Issue 
J. Space Weather Space Clim.
Volume 10, 2020
Topical Issue  Space Weather research in the Digital Age and across the full data lifecycle



Article Number  36  
Number of page(s)  16  
DOI  https://doi.org/10.1051/swsc/2020037  
Published online  30 July 2020 
Research Article
Probabilistic prediction of geomagnetic storms and the K_{p} index
^{1}
Bradley Department of Electrical & Computer Engineering, Virginia Tech, Blacksburg, 24061 VA, USA
^{2}
Space Science and Applications (ISR1), Los Alamos National Laboratory, Los Alamos, 87545 NM, USA
^{*} Corresponding author: shibaji7@vt.edu
Received:
23
December
2019
Accepted:
4
July
2020
Geomagnetic activity is often described using summary indices to summarize the likelihood of space weather impacts, as well as when parameterizing space weather models. The geomagnetic index K _{ p } in particular, is widely used for these purposes. Current stateoftheart forecast models provide deterministic K _{ p } predictions using a variety of methods – including empiricallyderived functions, physicsbased models, and neural networks – but do not provide uncertainty estimates associated with the forecast. This paper provides a sample methodology to generate a 3hourahead K _{ p } prediction with uncertainty bounds and from this provide a probabilistic geomagnetic storm forecast. Specifically, we have used a twolayered architecture to separately predict storm (K _{ p } ≥ 5^{−}) and nonstorm cases. As solar winddriven models are limited in their ability to predict the onset of transientdriven activity we also introduce a model variant using solar Xray flux to assess whether simple models including proxies for solar activity can improve the predictions of geomagnetic storm activity with lead times longer than the L1toEarth propagation time. By comparing the performance of these models we show that including operationallyavailable information about solar irradiance enhances the ability of predictive models to capture the onset of geomagnetic storms and that this can be achieved while also enabling probabilistic forecasts.
Key words: geomagnetic storms / K _{ p } forecasting / deep learning / LSTM / Gaussian process
© S. Chakraborty & S.K. Morley, Published by EDP Sciences 2020
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://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
Modern electrical systems and equipment on the Earth such as navigation, communication, satellite and power grid systems can be affected by space weather (e.g., Choi et al., 2011; Qiu et al., 2015; Morley, 2019). The societal impact of space weather is increasing (Schrijver et al., 2015; Eastwood et al., 2017) and operational centers provide a range of predictions for endusers (Bingham et al., 2019), including geomagnetic storm predictions based on the K _{ p } index (Sharpe & Murray, 2017).
K _{ p } is a planetary 3h averaged range index that describes the intensity of the magnetic disturbance (Bartels, 1949). K _{ p } starts from 0 (very quiet) to 9 (very disturbed) with 28 discrete values described by 0, 0^{+}, 1^{−}, 1, 1^{+}, …, 9−, 9 (Bartels, 1949). The National Oceanic and Atmospheric Administration (NOAA) Space Weather Prediction Center (SWPC) classifies geomagnetic activity in six levels, shown in Table 1, based on the ranges of K _{ p }. In addition to being a forecast product in its own right, the K _{ p } index is widely used as an input to other magnetospheric models (e.g., Carbary, 2005) including some aimed at operational use (Obrien, 2009; Horne et al., 2013).
Table showing different categories of geomagnetic storm and associated K _{ p } levels. The categorization is done based on the intensity of the geomagnetic storm following the NOAA SWPC scales.
There are three main categories of models for K _{ p } prediction: coupled physicsbased models such as the Space Weather Modeling Framework (e.g., Tóth et al., 2005; Haiducek et al., 2017); “traditional” empirical models (Newell et al., 2007; Luo et al., 2017); and machinelearning models (Costello, 1998; Boberg et al., 2000; Wing et al., 2005; Wintoft et al., 2017; Tan et al., 2018; Sexton et al., 2019).
Longer leadtime predictions are typically the domain of empirical (e.g., Luo et al., 2017) and machinelearning models (e.g., Sexton et al., 2019). Since the first neural networkbased K _{ p } forecasting model proposed by Costello (Costello, 1998), many subsequent forecast models (Boberg et al., 2000; Wing et al., 2005; Tan et al., 2018) implement different variants of the neural network to improve the forecast accuracy. To date, none of these predictions have provided a probabilistic prediction, and very few attempted to characterize the uncertainty associated with the predicted K _{ p } value (see, e.g., Wintoft et al., 2017). With the development of new machinelearning techniques, recent K _{ p } and storm forecast models come with much higher accuracy, but few have separately examined the model performance under different ranges of geomagnetic storm conditions (see, e.g., Zhelavskaya et al., 2019). Recent work on K _{ p } prediction by (Shprits et al., 2019) highlighted the inherent limitation of solar winddriven models for long leadtime predictions, and noted that “further improvements in long term modeling should include … empirical modeling driven by observations of the Sun”.
