Issue 
J. Space Weather Space Clim.
Volume 6, 2016
Statistical Challenges in Solar Information Processing



Article Number  A3  
Number of page(s)  19  
DOI  https://doi.org/10.1051/swsc/2015043  
Published online  25 January 2016 
Research Article
Image patch analysis of sunspots and active regions
II. Clustering via matrix factorization
^{1}
Electrical Engineering and Computer Science Department, University of Michigan, Ann Arbor, MI 48109, USA
^{2}
SIDC, Royal Observatory of Belgium, 1180
Brussels, Belgium
^{3}
National Solar Observatory, CO 80303, Boulder, USA
^{*} Corresponding author: krmoon@umich.edu
Received:
10
April
2015
Accepted:
10
December
2015
Context. Separating active regions that are quiet from potentially eruptive ones is a key issue in Space Weather applications. Traditional classification schemes such as Mount Wilson and McIntosh have been effective in relating an active region large scale magnetic configuration to its ability to produce eruptive events. However, their qualitative nature prevents systematic studies of an active region’s evolution for example.
Aims. We introduce a new clustering of active regions that is based on the local geometry observed in Line of Sight magnetogram and continuum images.
Methods. We use a reduceddimension representation of an active region that is obtained by factoring the corresponding data matrix comprised of local image patches. Two factorizations can be compared via the definition of appropriate metrics on the resulting factors. The distances obtained from these metrics are then used to cluster the active regions.
Results. We find that these metrics result in natural clusterings of active regions. The clusterings are related to large scale descriptors of an active region such as its size, its local magnetic field distribution, and its complexity as measured by the Mount Wilson classification scheme. We also find that including data focused on the neutral line of an active region can result in an increased correspondence between our clustering results and other active region descriptors such as the Mount Wilson classifications and the Rvalue.
Conclusions. Matrix factorization of image patches is a promising new way of characterizing active regions. We provide some recommendations for which metrics, matrix factorization techniques, and regions of interest to use to study active regions.
Key words: Sun / Active region / Sunspot / Neutral line / Data analysis / Classification / Clustering / Image patches / Hellinger distance / Grassmannian
© K.R. Moon et al., Published by EDP Sciences 2016
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
1. Introduction
1.1. Context
Identifying properties of active regions (ARs) that are necessary and sufficient for the production of energetic events such as solar flares is one of the key issues in space weather. The Mount Wilson classification (see Table 1 for a brief description of its four main classes) has been effective in relating a sunspot’s large scale magnetic configuration with its ability to produce flares. Künzel (1960) pointed out the first clear connection between flare productivity and magnetic structure, and introduced a new magnetic classification, δ, to supplement Hale’s α, β, and γ classes (Hale et al. 1919). Several studies showed that a large proportion of all major flare events begin with a δ configuration (Warwick 1966; Mayfield & Lawrence 1985; Sammis et al. 2000).
Mount Wilson classification rules, number of each AR, and total number of joint patches or pixels per Mount Wilson class used in this paper when using the STARA masks.
The categorical nature of the Mount Wilson classification, however, prevents the differentiation between two sunspots with the same classification and makes the study of an AR’s evolution cumbersome. Moreover, the Mount Wilson classification is generally carried out manually which results in human bias. Several papers (Colak & Qahwaji 2008, 2009; Stenning et al. 2013) have used supervised techniques to reproduce the Mount Wilson and other schemes which has resulted in a reduction in human bias.
To go beyond categorical classification in the flare prediction problem, the last decade has seen many efforts in describing the photospheric magnetic configuration in more details. Typically, a set of scalar properties is derived from line of sight (LOS) or vector magnetogram and analyzed in a supervised classification context to derive which combination of properties is predictive of increased flaring activity (Leka & Barnes 2004; Guo et al. 2006; Barnes et al. 2007; Georgoulis & Rust 2007; Schrijver 2007; Falconer et al. 2008; Song et al. 2009; Huang et al. 2010; Yu et al. 2010; Lee et al. 2012; Ahmed et al. 2013; Bobra & Couvidat 2015). Examples of scalar properties include: sunspot area, total unsigned magnetic flux, flux imbalance, neutral line length, maximum gradients along the neutral line, or other proxies for magnetic connectivity within ARs. These scalar properties are features that can be used as input in flare prediction. However, there is no guarantee that these selected features exploit the information present in the data in an optimal way for the flare prediction problem.
1.2. Contribution
We introduce a new datadriven method to cluster ARs using information contained in magnetogram and continuum. Instead of focusing on the best set of properties that summarizes the information contained in those images, we study the natural geometry present in the data via a reduceddimension representation of such images. The reduceddimension is implemented via matrix factorization of an image patch representation as explained in Section 1.3. We show how this geometry can be used for classifying ARs in an unsupervised way, that is, without including AR labels as input to the analysis.
We consider the same dataset as in Moon et al. (2015). It is obtained from the Michelson Doppler Imager (MDI) instrument (Scherrer et al. 1995) on board the SOHO Spacecraft. SOHOMDI provides two to four times per day a whitelight continuum image observed in the vicinity of the Ni I 676.7L nm photospheric absorption line. MDI LOS magnetograms are recorded with a higher nominal cadence of 96 min. We selected 424 sunspot images within the time range of 1996–2010. They span the various Mount Wilson classifications (see Table 1), are located within 30° of central meridian, and have corresponding observations in both MDI continuum and MDI LOS magnetogram. We use level 1.8 data for both modalities.
Our method can be adapted to any definition of the support of an AR, or Region of Interest (ROI), and such ROI must be given a priori. We consider three types of ROIs:

Umbrae and penumbrae masks obtained with the Sunspot Tracking and Recognition Algorithm (STARA; Watson et al. 2011) from continuum images. These sunspot masks encompass the regions of highest variation observed in both continuum and magnetogram images, and hence are used primarily to illustrate our method. Figure 1 provides some examples of AR images overlaid with their respective STARA masks.
Fig. 1. MDI continuum and magnetogram from NOAA 9097 on July 23, 2000 (top) and from NOAA 10045 on July 25, 2002 (bottom) overlaid with the corresponding STARA masks in green.

The neutral line region, defined as the set of pixels situated no more than 10 pixels (20 arcsec) away from the neutral line, and located within the Solar Monitor Active Region Tracker (SMART) masks (Higgins et al. 2011), which defines magnetic AR boundaries.

The set of pixels that are used as support for the computation of the Rvalue defined in Schrijver (2007). The Rvalue measures a weighted absolute magnetic flux, where the weights are positive only around the neutral line.
Our patchbased matrix factorization method investigates the fine scale structures encoded by localized gradients of various directions and amplitudes, or locally smooth areas for example. In contrast, the Mount Wilson classification encodes the relative locations and sizes of concentrations of opposite polarity magnetic flux on a large scale. Although both classification schemes rely on completely different methods, using the first ROI defined above, we find some similarities (see Sect. 5). Moreover, the Mount Wilson classification can guide us in the interpretation of the results and clusters obtained.
The shape of the neutral line separating the two main polarities in an AR is a key element in the Mount Wilson classification scheme, and the magnetic field gradients observed along the neutral line are important information in the quest for solar activity prediction (Schrijver 2007; Falconer et al. 2008). We therefore analyze the effect of including the neutral line region in Section 5.
Results based on the third ROI are compared directly to the Rvalue. The various comparisons enable us to evaluate the potential of our method for flare prediction.
1.3. Reduced dimension via matrix factorization
Our datadriven method is based on a reduceddimension representation of an AR ROI via matrix factorization of image patches. Matrix factorization is a widely used tool to reveal patterns in high dimensional datasets. Applications outside of solar physics are numerous and range e.g. from multimedia activity correlation, neuroscience, gene expression (Bazot et al. 2013), to hyperspectral imaging (Mittelman et al. 2012).
The idea is to express a kmultivariate observation z_{1} as a linear combination of a reduced number of r < k components a_{j}, each weighted by some (possibly random) coefficients h_{j,1}:(1)where n_{1} represents residual noise. With Z = [z_{1},…, z_{n}], the equivalent matrix factorization representation is written as(2)where Z is a k × n data matrix containing n observations of k different variables, A is the k × r matrix containing the dictionary elements’ (called “factor loadings” in some applications), and H is the r × n matrix of coefficients (or factor scores’). The k × n matrix N contains residuals from the matrix factorization model fitting. Finding A and H from the knowledge of Z alone is a severely illposed problem, hence prior knowledge is needed to constrain the solution to be unique.
Principal Component Analysis (PCA; Jolliffe 2002) is probably the most widely used dimensionality reduction technique. It seeks principal directions that capture the highest variance in the data under the constraints that these directions are mutually orthogonal, thereby defining a subspace of the initial space that exhibits information rather than noise. The PCA solution can be written as a matrix factorization thanks to the Singular Value Decomposition (SVD; Moon & Stirling 2000), and so we use SVD in the clustering method presented here.
The Nonnegative Matrix Factorization (NMF; Lee & Seung 2001) is also considered in this paper. Instead of imposing orthogonality, it constrains elements of matrices A and H to be nonnegative. We further impose that each column of H has elements that sum up to one, thereby effectively using a formulation identical to one used in hyperspectral unmixing (BioucasDias et al. 2012).
Unmixing techniques exploit the high redundancy observed in similar bandpasses. They aim at separating the various contributions and at estimating a smaller set of less dependent source images. Matrix factorization, known as blind source separation’ in this context, has many applications, ranging from biomedical imaging, chemometrics, to remote sensing (Comon & Jutten 2010), and recently to the extraction of salient morphological features from multiwavelength extreme ultraviolet solar images (Dudok de Wit et al. 2013).
In this paper, we wish to factorize a k × n data matrix Z containing n observations of k different variables as in Eq. (2) where the dictionary matrix A spans a subspace of the initial space, with r < k. We consider the cases where Z is formed from a single image as well as from multiple images.
When a single image is used, the data matrix Z is built from a n pixel image by taking overlapping m × mpixel neighborhoods called patches. Figure 2a presents such a patch and its column representation. The k rows of the ith column of Z are thus given by the m^{2} pixel values in the neighborhood of pixel i. The right plot in Figure 2 provides the number of patches in each pair of AR images when using the STARA masks. When multiple images are used, such as when analyzing collectively all images from a given Mount Wilson class, the patches are combined into a single data matrix. Table 1 gives the total number of patches from each Mount Wilson class when using the STARA masks.
Fig. 2. (a) An example of a 3 × 3 pixel neighborhood or patch extracted from the edge of a sunspot in a continuum image and its column representation. (b) The number of patches extracted from each pair of AR images when using the STARA masks. 
A factorization of a data matrix containing image patches is illustrated in Figure 3. In this figure, let z_{1} be the first column of Z, containing the intensity values for the first patch. These intensity values are decomposed as a sum of r elements as in Eq. (1) where a_{j} is the jth column of A and h_{j,1} is the (j,1)th element of H. In this representation, the vectors a_{j}, j = 1,…, r are the elementary building blocks common to all patches, whereas the h_{j,1} are the coefficients specific to the first patch.
Fig. 3. An example of linear dimensionality reduction where the data matrix of AR image patches Z is factored as a product of a dictionary A of representative elements and the corresponding coefficients in the matrix H. The A matrix consists of the basic building blocks for the data matrix Z and H contains the corresponding coefficients. 
To compare ARs and cluster them based on this reduceddimension representation, some form of distance is required. To measure the distance between two ARs, we apply some metrics to the corresponding matrices A or H obtained from the factorizations of the two ARs. These distances are further introduced into a clustering algorithm that groups ARs based on the similarity of their patch geometry.
This paper builds upon results obtained in Moon et al. (2015), which can be summarized as follows:

