveals a north–south hemispheric difference in the large-scale ionospheric variations and provides evidence for NSA based on geomagnetic coordinates. The two crests around the geomagnetic equator indicate the existence of an equatorial ionization anomaly (EIA). As shown in Fig. 5b, the geomagnetic latitude positions of those crests are \(10^{\circ } N\) and \(10^{\circ } S\), showing symmetry. The amplitudes of these two crests are 0.195 and 0.198, which are almost the same. Therefore, from the perspective of the ionospheric large-scale variation, the asymmetry shown in EIA is not clear.

### Daily and diurnal variations of NSA

We investigate the north–south asymmetry of large-scale ionospheric variations caused by solar ionization referring to geomagnetic coordinates. As introduced above, there are 12 GIMs that constitute a tensor \({\mathscr {A}}_{12\times 73\times 71}\) each day. Here, we use the data displayed in geomagnetic coordinates. Based on the rank-1 decomposition, the geomagnetic latitude mode, \(U^{(3)}\) is acquired each day. Then, the barycenter position of \(U^{(3)}\) can be calculated to indicate the north–south asymmetry in the large-scale ionospheric variations. Thus, from 2011 to 2013, 1096 barycenter positions \(\hat{x}\) are obtained. We investigate the temporal variation in \(\hat{x}\) to investigate the solar effect on the NSA. The results are shown in Fig. 6, where its frequency spectrum is calculated by Fourier Transform.

As Fig. 6a shows, the barycenters oscillate seasonally around the geomagnetic equator. The wave form is similar to the trajectory of subsolar position, which oscillates seasonally about the geographic equator. In Fig. 6b, \(f_1=2.7\times 10^{-3}\frac{1}{\mathrm{day}}\). The corresponding period is 370 days. There are about 5 days of difference between the daily variation in barycenter position and the subsolar point. Such differences may be attributed to the difference between the geomagnetic and geographic equator, as shown in Fig. 5a. Therefore, such phenomenon can indicate the effect of solar ionization on the NSA for large-scale ionospheric variations.

To compare such NSA between day and night, the CODE dataset displayed in geomagnetic coordinates is divided into two parts, day and night regions. Traditionally, day is defined as 06:00–18:00 LT and night as 18:00–06:00 LT. Every day, we select the GIM at UT4(6:00–8:00) when the eastern hemisphere is in day and the western hemisphere is night. Accordingly, from 2011 to 2013, 1096 GIMs at UT4 are selected. The right parts of those GIMs represent day, containing 37 rows of the GIM matrix. Similarly, the left ones represent night, containing 36 rows. Thus, the right parts of the GIMs constitute the day tensor, \({\mathscr {A}}^d_{1096\times 37\times 71}\), while the left parts constitute the night tensor, \({\mathscr {A}}^n_{1096\times 36\times 71}\). Using the rank-1 decomposition, large-scale ionospheric variations in geomagnetic latitude for day and night are shown in Fig. 7.

As shown in Fig. 7, the barycenter positions of diurnal \(U^{(3)}\) are \(6.3^\circ S\) and \(7.3^\circ S\), which are all in the southern hemisphere. Such phenomenon also provides evidence for north–south asymmetry in large-scale ionospheric variations during day and night. Moreover, both the waveforms of geomagnetic \(U^{(3)}\) during the day and night indicate the existence of an EIA. The geomagnetic latitudes of the crests are \(10^{\circ } N\) and \(10^{\circ } S\). The results are in agreement with the conclusions provided in Fig. 5. Thus, the NSAs for large-scale variations in the EIA during day and night are almost identical.

### Results of geomagnetic quiet GIMs

To investigate the effects of geomagnetic disturbances and storms on large-scale ionospheric variations, the GIMs obtained during the geomagnetic quiet periods are employed for analysis. First, although the ionospheric temporal variations are affected by geomagnetic disturbances and storms, those influences are negligible in our analysis. This is because geomagnetic disturbances and storms do not have a significant impact on long-term large-scale variations in the ionosphere. Specifically, the duration of geomagnetic disturbances and storms tends to range from a few minutes to tens of hours (Xu 2009), which is short-term compared to our 3-year data length. That is, the time scale of the ionospheric variation caused by the geomagnetic disturbance or storm is short-term compared to 3 years, and the tensor rank-1 decomposition only extracts long-term and large-scale ionospheric variations. Hence, the geomagnetic disturbances and storms would make little difference in the long-term ionospheric variations obtained by the tensor rank-1 decomposition.

As an index measuring the intensity of global geomagnetic activity, the planetary 3-hour-range index *Kp* has been widely used in ionospheric and geomagnetic fields. To further study the effects of geomagnetic disturbances and storms on the ionosphere, we select the *Kp* index as the geomagnetic activity index. Introduced by Bartels et al. (1939), *Kp* is the average *K*-index from 13 geomagnetic observatories between \(44^\circ\) and \(60^\circ\) northern or southern geomagnetic latitude, with a 3-h interval and value range of \(\{0_0,0_+,1_-,1_0,\cdots 9_-,9_0\}\). When \(Kp<4_0\), the geomagnetic field is considered quiet. *Kp* indices are obtained from the National Geophysical Data Center.**^{2} To study the influences of geomagnetic disturbances and storms on large-scale ionospheric variations, when \(Kp>4_0\), we remove the current GIM and the next one during tensor construction. Hence, the tensor of the ionosphere during geomagnetic quiet periods can be obtained. Then, the tensor rank-1 decomposition is employed to obtain large-scale ionospheric variations during geomagnetic quiet periods.