To assess the viability of moving beyond solar winddriven models using operationallyavailable data, we also investigate the inclusion of solar Xray flux data as a model parameter. Solar Xray flux was chosen as recent studies have shown that these data can be used to forecast solar flare activity (Winter & Balasubramaniam, 2015) as well as solar energetic particle (SEP) events (Núñez, 2018). While the majority of large geomagnetic storms are caused by CMEs (e.g., Gonzalez et al., 1999), it has been shown that CMEs are correlated with solar flare activity (Kay et al., 2003; Zhou et al., 2003; Lippiello et al., 2008; Wu et al., 2008). Further, solar Xray flux is operationally available from the NOAA GOES satellites (see https://www.swpc.noaa.gov/products/goesxrayflux). We, therefore, include GOES Xray data in a variant of our predictive model to determine whether its use, as a proxy of solar magnetic activity, allows us to better capture the (often CMEdriven) geomagnetic storms.
The primary aim of this paper is to generate a K _{ p } prediction with associated uncertainty bounds and exploit it to provide a probabilistic geomagnetic storm forecast. The secondary objective is to test whether a simple, operationallyavailable solar irradiance data set can be included in this framework to better capture the effects of solar transients. We use a machinelearning method to forecast K _{ p }, including the associated uncertainty, then exploit the uncertainty bounds in K _{ p } to provide a probabilistic forecast. The paper is organized as follows: Section 2 explains the data analysis and the model development; Section 3 describes the results, shows how we develop a probabilistic storm forecast and assesses the model performance; and finally we discuss the results in the context of similar work.
2 Data analysis & model architecture
Here we describe the data sets and the model architecture used in this study. Specifically, we present the basic characteristics of the data sets and a brief justification of our choices of model features. In addition, we provide a short introduction to the technical terms and metrics used to evaluate the model performance. Finally, we describe the construction of our predictive models and note some strengths and weaknesses of our approach.
2.1 Model features and data sources
The solar wind energy and magnetospheric coupling are known to be welldescribed by the solar wind parameters and the state of the magnetosphere (Dungey, 1961; Baker et al., 1981). However, many of the solar wind parameters are correlated with each other and might carry redundant solar wind structure information (e.g., Hundhausen, 1970; Wing et al., 2016). There is a long history of using plasma moments (number density and velocity) and the interplanetary magnetic field to describe the coupling of energy from the solar wind into the magnetosphere (e.g., Baker et al., 1981; Borovsky et al., 1998; Xu & Borovsky, 2015). More recentlydeveloped coupling functions using solar wind parameters have been shown to have better correlations with geomagnetic indices (e.g., Newell et al., 2007) and clear physical origins (e.g., Borovsky, 2013). It is also clear that including a measure of the present state of the magnetosphere helps predict the evolution of global indices like K _{ p } (Borovsky, 2014; Luo et al., 2017).
Based, in part, on these considerations we use just nine solar wind parameters and the historical K _{ p } as model features (input parameters). The input parameters are chosen based on the studies done by the previous studies (Newell et al., 2007; Xu & Borovsky, 2015). These model features are listed in Table 2 along with the notation we use in this paper and any transformations applied prior to model training. For the solar wind data, we use 20 years of 1min resolution values, starting from 1995, obtained from NASA’s OMNIWeb service (https://omniweb.gsfc.nasa.gov/ow_min.html). The 3hourly K _{ p } index is obtained from the GFZ German Research Centre for Geosciences at Potsdam (https://www.gfzpotsdam.de/en/kpindex/).
Table showing input features of the model, transformations used (if any), and which models use each feature. The given transformation is only used prior to fitting the Gaussian process model. BoxCox → B(x) = sgn(x) × log_{e} x and Erf → erf(x) = .