Continuum and magnetogram modalities are correlated, and there may be some advantage in considering both of them in an analysis.

A patch size of m = 3 includes a significant portion of spatial correlations present in continuum and magnetogram images.

Linear methods for dimensionality reduction (e.g. matrix factorization) are appropriate to analyze ARs observed with continuum images and magnetogram.
With an AR area equal to n pixels and an m × m patch, the corresponding continuum data matrix X and magnetogram data matrix Y each have size m^{2} × n. The full data matrix considered is with size 2m^{2} × n = 18 × n in our case. The images extracted from both modalities are normalized prior to analysis. An intrinsic dimension analysis in Moon et al. (2015) showed further that a sunspot can be represented accurately with a dictionary containing six elements.
1.4. Outline
Section 2 describes two matrix factorization methods: the singular value decomposition (SVD) and nonnegative matrix factorization (NMF). While more sophisticated methods exist that may lead to improved performance, we focus on SVD and NMF to demonstrate the utility of an analysis of a reduceddimension representation of image patches for this problem. Future work will include further refinement in the choice of matrix factorization techniques. To compare the results from this factorization we need a metric, and so we use the Hellinger distance for this purpose. To obtain some insight on how these factorizations separate the data, we make some general comparisons in Section 3. In particular, with the defined metric, we compute the pairwise distances between Mount Wilson classes to identify which classes are most similar or dissimilar according to the matrix factorization results.
Section 4 describes the clustering procedures that take the metrics’ output as input. The method called Evidence Accumulating Clustering with Dual rooted Prim tree Cuts’ (EACDC) was introduced by Galluccio et al. (2013) and is used to cluster the ARs. By combining the two matrix factorization methods, a total of two procedures are used to analyze the data. Besides analyzing the whole sunspot data, we also look at information contained in patches situated along the neutral lines. The results of the clustering analyses are provided in Section 5.
This paper improves and extends the work in Moon et al. (2014), where fixed size square pixel regions centered on the sunspot group were used as the ROI for the matrix factorization prior to clustering. Moreover, here we are using more appropriate metrics to compare the factorization results.
2. Matrix factorization
The intrinsic dimension analysis in Moon et al. (2015) showed that linear methods (e.g. matrix factorization) are sufficient to represent the data, and hence we focus on those. Matrix factorization methods aim at finding a set of basis vectors or dictionary elements such that each data point (in our case, pair of pixel patches) can be accurately expressed as a linear combination of the dictionary elements. Mathematically, if we use m × m patches then this can be expressed as Z ≈ AH, where Z is the 2m^{2} × n data matrix with n data points being considered, A is the 2m^{2} × r dictionary with the columns corresponding to the dictionary elements, and H is the r × n matrix of coefficients. The goal is to find matrices A and H whose product nearly approximates Z. The degree of approximation is typically measured by the squared error , where ·_{ F } denotes the Frobenius norm (Yaghoobi et al. 2009). Additional assumptions on the structure of the matrices A and H can be applied in matrix factorization depending on the application. Examples include assumptions of orthonormality of the columns of the dictionary A, sparsity of the coefficient matrix H (Ramírez & Sapiro 2012), and nonnegativity on A and H (Lin 2007).
We consider two popular matrix factorization methods: the singular value decomposition (SVD) and nonnegative matrix factorization (NMF).
2.1. Factorization using SVD
To perform matrix factorization using SVD, we take the singular value decomposition of the data matrix Z = UΣV^{T}, where U is the matrix of the left singular vectors, Σ is a diagonal matrix containing the singular values, and V is a matrix of the right singular vectors. If the size of the dictionary r is fixed and is less than 2m^{2}, then the matrix of rank r that is closest to Z in terms of the Frobenius norm is the matrix product , where U_{r} and V_{r} are matrices containing only the first r singular vectors and Σ_{r} contains only the first r singular values (Moon & Stirling 2000). Thus for SVD, the dictionary and coefficient matrices are A = U_{r} and , respectively. Note that SVD enforces orthonormality on the columns of U_{r}. Further details are included in Appendix A.1.
The intrinsic dimension estimated in Moon et al. (2015) determines the number of parameters required to accurately represent the data. It is used to provide an initial estimate for the size of the dictionaries r. For SVD, we choose r to be one standard deviation above the mean intrinsic dimension estimate, that is, or 6. The choice of r is then further refined by a comparison of dictionaries in Section 3. See Section 4.2 for more on selecting the dictionary size.
Figure 4 shows the learned dictionaries using SVD on the entire dataset of 424 image pairs of ARs. Interestingly, the SVD seems to consider the continuum and magnetogram separately as the magnetogram elements are essentially zero when the continuum elements are not and vice versa. This is likely caused by the orthonormality constraint. The dictionary patches largely consist of a mix of uniform patches and patches with gradients in varied directions. The second dictionary element is associated with the average magnetic field value of a patch.
Fig. 4. Learned dictionary elements using SVD. Dictionary elements are constrained to be orthonormal. The patches consist of uniform patches and gradients in varied directions. The magnetogram patches are essentially zero when the continuum components are nonzero and vice versa. The dictionary size r is first chosen based on the intrinsic dimension estimates in Moon et al. (2015) and then refined by comparing dictionaries of various sizes in Section 3. Section 4.2 contains more details on choosing r. 
2.2. Factorization using NMF
Nonnegative matrix factorization (NMF; Lee & Seung 2001) solves the problem of minimizing while constraining A and H to have nonnegative values. Thus NMF is a good choice for matrix factorization when the data is nonnegative. For our problem, the continuum data is nonnegative while the magnetogram data is not. Therefore we use a modified version of NMF using projected gradient where we only constrain the parts of A corresponding to the continuum to be nonnegative. An effect of using this modified version of NMF is that since the coefficient matrix H is still constrained to be nonnegative, we require separate dictionary elements that are either positive or negative in the magnetogram component. Thus we use approximately 1.5 times more dictionary elements for NMF than SVD.
Since we apply NMF to the full data matrix Z, this enforces a coupling between the two modalities by forcing the use of the same coefficient matrix to reconstruct the matrices X and Y. This is similar to coupled NMF which has been used in applications such as hyperspectral and multispectral data fusion (Yokoya et al. 2012).
Figure 5 shows the learned dictionary elements using NMF on the entire dataset. For NMF, the modalities are not treated separately as in the SVD results. But as for SVD, the patches largely consist of a mix of uniform patches and patches with gradients in varied directions.
Fig. 5. Learned dictionary elements using NMF where the continuum dictionary elements are constrained to be nonnegative. All the dictionary patches consist of uniform patches or gradients in varied directions. The order of the elements is not significant. The dictionary size r is chosen to be approximately 1.5 times larger than the SVD dictionary size, which is chosen based on the intrinsic dimension estimates in Moon et al. (2015) and then refined using the results in Section 3. 
2.3. SVD vs. NMF
There are advantages to both SVD and NMF matrix factorization methods which are summarized in Table 2. SVD produces the optimal rank r approximation of Z, is fast and unique, and results in orthogonal elements (Langville et al. 2006). NMF has the advantages of nonnegativity, sparsity, and interpretability. The interpretability comes from the additive partsbased representation inherent in NMF (Langville et al. 2006). In contrast, the SVD results are not sparse which can make interpretation more difficult. However, NMF is not as robust as SVD as the NMF algorithm is a numerical approximation to a nonconvex optimization problem having local minima. Thus the solution provided by the NMF algorithm depends on the initialization. More details on matrix factorization using NMF and SVD are included in Appendix A.1.
Summary of the advantages of SVD and NMF matrix factorization methods. The advantages of one method complement the disadvantages of the other (Langville et al. 2006). For example, the NMF optimization problem is nonconvex with local minima resulting in solutions that depend on the initialization of the algorithm.
2.4. Methods for comparing matrix factorization results
To compare the results from matrix factorization, we primarily seek a difference between the coefficients from H. To aid us in choosing a dictionary size r, we also require a measure of difference between dictionaries A. We use the Hellinger distance and Grassmannian projection metric to measure the respective differences.
In Moon et al. (2014), the Frobenius norm was used to compare the dictionaries. However, this fails to take into account the fact that two dictionaries may have the same elements but in a different order. In this case, the Frobenius norm of the difference between two dictionaries may be high even though the dictionaries span the same subspace. A better way to measure the difference would be to compare the subspaces spanned by the dictionaries. The Grassmannian Gr(r, V) is a space which parameterizes all linear subspaces with dimension r of a vector space V. As an example, the Grassmannian is the space of planes through the origin of the standard Euclidean vector space in . In our case, we are concerned with the Grassmannian , where r is the size of the dictionary. The space spanned by a given dictionary A is then a single point in . Several metrics have been defined on this space including the Grassmannian projection metric (Stewart 1973; Edelman et al. 1998). It can be defined aswhere P_{A} = A (A^{T}A)^{−1}A^{T} is the projection matrix of A and · is the norm. This metric is invariant to the order of the dictionary elements and compares the subspaces spanned by the dictionaries. This metric has a maximum value of 1.
To compare the coefficient matrices, we assume that the 18dimensional pixel patches within an AR are samples from an 18dimensional probability distribution, and that each AR has a corresponding (potentially unique) probability distribution of pixel patches. We project these samples onto a lower dimensional space by matrix factorization. In other words, we learn a dictionary A and the coefficient matrix H for the entire dataset Z, and then separate the coefficients in H according to the K different ARs (or groups of ARs) considered: Z = A (H_{1}H_{2} … H_{K}). The columns of H_{i} are a collection of projected, lowdimensionality, samples from the ith AR (or group), and we let f_{i} denote the corresponding probability density function. Given two such collections, we can estimate the difference between their probability distributions by estimating the information divergence. Many kinds of divergences exist such as the popular KullbackLeibler divergence (Kullback & Leibler 1951). We use the Hellinger distance which is defined as (Hellinger 1909; Bhattacharyya 1946; Csiszar 1967):where f_{i} and f_{j} are the two probability densities being compared. The Hellinger distance has the advantage over other divergences of being a metric which is not true of divergences in general. To estimate the Hellinger distance, we use the nonparametric estimator derived in Moon & Hero III (2014a, 2014b) that is based on the knearest neighbor density estimators for the densities f_{i} and f_{j}. This estimator is simple to implement and achieves the parametric convergence rate when the densities are sufficiently smooth.
3. Comparisons of general matrix factorization results
We apply the metrics mentioned in Section 2.4 and compare the local features as extracted by matrix factorization per Mount Wilson class. One motivation for these comparisons is to investigate differences between the Mount Wilson classes based on the Hellinger distance. Another motivation is to further refine our choice of dictionary size r in preparation for clustering the ARs. When comparing the dictionary coefficients using the Hellinger distance, we want a single, representative dictionary that is able to accurately reconstruct all of the images. Then the ARs will be differentiated based on their respective distributions of dictionary coefficients instead of the accuracy of their reconstructions. The coefficient distributions can then be compared to interpret the clustering results as is done in Section 5.1.
Recall that our goal is to use unsupervised methods to separate the data based on the natural geometry. Our goal is not to replicate the Mount Wilson results. Instead we use the Mount Wilson labels in this section as a vehicle for interpreting the results.