For large-scale longitudinal patterns via \(U^{(2)}\), similar to the previous analysis, we construct a tensor using the geomagnetic quiet GIMs in each UT interval. The number of geomagnetic quiet GIMs in the tensor in each UT interval is shown in the titles of the subfigures in Fig. 8. This figure shows the results of \(U^{(2)}\) for geomagnetic quiet GIMs in each UT interval. As shown, the longitude differences between the maxima of large-scale longitudinal variations and those of solar irradiation in \(U^{(2)}\) are the same as those in Fig. 3. In addition, removing the GIMs affected by the geomagnetic disturbances and storms, we obtain 11,700 GIMs to investigate the NSA for large-scale ionospheric variations. Figure 9 is achieved by tensor rank-1 decomposition during the geomagnetic quiet periods, showing the results of north–south hemispheric asymmetry in large-scale ionospheric variations. The characteristics of \(U^{(3)}\) in Fig. 9 are similar with those of \(U^{(3)}\) in Fig. 5b. The positions and amplitudes the crests are \(\pm 10^\circ\) and about 0.19. Thus, the NSA in EIA is masked in the large-scale ionospheric variations during the geomagnetic quiet periods. In Fig. 9, the geomagnetic latitude position of the barycenter in \(U^{(3)}\) is \(1.89^\circ S\). Thus, after removing the influences of geomagnetic disturbances, the results still show the existence of NSA in large-scale ionospheric variations. Therefore, the influences of geomagnetic disturbances and storms make little difference with respect to our previous conclusions. More explicitly, the geomagnetic disturbances/storms have little effect on the results of the tensor rank-1 decomposition in the ionospheric spatiotemporal analysis. The rank-1 decomposition mainly extracts both temporal and spatial variations at large scale in the ionosphere, while the ionospheric variations caused by the geomagnetic disturbances and storms have a relatively small spatiotemporal scale. This phenomenon also shows the robustness of the tensor rank-1 decomposition in analyzing large-scale spatiotemporal variations in the ionosphere.

## Conclusions

As an important component of the geospace environment, the ionosphere has received increasing attention. Research on the ionosphere is of great value in both application and theory. In this paper, VTEC data for 2011–2013 supplied by CODE are employed. The data, which is in the form of a time series of global ionospheric maps, constitute 3D tensors. We propose using the tensor rank decomposition, which can be used to analyze different components in a multidimensional array, to jointly analyze the temporal–longitudinal–latitudinal characteristics of the ionosphere. Compared with EOF and PCA, tensor rank decomposition captures both the spatiotemporal and longitudinal–latitudinal characteristics. To analyze the large-scale ionospheric structures, the tensor rank-1 decomposition, also known as the best rank-1 approximation, is used to extract the first principal component of the GIM series.

Through rank-1 decomposition, large-scale ionospheric variations \(U^{(1)}\), \(U^{(2)}\) and \(U^{(3)}\) are achieved, which are the resulting unit-norm vectors for time, longitude, and latitude mode, respectively. The correspondence between the spectrum of \(U^{(1)}\) and solar variation indicates that the rank-1 decomposition describes the large-scale ionospheric temporal variations, mainly caused by solar irradiation. Second, using the GIM tensors for different UT intervals, between the maxima of ionospheric \(U^{(2)}\) and solar irradiation, the time lags can be obtained. The time lag primarily ranges from 1 to 3.7 h. Monthly variations in time lags indicates that the time lag between the ionospheric responses and solar irradiation varies without seasonal dependence. The differences in time lags likely indicate different processes in the M–I–T system. When the time lag is close to 1 h, ionization and recombination processes play a significant role in the M–I–T system, while 2–3-h time lags indicate that Joule heating probably is primary. Moreover, the spatial variation in the rank-1 decomposition is oriented in geomagnetic coordinates. The position of the barycenter for \(U^{(3)}\) in geomagnetic coordinates provides evidence for an NSA for large-scale ionospheric variations. Furthermore, the daily variation in hemispheric asymmetry indicates the effect of the Sun on large-scale ionospheric characteristics. The diurnal \(U^{(3)}\) in geomagnetic coordinates show that the large-scale variations in the EIA during the day and night are almost identical. Finally, we investigate the influence of geomagnetic disturbances by excluding the GIMs obtained during the geomagnetic disturbances. The results show that the geomagnetic disturbance makes little difference with respect to our primary conclusions. Generally speaking, the rank-1 decomposition can decouple the correlations between time, longitude, and latitude in the ionosphere, and capture smooth ionospheric structures caused by the Sun, geomagnetic field, and magnetosphere.

## Declarations

### Authors’ contributions

SL and HZ performed the major theoretical analysis and led the writing of the manuscript. SL analyzed the data. XL, YL, and DL helped conduct the research and provided constructive edits to the manuscript. CN and XY participated in the manuscript discussion. All authors read and approved the final manuscript.

### Acknowledgements

This work was supported by the National Natural Science Foundation of China (41374154 and 41774156). We are grateful to Adam Woods from CIRES, University of Colorado, the David Skaggs Research Center, and Rolf Dach and Stefan Schaer from the Astronomical Institute at the University of Bern. Their help in providing data is appreciated. The GIMs from CODE are available at ftp://ftp.unibe.ch/aiub/CODE. Furthermore, we are grateful to K. M. Laundal from the Birkeland Centre for Space Science, University of Bergen. He kindly helped obtain the geomagnetic coordinates based on apex. We also want to express our thanks to the reviewers for their thoughtful comments and suggestions. Moreover, Shikun Lu would like to thank, in particular, the ongoing and unwavering support from Taotao Sun over the years.

### Competing interests

The authors declare that they have no competing interests.

### Ethics approval and consent to participate

Not applicable.

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## Authors’ Affiliations

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