3.1. Grassmannian metric comparisons
We first learn dictionaries for each of the Mount Wilson types by applying matrix factorization to a subset of the patches corresponding to sunspot groups of the respective type. We then use the Grassmannian metric to compare the dictionaries. For example, if we want to compare the α and β groups, we collect a subset of patches from all ARs designated as α groups into a single data matrix Z_{α}. We then factor this matrix with the chosen method to obtain Z_{α} = A_{α}H_{α}. Similarly, we obtain Z_{β} = A_{β}H_{β} and then calculate d_{G} (A_{α}, A_{β}).
The reason we use only a subset of patches is that each AR type has a different number of total patches (see Table 1) which may introduce bias in the comparisons. One source of potential bias in this case is due to the potentially increased patch variability in groups with more patches, which would result in increased difficulty in characterizing certain homogeneities of the patch features. This is mitigated somewhat by the fact that the local intrinsic dimension is typically less than 6 (Moon et al. 2015). However, it is possible that there may be different local subspaces with the same dimension. A second source of potential bias is in the different levels of variance of the estimates due to difference in patch numbers. To circumvent these potential biases, we use the same number of patches in each group for each comparison. For the interclass comparison, we randomly take 13,358 patches (the number of patches in the smallest class) from each class to learn the dictionary, and then calculate the Grassmannian metric. For the intraclass comparison, we take two disjoint subsets of 6679 patches (half the number of patches in the smallest class) from each class to learn the dictionaries. This process is repeated 100 times and the resulting mean and standard deviation are reported.
Table 3 shows the corresponding average Grassmannian distance metrics when using SVD and NMF and for different sizes of dictionaries r. For SVD, the results are very sensitive to r. Choosing r = 5 results in large differences between the different dictionaries but for r = 6, the dictionaries are very similar. This suggests that for SVD, six principal components are sufficient to accurately represent the subspace upon which the sunspot patches lie. This is consistent with the results of Moon et al. (2015) where the intrinsic dimension is found to be less than 6 for most patches.
Difference between dictionaries learned from the collection of sunspot patches corresponding to the different Mount Wilson types as measured by the Grassmannian metric d_{G}, e.g. d_{G} (A_{α}, A_{β}). Dictionaries are learned using random subsets of the data and the results are reported in the form of mean ± standard deviation using 100 trials. Different sizes of dictionaries r are used. The SVD results are sensitive to r.
Interestingly, for the r = 5 SVD results, the βγ group is the most dissimilar to the other groups while being relatively similar to itself. In contrast, the β group is fairly dissimilar to itself and relatively similar to the α and βγδ groups.
The NMF results are less sensitive to r. The average difference between the dictionaries and its standard deviation is larger when r = 9 compared to when r = 8. However, for a given r, all of the mean differences are within a standard deviation of each other. Thus on aggregate, the NMF dictionaries learned from large collections of patches from multiple images differ from each other to the same degree regardless of the Mount Wilson type.
3.2. Hellinger distance comparisons
For the Hellinger distance, we learn a dictionary A and the coefficient matrix H for the entire dataset Z. We then separate the coefficients in H according to the Mount Wilson type and compare the coefficient distributions using the Hellinger distance. For example, suppose that the data matrix is arranged as Z = (Z_{α}Z_{β}Z_{βγ}Z_{βγδ}). This is factored as Z = A(H_{α}H_{β}H_{βγ}H_{βγδ}). To compare the α and β groups, we assume that the columns in H_{α} are samples from the distribution f_{α} and similarly H_{β} contains samples from the distribution f_{β}. We then estimate the Hellinger distance H(f_{α}, f_{β}) using the divergence estimator in Moon & Hero III (2014a).
When the Hellinger distance is used to compare the collections of dictionary coefficients within the sunspots, the groups are very similar, especially when using SVD (Table 4). This indicates that when the coefficients of all ARs from one class are grouped together, the distribution looks similar to the distribution of the other classes. However, there are some small differences. First the intraclass distances are often much smaller than the interclass distances which indicates that there is some relative difference between most classes. Second, for both matrix factorization methods, the βγδ groups are the most dissimilar. This could be due to the presence of a δ spot configuration, where umbrae of opposite polarities are within a single penumbra. Such a configuration may require specific linear combinations of the dictionary elements as compared to the other classes. The presence and absence of these linear combinations in two Mount Wilson types would result in a higher Hellinger distance between them.
Difference between the collection of dictionary coefficients pooled from the different Mount Wilson classes as measured by the Hellinger distance. Intraclass distances are reported in the form of mean ± standard deviation and are calculated by randomly splitting the data and then calculating the distance over 100 trials. The size of the dictionaries is r = 6 and 8 for SVD and NMF, respectively. The βγδ group is most dissimilar to the others.
Again, for clustering, we compute the pairwise Hellinger distance between each AR’s collection of coefficients. This is done by forming the data matrix from the 424 ARs as Z = (Z_{1}Z_{2} … Z_{424}) and factoring it as Z = A(H_{1}H_{2} … H_{424}). The columns of H_{i} are samples from a distribution f_{i} and the distributions f_{i} and f_{j} are compared by estimating H(f_{i}, f_{j}). The corresponding dictionaries for the two methods are shown in Figures 4 and 5.
Table 5 gives the average pairwise Hellinger distance between the ARs. The average distances differ more with the NMFbased coefficients resulting in larger dissimilarity. The average distance is smallest when comparing the β groups to all others and largest when comparing the βγ groups to the rest. The standard deviation is also larger when comparing α and β groups. This may be partially related to the variability in estimation due to smaller sample sizes as the α and β groups contain more of the smaller ARs (see Fig. 2). Overall, the average distances show that there are clear differences between the ARs within the sunspots using this metric.
Average pairwise difference between dictionary coefficients from each AR from different Mount Wilson types as measured by the Hellinger distance. Results are reported in the form of mean ± standard deviation. The size of the dictionaries is r = 6 and 8 for SVD and NMF, respectively. The βγ ARs are most dissimilar to each other and the other classes while the β ARs are most similar.
4. Clustering of active regions: methods
4.1. Clustering algorithm
The clustering algorithm we use is the Evidence Accumulating Clustering with Dual rooted Prim tree Cuts (EACDC) method in Galluccio et al. (2013) which scales well for clustering in high dimensions. EACDC clusters the data by defining a metric based on the growth of two minimal spanning trees (MSTs) grown sequentially from a pair of points. To grow the MSTs, a base dissimilarity measure is required as input such as the Hellinger distance described in Section 2.4. From the new metric defined using the MSTs, a similarity measure between inputs is created. It is fed into a spectral clustering algorithm that groups together inputs which are most similar. The similarity measure based on the MSTs adapts to the geometry of the data, and this results in a clustering method that is robust and competitive with other algorithms (Galluccio et al. 2013). See Appendix A.2 for more details.
4.2. Clustering input: dictionary sizes
As input to the clustering algorithm, we use the matrix factorization results as described in Section 2.4. We learn a single dictionary from the entire dataset. We then project the data onto a lower dimensional space, i.e. we learn the coefficient matrices H_{i}. These matrices are the inputs in this method and the base dissimilarity measure is the Hellinger distance estimated using each AR’s respective coefficients. Table 6 provides a summary of the various dissimilarity and similarity measures that we use.
Summary of the dissimilarity and similarity measures used.
As mentioned in Section 2, the estimated intrinsic dimension from Moon et al. (2015) is used to provide an initial estimate for the size of the dictionaries r. The choice of r is further refined by the dictionary comparison results from Section 3. For SVD, we choose r to be one standard deviation above the mean intrinsic dimension estimate which is approximately 5 or 6. When comparing the dictionary coefficients, we want the single dictionary to accurately represent the images. The dictionary should not be too large as this may add spurious dictionary elements due to the noise. The results in Table 3 suggest that for SVD, the dictionaries are essentially identical for r = 6. This means that six dictionary elements are sufficient to accurately reconstruct most of the images. This is consistent with the intrinsic dimension estimates in Moon et al. (2015). Thus we choose r = 6 when using the Hellinger distance for the SVD dictionary coefficients.
Since our mixed version of NMF requires approximately 1.5 times the number of dictionary elements as SVD (see Sect. 2.1), we choose r = 8 within the sunspots. Since the differences between classes were similar for r = 8 and r = 9, choosing r = 8 strikes a balance between accurate representation of the data and limiting the effects of noise.
4.3. Clustering input: patches within sunspots and along the neutral line
Our main focus up to this point in this paper has been on data matrices Z containing the patches within the STARA masks, that is, within sunspots. The clustering based on these patches is discussed in Sections 5.1 and 5.2.
It is well known, however, that the shape of the neutral line separating the main polarities plays an important role in the Mount Wilson classification. For this reason, we conduct two experiments involving data from along the neutral line.
The results of the first experiment are given in Section 5.3 where we apply matrix factorization on a data matrix containing only the patches situated along the neutral line using the same ARs as in Sections 5.1 and 5.2. To compute the location of a neutral line in this experiment, we assume it is situated in the middle between regions of opposite polarity, and proceed as follows. First, we determine regions of high magnetic flux of each polarity using an absolute threshold at 50 Gauss. Second, we compute for each pixel the distance to the closest high flux region in each polarity using the Fast Marching method (Sethian 1995). Once the two distance fields (one for each polarity) are calculated, the neutral line can be obtained by finding the pixels that lie on or are close to the zero levelset of the difference of these two distance fields. In this paper, we choose a maximum distance of 10 pixels to determine the neutral line region.
We extract the patches that lie in the neutral line region and within the SMART mask associated to the AR. Call the resulting data matrix Z_{N}. We then apply SVD or NMF matrix factorization as before and calculate the pairwise distance between each AR neutral line using the Hellinger distance on the results. Define the resulting 424 × 424 dissimilarity matrix as D_{N} for whichever factorization method we are currently using. Similarly, define Z_{S} and D_{S} as the respective data matrix and dissimilarity matrix of the data from within the sunspots using the same configuration. The base dissimilarity measure D inputted in the clustering algorithm is now a weighted average of the distances computed within the neutral line regions and within the sunspots: D = _{w}D_{N} + (1 − w)D_{S} where 0 ≤ w ≤ 1. Using a variety of weights, we then compare the clustering output to different labeling schemes based on the Mount Wilson labels as shown in Table 7.
The labels used to compare with the clustering results when analyzing the effects of including the neutral line.
For the second experiment, we perform clustering on a ROI that selects pixels along a strong field polarity reversal line. The high gradients near strong field polarity reversal lines in LOS magnetograms are a proxy for the presence of nearphotospheric electrical currents, and thus might be indicative of a nonpotential configuration (Schrijver 2007). To compute this ROI, the magnetograms are first reprojected using an equalarea, sinusoidal reprojection that uses SingularValue Padding (DeForest 2004). The latter is known to be more accurate than image interpolation on transformed coordinates. To conserve flux, the magnetograms are also areanormalized.
In the reprojected magnetograms, we delimit an AR using sunspot information from the Debrecen catalog (Győri et al. 2010) to obtain the location of all the pixels that belong to the spots related to an AR (called “Debrecen spots” hereafter). The ROI consists of a binary array constructed as follows:

The pixels that belong to the Debrecen spots are assigned the scalar value 1 and all others are assigned the scalar value −1.

From this twovalued array, we retrieve the distances from the zero levelset using a fast marching method (Sethian 1995) implemented in the Python SciKits’ module “scikitfmm”.

We mask out the pixels within a distance of 80 pixels from the zero levelset (in the equalareareprojected coordinate system).

The ROI is delimited by the convex hull of the resulting mask, that is, the smallest convex polygon that surrounds all 1valued pixels. The resulting mask is a binary array with the pixels inside the convex hull set to True.
Within the ROI, the Rvalue is calculated similarly to the method described in Schrijver (2007). We dilate the image using a dilation factor of three pixels, and extract the flux using overlapping Gaussian masks with σ = 2 px. Integrating the nonzero values outputs the Rvalue, i.e, the total flux in the vicinity of the polarityinversion line.
We then perform an image patch analysis using image patches from this region. We do this by using either SVD or NMF to do dimensionality reduction on the patches, and then estimate the Hellinger distance between ARs using the reduceddimension representation. We exclude α groups from the analysis as they do not have a strong field polarity reversal line. This leaves 420 images to be clustered. The clustering assignments are then compared to the calculated Rvalue via the correlation coefficient. The results are presented in Section 5.4.
5. Clustering of active regions: results
Given the choices of matrix factorization techniques (NMF and SVD) we have two different clustering results on the data. Section 5.1 focuses on the clusterings using data from within the sunspots, and Section 5.2 provides some recommendations for which metrics and matrix factorization techniques to use to study different ARs. The neutral line clustering results are then given in Section 5.3 followed by the Rvalue based experiment in Section 5.4.
5.1. Clustering within the sunspot
We now present the clustering results when using the Hellinger distance as the base dissimilarity. The corresponding dictionary elements to the coefficients are represented in Figure 4 (for the SVD factorization) and in Figure 5 (for the NMF).
The EACDC algorithm does not automatically choose the number of clusters. We use the mean silhouette heuristic to determine the most natural number of clusters as a function of the data (Rousseeuw 1987). The silhouette is a measure of how well a data point belongs to its assigned cluster. The heuristic chooses the number of clusters that results in the maximum mean silhouette. In both clustering configurations, the number of clusters that maximizes the mean silhouette is 2 so we focus on the two clustering case for all clustering schemes throughout.
To compare the clustering correspondence, we use the adjusted Rand index (ARI). The ARI is a measure of similarity between two clusterings (or a clustering and labels) and takes values between −1 and 1. A 1 indicates perfect agreement between the clusterings and a 0 corresponds to the agreement from a random assignment (Rand 1971). Thus a positive ARI indicates that the clustering correspondence is better than a random clustering while a negative ARI indicates it is worse. The ARI between the NMF and SVD clusterings is 0.27 which indicates some overlap.
Visualizing the clusters in lower dimensions is done with multidimensional scaling (MDS) as in Moon et al. (2014). Let S be the 424 × 424 symmetric matrix that contains the AR pair similarities as created by EACDC algorithm. MDS projects the similarity matrix S onto the eigenvectors of the normalized Laplacian of S (Kruskal & Wish 1978). Let be the projection onto the ith eigenvector of S using NMF. The first eigenvector represents the direction of highest variability in the matrix S, and hence a high value of the kth element of c_{1} indicates that the kth AR is dissimilar to other ARs.
Figure 6 displays the scatter plot of c_{1} vs. c_{2} (top) and c_{1} vs. c_{3} (bottom) using NMF. Comparing them with the Mount Wilson classification we see a concentration of simple ARs in the region with highest c_{1} values (most dissimilar ARs), and a concentration of complex ARs in the region with lowest c_{1} (more similar ARs). We can show this more precisely by computing the mean similarity of the ith AR to all other ARs as the mean of the ith row (or column) of S. The value from c_{1} is then inversely related to this mean similarity as seen in Figure 7.
Fig. 6. Scatter plot of MDS variables c_{1} vs. c_{2} (a, b) and c_{1} vs. c_{3} (c, d) where is the projection of the similarity matrix onto the ith eigenvector of the normalized Laplacian of the similarity matrix when using the NMF coefficients. Each point corresponds to one AR and they are labeled according to the clustering (a, c) and the Mount Wilson labels (b, d). In this space, the clusters data appear to be separable and there are concentrations of complex ARs in the region with lowest c_{1} values. Other patterns are described in the text. 
Fig. 7. Mean similarity of an AR with all other ARs as a function of its MDS variable c_{1} using NMF. Cluster 2 is associated with those ARs that are most similar to all other ARs while Cluster 1 contains those that are least similar to all others. 
The similarity defined under this clustering scheme gathers in Cluster 2 “similar” ARs that are for a large part of the types βγ and βγδ, whereas Cluster 1 contains ARs that are more dissimilar’ to each other, with a large part of α or β active regions. The other clustering configuration has a similar relationship between the first MDS coefficient and the mean similarity.
Table 8 makes this clearer by showing the mean similarity measure within each cluster and between the two clusters, which is calculated in the following manner. Suppose that the similarity matrix is organized in block form where the upper left block corresponds to Cluster 1 and the lower right block corresponds to Cluster 2. The mean similarity of Cluster 1 is calculated by taking the mean of all the values in the upper left block of this reorganized similarity matrix. The mean similarity of Cluster 2 is found similarly from the lower right block and the mean similarity between the clusters is found from either the lower left or upper right blocks. These means show that under the NMF clustering scheme, ARs in Cluster 2 are very similar to each other while ARs in Cluster 1 are not very similar to each other on average. In fact, the ARs in Cluster 1 are more similar to the ARs in Cluster 2 on average than to each other. The other clustering configuration has a similar relationship between cluster assignment and mean similarity.
Mean similarity of ARs to other ARs either in the same cluster (1 vs. 1 or 2 vs. 2) or in the other cluster (1 vs. 2) under the different schemes. Cluster 1 contains ARs that are very dissimilar to each other while Cluster 2 contains ARs that are very similar to each other.
This relationship between AR complexity and clustering assignment is further noticeable in Figure 8 which gives a histogram of the Mount Wilson classes divided by clustering assignment. This figure shows clear patterns between the clusterings and Mount Wilson type distribution, where the clustering separates somewhat the complex sunspots from the simple sunspots. This suggests that these configurations are clustering based on some measure of AR complexity.
Fig. 8. Histograms of the Mount Wilson classes divided by clustering assignment using the Hellinger distance. Cluster 1 contains more of the complex ARs while Cluster 2 contains more of the simple ARs. 
The Hellingerbased clusterings are correlated with sunspot size for some of the Mount Wilson classes, see Table 9. Based on the mean and median number of pixels, the Hellinger distance on the NMF coefficients tends to gather in Cluster 2 the smallest AR from classes α, β, and βγ. Similarly, the Hellinger distance on the SVD coefficients separates the β and βγ AR by size with Cluster 1 containing the largest and Cluster 2 containing the smallest AR.
Mean and median number of pixels of the ARs in each cluster under the Hellinger clustering schemes. Cluster 1 contains the larger sunspots for all groups when using NMF and for some of the groups when using SVD.
Since the Hellinger distance calculates differences between ARs based on their respective distribution of dictionary coefficients, we can examine the coefficient distribution to obtain insight on what features the clustering algorithm is exploiting. For simplicity, we examine the marginal histograms of the coefficients pooled from ARs of a given cluster. When looking at the SVD coefficients, we see that their marginal distributions are similar across clusters, except for the coefficients that correspond to the second dictionary element of Figure 4. Recall that this second dictionary element is associated with the average magnetic field value of a patch. If the corresponding coefficient is close to zero, it means the average magnetic field in the patch is also close to zero.
Figure 9 shows histograms of the coefficients of the second dictionary element. The histograms correspond to patches from all ARs separated by cluster assignment. The histograms show that Cluster 1 has a high concentration of patches with near zero average magnetic field. In contrast, the larger peaks for Cluster 2 are centered around +1 and −1. This suggests that the clustering assignments are influenced somewhat by the amount of patches in an AR that have near zero average magnetic field values. As we are considering only the core (sunspot) part of the AR, having 3 × 3 patch with a near zero average magnetic field entails that the corresponding patch is likely to be located along the neutral line separating strong magnetic fields of opposite polarity. Thus the local distribution of magnetic field values is related to cluster assignments when using the SVD coefficients. This is consistent with Figure 8 where Cluster 1 contains more of the complex ARs (βγ and βγδ) and fewer simple ARs (α and β) than Cluster 2 as measured by the Mount Wilson scheme.
Fig. 9. Histograms of the marginal distributions of the coefficients corresponding to the mean magnetic field value (dictionary element 2 in Fig. 3) for Cluster 1 (left) and Cluster 2 (right) using the SVD coefficients. Cluster 1 ARs contain more patches with near neutral magnetic field values. 
Checking the individual ARs and their coefficient distributions in each cluster, we see indeed that Cluster 1 does contain more ARs with patches having near zero average magnetic field. This tends to include more of the complex ARs in Cluster 1 since they are more likely to have a neutral line close to the regions of strong magnetic fields that will therefore be included in the STARA masks.
It should be noted however that the correspondence is not perfect. There are some ARs in Cluster 2 where the regions of opposing polarity are close to each other and some ARs in Cluster 1 where the regions of opposing polarity are far apart. Thus the distribution of average magnetic field values is only one factor in the natural geometry of the ARs defined by the Hellinger distance. As mentioned previously, the size of the AR is another factor, especially for β groups. This is consistent with Figure 8 where Cluster 1 does contain some of the simple ARs which are less likely to have strong magnetic fields around the neutral line.
Investigating the joint histograms of the NMF dictionary elements corresponding to positive and negative magnetic field values reveals that the NMF Hellinger clustering results are also influenced by the local magnetic field distribution.
All these observations indicate that the natural geometry exploited by both clustering configurations is related to some form of complexity of the ARs.
5.2. Discussion of sunspot results
We note that the Cluster 2 ARs containing the smallest sunspots are most similar to each other while the Cluster 1 ARs are more dissimilar (see Tables 8 and 9). This indicates that the Hellinger distance approaches are best for distinguishing between different types of larger or complex ARs.
When NMF is applied on datasets where all values in the dictionary and coefficient matrices are constrained to be nonnegative, its results are generally more interpretable than SVD. In our application however, the magnetogram components can be negative. Hence the NMF results are not particularly sparse and lose some benefits of nonnegativity since the positive and negative magnetogram components can cancel each other. This results in some loss of interpretability. Additionally, the SVD results seem to be more interpretable due to separate treatment of the continuum and magnetogram components. However, there is still some value in the NMF approach as we see that the clustering on NMF coefficients is better at separating the ARs by size than the SVD approach. Additionally, the NMF approaches tend to agree more strongly with the Mount Wilson labels than their SVD counterparts as is seen in Section 5.3 below. Future work could include using alternate forms of NMF such as in Ding et al. (2010) where sparsity and interpretability is preserved even when the dictionary is no longer constrained to be nonnegative. Another variation in coupled NMF that may be applicable is soft NMF (Seichepine et al. 2014) where the requirement that the two modalities share the same regression coefficients is relaxed somewhat. Finally, future work could perform factorization using a composite objective function comprised of two terms corresponding to the two modalities that are scaled according to their noise characteristics.
5.3. Clustering with neutral line data
As described in Section 4.3, we analyze the effects of including data from the neutral line in the clustering. We proceed by taking a weighted average of the dissimilarities calculated from the sunspots and from the neutral line data matrices. Using the ARI, we compare the results to labels based on the Mount Wilson classification scheme, see Table 7 for the label definition. We use a grid of weights, starting from a weight of 0 for a clustering using only patches within sunspots up to a weight of 1 for a clustering that takes into account only the neutral line data.
Figure 10 plots the ARI for the four different schemes as a function of the weight. In nearly all cases, the ARI is above zero which indicates that the clustering does slightly better than a random assignment. In general, the correspondence of the clustering results with the Mount Wilson based labels decreases as the weight approaches 1. This means that the natural clusterings associated with only the neutral line data do not correspond as well with the Mount Wilson based labels. However in several cases, including some information from the neutral line at lower weights appears to increase the correspondence, e.g., the ARI increases for the three and four cluster cases for the SVD coefficients. This suggests that the neutral line and the sunspots contain information about AR complexity that may be different.
Fig. 10. Plot of the adjusted Rand index (ARI) using and Hellinger distances within the neutral line and sunspots as a function of the weight. A weight of 0 corresponds to clustering with only the sunspots while a weight of 1 clusters with only the neutral line. The different lines correspond to different numbers of clusters and the corresponding labels from Table 6. Higher ARI indicates greater correspondence. 
Note that clustering separates the ARs based on the natural geometry in the spaces we are considering. Thus we can influence the clustering by choosing the space. For example, if we restrict our analysis to include only coefficients corresponding to specific dictionary patches, then this will influence the clustering.
The gradients of magnetic field values across the neutral line are a key quantity used in several indicators of potential eruptive activity (Schrijver 2007). We therefore repeated the neutral line experiment where we focused only on the gradients within the magnetogram as follows. When we applied SVD to the data matrix Z extracted from the neutral line, the resulting dictionary matrix A was very similar to that shown in Figure 4. Note that elements 3 and 4 correspond to the gradient patterns within the magnetogram data. Therefore, after learning A and H from Z, we kept only the coefficients corresponding to dictionary elements 3 and 4, i.e. the 3rd and 4th rows of H. We then estimated the Hellinger distance between the ARs’ underlying distributions of these two coefficients. This restricted the neutral line analysis to include only the coefficients corresponding to magnetogram gradients. For the data within the sunspots, we included all coefficients as before.
Figure 11 shows the ARI as a function of the weight for this experiment. For all cases, the ARI stays fairly constant until the weight increases to 0.9, after which it drops dramatically. We can compare this to the results in Figure 10a to determine if using only the neutral line gradient coefficients results in increased correspondence with the Mount Wilson labels relative to using all of the neutral line coefficients. From this comparison, the ARI is higher when using only the gradient components for weights greater than 0.1 and less than 1. Thus the correspondence with the Mount Wilson labels and the clustering is higher when we only include the magnetogram gradient coefficients. Since the Mount Wilson scheme is related to the complexity of the neutral line, this higher correspondence suggests that focusing on the gradients in the neutral line results in a natural geometry that is more closely aligned with the complexity of the neutral line than simply using all of the coefficients. Applying supervised techniques would lead to improved correspondence.
Fig. 11. Plot of the ARI using the Hellinger distance within the neutral line on only the coefficients corresponding to the SVD dictionary elements associated with magnetogram gradients. The corresponding dictionary elements are similar to the third and fourth elements in Figure 4. Focusing on the gradients results in a higher ARI for higher weights than when all coefficients are used as seen in Figure 10. 
The clear patterns in the ARI indicate that the relationship between the weight and the ARI is unlikely to be due entirely to noise. Thus including data from the neutral line with the data from the sunspots would add value in an unsupervised setting and would likely lead to improved performance in a supervised setting.
5.4. Clustering of regions exhibiting strong field polarity reversal lines
We now analyze ARs exhibiting strong field polarity reversal lines by comparing the natural clustering of these ARs to the calculated Rvalue as described in Section 4.3. When we apply dimensionality reduction on this data using SVD, the resulting dictionary is very similar to Figure 4 with the first two patches consisting of uniform nonzero patches, the third and fourth patches consisting of gradients in the magnetogram, and the fifth and sixth patches consisting of gradients in the continuum.
As before, the mean silhouette width indicates that the appropriate number of clusters is 2. When we cluster the ARs using the SVD coefficients corresponding to all six patches, we obtain a correlation between cluster assignment and R of 0.09 (see Table 10). This isn’t particularly high which suggests that the natural geometry based on the distribution of all six coefficients does not correlate well with R. However, since the clustering is separating the ARs based on the natural geometry in the spaces we are considering, we can influence the clustering by choosing the space. In other words, if we restrict our analysis to only coefficients corresponding to specific dictionary patches, then this will influence the clustering.
Magnitude of the correlation coefficient of the clustering assignment with either R or log R when using all of the coefficients, only the coefficients corresponding to the magnetogram component (SVD elements 2–4 in Fig. 4), or only magnetogram gradient coefficients (SVD elements 3 and 4 in Fig. 4). For NMF, all of the dictionary elements are associated with the magnetogram and many of them have gradient components so we only perform clustering with all of the coefficients.
Restricting the clustering analysis to the SVD coefficients corresponding only to the magnetogram components (i.e. elements 2, 3, and 4 in Fig. 4) results in a correlation of 0.30 between cluster assignment and Rvalue. If we only consider the gradient components (elements 3 and 4), then the correlation is 0.34.
The relationship between cluster assignment and R may not be linear as the correlation between the clustering assignment using only the gradient components and log R is 0.45. Comparing the magnetogram only componentsbased clustering with log R similarly increases the correlation coefficient. Given that clustering is an unsupervised method and that we are only clustering into two groups, this correlation is quite high. This suggests that the natural geometry of the image patch analysis increasingly corresponds with R as we restrict the analysis to magnetogram gradients. Supervised methods, such as regression, should lead to an even greater correspondence. Additionally, since the correlation is not perfect, this suggests that there is information in the image patch analysis that is not present in the Rvalue which may be useful for AR analysis.
For NMF, when we include all of the coefficients, the correlation between R and clustering assignment is 0.15. While this is small, we are again comparing the labels of an unsupervised approach to a continuum of values. Thus we can expect that the performance would be better in a supervised setting. If we compare the clusering to log R, the correlation decreases to 0.08. It is difficult to restrict the NMF dictionary to only continuum and magnetogram parts and gradients as most of the components contain a gradient component in the magnetogram. Therefore we only cluster the ARs using all NMF coefficients.
6. Conclusion
In this work, we introduce a reduceddimension representation of an AR that allows a datadriven unsupervised classification of ARs based on their local geometry. The ROI that surrounds and includes the AR represents its most salient part and must be provided by the user. We used STARA masks in conjunction with masks situated around the neutral line, and compared our results with the Mount Wilson classification in order to ease interpretation of the unsupervised scheme.
The Mount Wilson scheme focuses on the largest length scale when describing the geometrical arrangements of the magnetic field, whereas our method focuses on classifying ARs using information from fine length scale. We have shown that when we analyze and cluster the ARs based on the global statistics of the local properties, there are similarities to the classification based on the large scale characteristics. For example, when clustering using the Hellinger distance, one cluster contained most of the complex ARs. Other large scale properties such as the size of the AR also influenced the clustering results. Table 11 summarizes the properties that are found to influence the clustering under the two schemes.
Summary of features distinguishing the clusters under the various classification schemes tested.
In this comparison with the Mount Wilson scheme, we found that the STARA masks were sometimes too restrictive which led to a mismatch between the Mount Wilson label and the extracted data. For example, there were several cases where an AR was labeled as a β class but the STARA mask only extracted magnetic field values of one polarity. We showed that the neutral line contains additional information about the complexity of the AR. For this reason, we expect that including information beyond the STARA masks will lead to improved matching with the Mount Wilson labels.
To investigate the possibility for our method to distinguish between potential and nonpotential fields, we considered a ROI made of pixels situated along highgradient, strong field polarity reversal lines. This is the same ROI as that used in the computation of the Rvalue, which has proved useful in flare prediction in a supervised context. We found that our clustering was correlated with the Rvalue, that is, the clustering based on the reduceddimension representation separates ARs corresponding to low R from the ones with large R.
In future work, we plan to study the efficiency of supervised techniques applied to the reduced dimension representation. Supervised classification can always do at least as well as unsupervised learning in the task of reproducing class labels (e.g. Mount Wilson label). Indeed, in supervised classification, a training dataset with labels must be provided. A classifier (or predictor) is then built within the input feature space, and is used to provide a label to new observations. In contrast, unsupervised classification or clustering separates the ARs naturally based on the geometry of the input feature space and does not use labels. Thus if the goal is for example to reproduce the Mount Wilson classes, or to detect nonpotentiality using global statistics of local properties, then supervised methods would lead to increased correspondence relative to our unsupervised results.
In case of flare prediction, the labels would be some indicator of flare activity such as the strength of the largest flare that occurred within a specified time period after the image was taken. Supervised techniques such as classification or regression could be applied depending on the nature of the label (i.e. categorical vs. continuum).
A good way of assessing how well a given feature space can do in a supervised setting is to estimate the Bayes error. The Bayes error gives the minimum average probability of error that any classifier can achieve on the given data and can be estimated in the two class setting by estimating upper and lower bounds such as the Chernoff bound using a divergencebased estimator as in Moon & Hero III (2014b). These bounds can be estimated using various schemes and combinations of data (inside sunspots, along the neutral line, etc.) to determine which scheme is best at reproducing the desired labels (e.g., the Mount Wilson labels). This can also be done in combination with physical parameters of the ARs such those used in Bobra & Couvidat (2015) (e.g. the total unsigned flux, the total area, the sum of flux near the polarityinversion line, etc.).
These methods of comparing AR images can also be adapted to a time series of image pairs. For example, image pairs from a given point in time may be compared to the image pairs from an earlier period to measure how much the ARs have changed. The evolution of an AR may also be studied by defining class labels based on the results from one of the clustering schemes in this paper. From the clustering results, a classifier may be trained that is then used to assign an AR to one of these clusters at each time step. The evolution of the AR’s cluster assignment can then be examined.
Acknowledgments
This work was partially supported by the US National Science Foundation (NSF) under Grant CCF1217880 and a NSF Graduate Research Fellowship to KM under Grant No. F031543. VD acknowledges support from the Belgian Federal Science Policy Office through the ESAPRODEX program, Grant No. 4000103240, while RDV acknowledges support from the BRAIN.be program of the Belgian Federal Science Policy Office, Contract No. BR/121/PI/PREDISOL. We thank Dr. Laura Balzano at the University of Michigan, as well as Dr. Laure Lefèvre, Dr. Raphael Attie, and Ms. Marie Dominique at the Royal Observatory of Belgium for their feedback on the manuscript. The authors gratefully acknowledge Dr. Paul Shearer’s help in implementing the modified NMF algorithm. The editor thanks two anonymous referees for their assistance in evaluating this paper.
References
 Ahmed, O.W., R. Qahwaji, T. Colak, P.A. Higgins, P.T. Gallagher, and D.S. Bloomfield. Solar flare prediction using advanced feature extraction, machine learning, and feature selection. Sol. Phys., 283, 157–175, 2013, DOI: 10.1007/s1120701198961. [NASA ADS] [CrossRef] [Google Scholar]
 Barnes, G., K.D. Leka, E.A. Schumer, and D.J. DellaRose. Probabilistic forecasting of solar flares from vector magnetogram data. Space Weather, 5, S09002, 2007, DOI: 10.1029/2007SW000317. [CrossRef] [Google Scholar]
 Bazot, C., N. Dobigeon, J.Y. Tourneret, A. Zaas, G. Ginsburg, and A.O. HeroIII. Unsupervised Bayesian linear unmixing of gene expression microarrays. BMC Bioinf., 14 (1), 99, 2013, DOI: 10.1186/147121051499. [CrossRef] [Google Scholar]
 Bhattacharyya, A. On a measure of divergence between two multinomial populations. Sankhya, 7 (4), 401–406, 1946. [Google Scholar]
 BioucasDias, J.M., A. Plaza, N. Dobigeon, M. Parente, Q. Du, P. Gader, and J. Chanussot. Hyperspectral unmixing overview: geometrical, statistical, and sparse regressionbased approaches. IEEE J. Sel. Topics Appl. Earth Observations Remote Sensing, 5 (2), 354–379, 2012. [CrossRef] [Google Scholar]
 Bobra, M.G., and S. Couvidat. Solar flare prediction using SDO/HMI vector magnetic field data with a machinelearning algorithm. Astrophys. J., 798, 135, 2015, DOI: 10.1088/0004637X/798/2/135. [NASA ADS] [CrossRef] [Google Scholar]
 Colak, T., and R. Qahwaji. Automated McIntoshbased classification of sunspot groups using MDI images. Sol. Phys., 248, 277–296, 2008, DOI: 10.1007/s1120700790943. [NASA ADS] [CrossRef] [Google Scholar]
 Colak, T., and R. Qahwaji. Automated solar activity prediction: a hybrid computer platform using machine learning and solar imaging for automated prediction of solar flares. Space Weather, 7, S06001, 2009, DOI: 10.1029/2008SW000401. [NASA ADS] [CrossRef] [Google Scholar]
 Comon, P., and C. Jutten. Handbook of Blind Source Separation: Independent Component Analysis and Blind Deconvolution. Academic Press, Oxford, 2010. [Google Scholar]
 Csiszar, I. Informationtype measures of difference of probability distributions and indirect observations. Studia Sci. Math. Hungar., 2, 299–318, 1967. [Google Scholar]
 DeForest, C. On resampling of solar images. Sol. Phys., 219 (1), 3–23, 2004. [NASA ADS] [CrossRef] [Google Scholar]
 Ding, C., T. Li, and M.I. Jordan. Convex and seminonnegative matrix factorizations. IEEE Trans. Pattern Anal. Mach. Intell., 32 (1), 45–55, 2010. [CrossRef] [Google Scholar]
 Dudok de Wit, T., S. Moussaoui, C. Guennou, F. Auchère, G. Cessateur, M. Kretzschmar, L.A. Vieira, and F.F. Goryaev. Coronal temperature maps from solar EUV images: a blind source separation approach. Sol. Phys., 283, 31–47, 2013, DOI: 10.1007/s1120701201422. [CrossRef] [Google Scholar]
 Edelman, A., T.A. Arias, and S.T. Smith. The geometry of algorithms with orthogonality constraints. SIAM J. Matrix Anal. Appl., 20 (2), 303–353, 1998. [CrossRef] [Google Scholar]
 Falconer, D.A., R.L. Moore, and G.A. Gary. Magnetogram measures of total nonpotentiality for prediction of solar coronal mass ejections from active regions of any degree of magnetic complexity. Astrophys. J., 689, 1433–1442, 2008, DOI: 10.1086/591045. [NASA ADS] [CrossRef] [Google Scholar]
 Galluccio, L., O. Michel, P. Comon, M. Kliger, and A.O. HeroIII. Clustering with a new distance measure based on a dualrooted tree. Inform. Sciences, 251, 96–113, 2013. [CrossRef] [Google Scholar]
 Georgoulis, M.K., and D.M. Rust. Quantitative forecasting of major solar flares. Astrophys. J. Lett., 661, L109–L112, 2007, DOI: 10.1086/518718. [NASA ADS] [CrossRef] [Google Scholar]
 Guo, J., H. Zhang, O.V. Chumak, and Y. Liu. A quantitative study on magnetic configuration for active regions. Sol. Phys., 237, 25–43, 2006, DOI: 10.1007/s1120700620812. [NASA ADS] [CrossRef] [Google Scholar]
 Győri, L., T. Baranyi, and A. Ludmány. Photospheric data programs at the Debrecen observatory. Proc. Int. Astron. Union, 6 (S273), 403–407, 2010. [CrossRef] [Google Scholar]
 Hale, G.E., F. Ellerman, S.B. Nicholson, and A.H. Joy. The magnetic polarity of sunspots. Astrophys. J., 49, 153, 1919, DOI: 10.1086/142452. [NASA ADS] [CrossRef] [Google Scholar]
 Hellinger, E. Neue Begründung der Theorie quadratischer Formen von unendlichvielen Veränderlichen. Journal für die reine und angewandte Mathematik, 136, 210–271, 1909. [Google Scholar]
 Higgins, P.A., P.T. Gallagher, R. McAteer, and D.S. Bloomfield. Solar magnetic feature detection and tracking for space weather monitoring. Adv. Space Res., 47 (12), 2105–2117, 2011. [NASA ADS] [CrossRef] [Google Scholar]
 Huang, X., D. Yu, Q. Hu, H. Wang, and Y. Cui. Shortterm solar flare prediction using predictor teams. Sol. Phys., 263, 175–184, 2010, DOI: 10.1007/s1120701095423. [NASA ADS] [CrossRef] [Google Scholar]
 Jolliffe, I.T. Principal Component Analysis, 2nd ed., SpringerVerlag New York, Inc., New York, 2002. [Google Scholar]
 Kruskal, J.B., and M. Wish. Multidimensional Scaling, vol. 11, Sage, New York, 1978. [CrossRef] [Google Scholar]
 Kullback, S., and R.A. Leibler. On information and sufficiency. Ann. Math. Stat., 22, 79–86, 1951. [CrossRef] [MathSciNet] [Google Scholar]
 Künzel, H. Die FlareHäufigkeit in Fleckengruppen unterschiedlicher Klasse und magnetischer Struktur. Astron. Nachr., 285, 271–271, 1960. [NASA ADS] [CrossRef] [Google Scholar]
 Langville, A.N., C.D. Meyer, R. Albright, J. Cox, and D. Duling. Initializations for the nonnegative matrix factorization, in Proceedings of the Twelfth ACM SIGKDD International Conference on Knowledge Discovery and Data Mining, Philadelphia, USA, Citeseer, 2006. [Google Scholar]
 Lee, D.D., and H.S. Seung. Algorithms for nonnegative matrix factorization, in Advances in Neural Information Processing Systems (NIPS), 556–562, 2001. [Google Scholar]
 Lee, K., Y.J. Moon, J.Y. Lee, K.S. Lee, and H. Na. Solar flare occurrence rate and probability in terms of the sunspot classification supplemented with sunspot area and its changes. Sol. Phys., 281, 639–650, 2012, DOI: 10.1007/s1120701200919. [CrossRef] [Google Scholar]
 Leka, K.D., and G. Barnes. Photospheric magnetic field properties of flaring vs. flarequiet active regions III: discriminant analysis of a statistically significant database. In American Astronomical Society Meeting Abstracts #204, vol. 36 of Bulletin of the American Astronomical Society, 715, 2004. [Google Scholar]
 Lin, C.J. Projected gradient methods for nonnegative matrix factorization. Neural Comput., 19 (10), 2756–2779, 2007. [CrossRef] [Google Scholar]
 Mayfield, E.B., and J.K. Lawrence. The correlation of solar flare production with magnetic energy in active regions. Sol. Phys., 96, 293–305, 1985, DOI: 10.1007/BF00149685. [CrossRef] [Google Scholar]
 Mittelman, R., N. Dobigeon, and A. Hero. Hyperspectral image unmixing using a multiresolution sticky HDP. IEEE Trans. Signal Process., 60 (4), 1656–1671, 2012, DOI: 10.1109/TSP.2011.2180718. [CrossRef] [Google Scholar]
 Moon, K.R., and A.O. HeroIII. Ensemble estimation of multivariate fdivergence, in Information Theory (ISIT), 2014 IEEE International Symposium on, Honolulu, USA, IEEE, 356–360, 2014a. [Google Scholar]
 Moon, K.R., and A.O. HeroIII. Multivariate fdivergence estimation with confidence. Adv. Neural Inf. Process. Syst., 27, 2420–2428, 2014b. [Google Scholar]
 Moon, K.R., J.J. Li, V. Delouille, F. Watson, and A.O. HeroIII. Image patch analysis and clustering of sunspots: a dimensionality reduction approach, in IEEE International Conference on Image Processing (ICIP), Paris, France, IEEE, 1623–1627, 2014. [Google Scholar]
 Moon, K.R., J.J. Li, V. Delouille, R. De Visscher, F. Watson, and A.O. HeroIII. Image patch analysis of sunspots and active regions. I. Intrinsic dimension and correlation analysis. J. Space Weather Space Clim., 2015. [Google Scholar]
 Moon, T.K., and W.C. Stirling. Mathematical Methods and Algorithms for Signal Processing, Prentice Hall, New York, 2000. [Google Scholar]
 Prim, R.C. Shortest connection networks and some generalizations. Bell Syst. Tech. J., 36 (6), 1389–1401, 1957. [NASA ADS] [CrossRef] [Google Scholar]
 Ramírez, I., and G. Sapiro. An MDL framework for sparse coding and dictionary learning. IEEE Trans. Signal Process., 60 (6), 2913–2927, 2012. [CrossRef] [Google Scholar]
 Rand, W.M. Objective criteria for the evaluation of clustering methods. J. Amer. Statist. Assoc., 66 (336), 846–850, 1971. [CrossRef] [Google Scholar]
 Rousseeuw, P.J. Silhouettes: a graphical aid to the interpretation and validation of cluster analysis. J. Comput. Appl. Math., 20, 53–65, 1987. [CrossRef] [Google Scholar]
 Sammis, I., F. Tang, and H. Zirin. The dependence of large flare occurrence on the magnetic structure of sunspots. Astrophys. J., 540, 583–587, 2000, DOI: 10.1086/309303. [NASA ADS] [CrossRef] [Google Scholar]
 Scherrer, P.H., R.S. Bogart, R.I. Bush, J.T. Hoeksema, A.G. Kosovichev, et al. The solar oscillations investigation – Michelson Doppler imager. Sol. Phys., 162, 129–188, 1995, DOI: 10.1007/BF00733429. [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Schrijver, C.J. A characteristic magnetic field pattern associated with all major solar flares and its use in flare forecasting. Astrophys. J. Lett., 655, L117–L120, 2007, DOI: 10.1086/511857. [NASA ADS] [CrossRef] [Google Scholar]
 Seichepine, N., S. Essid, C. Févotte, and O. Cappé. Soft nonnegative matrix cofactorization. IEEE Trans. Signal Process., 62 (22), 5940–5949, 2014. [CrossRef] [Google Scholar]
 Sethian, J.A. A fast marching level set method for monotonically advancing fronts. Proc. Nat. Acad. Sci., 93, 1591–1595, 1995. [CrossRef] [Google Scholar]
 Song, H., C. Tan, J. Jing, H. Wang, V. Yurchyshyn, and V. Abramenko. Statistical assessment of photospheric magnetic features in imminent solar flare predictions. Sol. Phys., 254, 101–125, 2009, DOI: 10.1007/s1120700892883. [NASA ADS] [CrossRef] [Google Scholar]
 Stenning, D.C., T.C.M. Lee, D.A. van Dyk, V. Kashyap, J. Sandell, and C.A. Young. Morphological feature extraction for statistical learning with applications to solar image data. Stat. Anal. Data Min., 6 (4), 329–345, 2013, DOI: 10.1002/sam.11200. [CrossRef] [Google Scholar]
 Stewart, G.W. Error and perturbation bounds for subspaces associated with certain eigenvalue problems. SIAM Rev., 15 (4), 727–764, 1973. [CrossRef] [Google Scholar]
 Warwick, C.S. Sunspot configurations and proton flares. Astrophys. J., 145, 215, 1966, DOI: 10.1086/148755. [NASA ADS] [CrossRef] [Google Scholar]
 Watson, F.T., L. Fletcher, and S. Marshall. Evolution of sunspot properties during solar cycle 23. Astron. Astrophys., 533, A14, 2011, DOI: 10.1051/00046361/201116655. [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Yaghoobi, M., T. Blumensath, and M.E. Davies. Dictionary learning for sparse approximations with the majorization method, IEEE Trans. Signal Process., 57 (6), 2178–2191, 2009. [CrossRef] [Google Scholar]
 Yokoya, N., T. Yairi, and A. Iwasaki. Coupled nonnegative matrix factorization unmixing for hyperspectral and multispectral data fusion. IEEE Trans. Geosci. Remote Sens., 50 (2), 528–537, 2012. [CrossRef] [Google Scholar]
 Yu, D., X. Huang, H. Wang, Y. Cui, Q. Hu, and R. Zhou. Shortterm solar flare level prediction using a Bayesian network approach. Astrophys. J., 710, 869–877, 2010, DOI: 10.1088/0004637X/710/1/869. [NASA ADS] [CrossRef] [Google Scholar]
Appendix A: method details
A.1. Matrix factorization
As mentioned in Section 2, the goal of matrix factorization is to accurately decompose the 2m^{2} × n data matrix Z into the product of two matrices A (with size 2m^{2} × r) and H (with size r × n), where A has fewer columns than rows (r < 2m^{2}). The matrix A is the dictionary and the matrix H is the coefficient matrix. The columns of A form a basis for the data in Z.
The two matrix factorization methods we use are singular value decomposition (SVD) and nonnegative matrix factorization (NMF). These two methods can be viewed as solving two different optimization problems where the objective function is the same but the constraints differ. Let A = [a_{1}, a_{2}, …, a_{r}] and H = [h_{1}, h_{2}, … h_{n}]. For SVD, the optimization problem is
In words, SVD requires the columns of A to be orthonormal.
For standard NMF, the optimization problem iswhere a ≥ 0 applied to a vector a implies that all of a’s entries are greater than or equal to 0. In our problem, only the continuum is nonnegative so we only apply the constraint to the continuum part of the matrix A. So if a_{i} and b_{i} are both vectors with length m^{2} corresponding to the continuum and magnetogram parts, respectively, then we have . The NMF method we use also constrains the columns of H to lie on a simplex, i.e. . Thus the optimization problem for our approach to NMF is
This problem is not convex and is solved in an alternating manner by fixing H, finding the matrix A that solves the problem assuming H is fixed, and then solving for H while A is fixed. This process is repeated until the algorithm converges to a local minimum. See Lin (2007) for more details on the convergence analysis.
A.2. The EACDC clustering method
Let V = {v_{1}, v_{2},…, v_{N}} be a set of vertices and let E = {e_{ij}}, where e_{ij} denotes an edge between vertices v_{i}, v_{j}, i, j∈{1,…, N}, be a set of undirected edges between them. The pair (V, E) = G is the corresponding undirected graph. In our application, V corresponds to the set of AR image pairs being clustered and E contains all possible edges between the vertices. The weight of an edge e_{ij} is defined as w_{ij} and measures the base dissimilarity between two vertices v_{i} and v_{j}. In many applications, the base dissimilarity is the Euclidean distance. In our case, we use the Hellinger distance as the base dissimilarity measure.
A spanning tree T of the graph G is a connected acyclic subgraph that passes through all N vertices of the graph and the weight of T is the sum of all the edge weights used to construct the tree, . A minimal spanning tree of G is a spanning tree which has the minimal weight .
Prim’s algorithm (Prim 1957) is used by Galluccio et al. (2013) to construct the dual rooted MST. In Prim’s algorithm, the MST is grown sequentially where at each step, a single edge is added. This edge corresponds to the edge with minimal weight that connects a previously unconnected vertex to the existing tree. The root of the MST corresponds to the beginning vertex. For the dual rooted MST, we begin with two vertices v_{i} and v_{j} and construct the minimal spanning trees T_{i} and T_{j}. At each step, the two edges that would grow both trees T_{i} and T_{j} using Prim’s algorithm are proposed and the edge with minimal weight is added. This continues until T_{i} and T_{j} connect. The weight of the final edge added in this algorithm defines a new metric between the vertices v_{i} and v_{j}. This process is repeated for all pairs of vertices and this new metric is used as input to spectral clustering (Galluccio et al. 2013).
A primary advantage of this metric based on the hitting time of the two MSTs is that it depends on the MST topology of the data. Thus if two vertices belong to the same cluster, then the MST distance between them will be small since cluster points will be close together. This is the case even if the vertices are far away from each other (e.g. on opposite ends of the cluster). However, if the two vertices are in different clusters that are well separated, then the MST distance between them will be large. See Figure A.1 for an example. Thus this method of clustering is very robust to the shape of the clusters. Galluccio et al. (2013) contains many more examples.
Fig. A.1. Dual rooted Prim tree built on a 2dimensional data set when the roots are chosen from the same class (a) and different classes (b). The X’s mark the roots of the trees and the dashed line is the last connected edge. The length of the last connected edge is greater when the roots belong to clusters that are more separated. 
The MSTbased metric can be computationally intensive to compute as Prim’s algorithm must be run as many times as there are pairs of vertices. To counter this, Galluccio et al. (2013) proposed the EACDC algorithm which uses the information from only a subset of the dual rooted MSTs. This is done by calculating the dual rooted MSTs for a random pair of vertices. Three clusters are defined for each run: all vertices that are connected to one of the roots in the MSTs form two of the clusters (one for each root) while all points that are not connected to either of the MSTs are assigned to a third “rejection” cluster. A coassociation measure for two vertices is then defined as the number of times those vertices are contained in the same nonrejection cluster divided by the total number of runs (dual rooted MSTs). This coassociation measure forms a similarity measure to which spectral clustering is applied.
Cite this article as: Moon KR, Delouille V, Li JJ, De Visscher R, Watson F, et al. Image patch analysis of sunspots and active regions. II. Clustering via matrix factorization. J. Space Weather Space Clim., 6, A3, 2016, DOI: 10.1051/swsc/2015043.
All Tables
Mount Wilson classification rules, number of each AR, and total number of joint patches or pixels per Mount Wilson class used in this paper when using the STARA masks.
Summary of the advantages of SVD and NMF matrix factorization methods. The advantages of one method complement the disadvantages of the other (Langville et al. 2006). For example, the NMF optimization problem is nonconvex with local minima resulting in solutions that depend on the initialization of the algorithm.
Difference between dictionaries learned from the collection of sunspot patches corresponding to the different Mount Wilson types as measured by the Grassmannian metric d_{G}, e.g. d_{G} (A_{α}, A_{β}). Dictionaries are learned using random subsets of the data and the results are reported in the form of mean ± standard deviation using 100 trials. Different sizes of dictionaries r are used. The SVD results are sensitive to r.
Difference between the collection of dictionary coefficients pooled from the different Mount Wilson classes as measured by the Hellinger distance. Intraclass distances are reported in the form of mean ± standard deviation and are calculated by randomly splitting the data and then calculating the distance over 100 trials. The size of the dictionaries is r = 6 and 8 for SVD and NMF, respectively. The βγδ group is most dissimilar to the others.
Average pairwise difference between dictionary coefficients from each AR from different Mount Wilson types as measured by the Hellinger distance. Results are reported in the form of mean ± standard deviation. The size of the dictionaries is r = 6 and 8 for SVD and NMF, respectively. The βγ ARs are most dissimilar to each other and the other classes while the β ARs are most similar.
The labels used to compare with the clustering results when analyzing the effects of including the neutral line.
Mean similarity of ARs to other ARs either in the same cluster (1 vs. 1 or 2 vs. 2) or in the other cluster (1 vs. 2) under the different schemes. Cluster 1 contains ARs that are very dissimilar to each other while Cluster 2 contains ARs that are very similar to each other.
Mean and median number of pixels of the ARs in each cluster under the Hellinger clustering schemes. Cluster 1 contains the larger sunspots for all groups when using NMF and for some of the groups when using SVD.
Magnitude of the correlation coefficient of the clustering assignment with either R or log R when using all of the coefficients, only the coefficients corresponding to the magnetogram component (SVD elements 2–4 in Fig. 4), or only magnetogram gradient coefficients (SVD elements 3 and 4 in Fig. 4). For NMF, all of the dictionary elements are associated with the magnetogram and many of them have gradient components so we only perform clustering with all of the coefficients.
Summary of features distinguishing the clusters under the various classification schemes tested.
All Figures
Fig. 1. MDI continuum and magnetogram from NOAA 9097 on July 23, 2000 (top) and from NOAA 10045 on July 25, 2002 (bottom) overlaid with the corresponding STARA masks in green. 

In the text 
Fig. 2. (a) An example of a 3 × 3 pixel neighborhood or patch extracted from the edge of a sunspot in a continuum image and its column representation. (b) The number of patches extracted from each pair of AR images when using the STARA masks. 

In the text 
Fig. 3. An example of linear dimensionality reduction where the data matrix of AR image patches Z is factored as a product of a dictionary A of representative elements and the corresponding coefficients in the matrix H. The A matrix consists of the basic building blocks for the data matrix Z and H contains the corresponding coefficients. 

In the text 
Fig. 4. Learned dictionary elements using SVD. Dictionary elements are constrained to be orthonormal. The patches consist of uniform patches and gradients in varied directions. The magnetogram patches are essentially zero when the continuum components are nonzero and vice versa. The dictionary size r is first chosen based on the intrinsic dimension estimates in Moon et al. (2015) and then refined by comparing dictionaries of various sizes in Section 3. Section 4.2 contains more details on choosing r. 

In the text 
Fig. 5. Learned dictionary elements using NMF where the continuum dictionary elements are constrained to be nonnegative. All the dictionary patches consist of uniform patches or gradients in varied directions. The order of the elements is not significant. The dictionary size r is chosen to be approximately 1.5 times larger than the SVD dictionary size, which is chosen based on the intrinsic dimension estimates in Moon et al. (2015) and then refined using the results in Section 3. 

In the text 
Fig. 6. Scatter plot of MDS variables c_{1} vs. c_{2} (a, b) and c_{1} vs. c_{3} (c, d) where is the projection of the similarity matrix onto the ith eigenvector of the normalized Laplacian of the similarity matrix when using the NMF coefficients. Each point corresponds to one AR and they are labeled according to the clustering (a, c) and the Mount Wilson labels (b, d). In this space, the clusters data appear to be separable and there are concentrations of complex ARs in the region with lowest c_{1} values. Other patterns are described in the text. 

In the text 
Fig. 7. Mean similarity of an AR with all other ARs as a function of its MDS variable c_{1} using NMF. Cluster 2 is associated with those ARs that are most similar to all other ARs while Cluster 1 contains those that are least similar to all others. 

In the text 
Fig. 8. Histograms of the Mount Wilson classes divided by clustering assignment using the Hellinger distance. Cluster 1 contains more of the complex ARs while Cluster 2 contains more of the simple ARs. 

In the text 
Fig. 9. Histograms of the marginal distributions of the coefficients corresponding to the mean magnetic field value (dictionary element 2 in Fig. 3) for Cluster 1 (left) and Cluster 2 (right) using the SVD coefficients. Cluster 1 ARs contain more patches with near neutral magnetic field values. 

In the text 
Fig. 10. Plot of the adjusted Rand index (ARI) using and Hellinger distances within the neutral line and sunspots as a function of the weight. A weight of 0 corresponds to clustering with only the sunspots while a weight of 1 clusters with only the neutral line. The different lines correspond to different numbers of clusters and the corresponding labels from Table 6. Higher ARI indicates greater correspondence. 

In the text 
Fig. 11. Plot of the ARI using the Hellinger distance within the neutral line on only the coefficients corresponding to the SVD dictionary elements associated with magnetogram gradients. The corresponding dictionary elements are similar to the third and fourth elements in Figure 4. Focusing on the gradients results in a higher ARI for higher weights than when all coefficients are used as seen in Figure 10. 

In the text 
Fig. A.1. Dual rooted Prim tree built on a 2dimensional data set when the roots are chosen from the same class (a) and different classes (b). The X’s mark the roots of the trees and the dashed line is the last connected edge. The length of the last connected edge is greater when the roots belong to clusters that are more separated. 

In the text 
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