As solar wind structures are spatial in nature, the measured parameters are autocorrelated. Solar wind data from L1 monitors are point measurements and hence spatial structure along the Sun–Earth line manifests as a temporal correlation. Hence, we performed an autocorrelation analysis of all the solar wind parameters as presented in Figure 1. From the figure, we can conclude that, during solar minimum, most of the solar wind parameters are highly autocorrelated for a longer duration, while during solar maximum, the correlation coefficient drops within a few hours. This suggests more transients in solar wind during solar maximum than the solar minimum, consistent with observations (Richardson & Cane, 2012). All parameters selected as model features display autocorrelation, and most parameters decorrelate within 3 h, with solar wind speed being a notable exception. Indeed, at solar maximum, all parameters except solar wind speed decorrelate in less than 3 h. At solar minimum, the autocorrelation for the majority of parameters falls below 0.5 within 3 h. We, therefore, used 3hourly averaged solar wind data to train our models, which has the added benefit of placing the input data on the same cadence as the predicted output. Note that the goal of this linear analysis (autocorrelation) is to describe the redundant information given in subsequent samples of individual solar wind parameters, rather than identifying time lags in the magnetospheric response to solar wind driving. In addition, we acknowledge that including nonlinear correlations may provide more robust estimates of the correlation scales, and could exhibit different behaviors (e.g., Wing et al., 2016; Johnson et al., 2018).
Fig. 1
Autocorrelation functions of different solarwind parameters during: (a) solar minima, and (b) solar maxima. 
As the K _{ p } index is quasilogarithmic and essentially categorical (Mayaud, 1980), we converted the reported K _{ p } values to decimal numbers using following Tan et al. (2018).
In this study, we will also test the effectiveness of including a previouslyunused set of solar data for K _{ p } prediction. That is, we will introduce our modeling approach using a standard construction with only upstream solar wind measurements to drive the model. We will then train a second model that differs only in the inclusion of Xray flux in the model features.
As described above, the idea behind using the solar Xray data is that the upstream solar wind carries little to no information about transients that are moving towards Earth. Advanced notice of transients from insitu L1 measurements is therefore limited to periods typically less than 1 h. By including solar data, even a coarse measure such as the Xray flux, we aim to demonstrate that additional information about the likelihood of transients can be included in the model and improve forecasts with a lead time longer than the L1toEarth propagation time. In other words, we treat the Xray flux data as a proxy for the magnetic complexity of the Sun and anticipate that including this data will allow the model to predict the arrival of CMEs earlier than a modeldriven purely by solar wind measurements. We obtain the GOES Xray flux data from NOAA’s National Centers for Environmental Information (https://satdat.ngdc.noaa.gov/sem/goes/data/).
The GOES Xray sensors have two channels that measure solar irradiance in two wavebands, namely, hard (0.05–0.4 nm) and soft (0.1–0.8 nm) Xrays. In this study, we followed Winter & Balasubramaniam (2015) in using a background term and a flux ratio derived from the two GOES wavebands. The Xray background (B) has been computed as the smoothed minimum flux in a 24h window preceding each 1min GOES soft Xray flux observation. In a recent study, the Xray background parameter was found to describe the solar activity cycle better than the daily F10.7 parameter (Winter & Balasubramaniam, 2014). The Xray flux ratio (R) has been calculated by taking the ratio of hard Xray flux over soft Xray flux, and provides a measure of the temperature of the flare emission (Garcia, 1994). Kay et al. (2003) showed that flares associated with CMEs tended to have lower temperatures, at a given intensity level, than flares without CMEs. Thus both the soft Xray flux and the flux ratio, R, are important for determining the likelihood of an eruptive event. Further, Michalek (2009) showed a good correlation between the energy of the CME and the peak of the Xray flare. Finally, recent studies showed that the Xray flux ratio is a good predictor for extreme solar events (Kahler & Ling, 2018; Núñez, 2018).
As Xrays propagate from the Sun to the Earth at the speed of light, there will, of course, be a time lag associated with the arrival at Earth of any related geomagnetic activity due to associated coronal mass ejections. In this preliminary work to demonstrate the utility of including solar Xray flux data in a K _{ p } prediction model, we assume a constant time lag that we apply to the derived Xray products B and R. Figure 2 presents a timelagged crosscorrelation analysis of B and R with other solar wind parameters to highlight any time lags between these two data sets. The correlation analysis shows that the Xray background (B) parameter is significantly correlated with many solar wind parameters at lags around 48 h. The correlations between the Xray flux ratio (R) and the solar wind parameters are smaller and less consistent across solar wind parameters. A lack of clear, or strong, linear correlations with solar wind parameters at a given fixed lag does not necessarily indicate that the parameter R is confounding. Better lag estimates could be obtained using nonlinear analysis (e.g., Wing et al., 2016; Johnson et al., 2018), however, models used in this study can extract nonlinear relationships. We therefore expect nonlinear relationships in the dataset to be captured by the proposed models.
Fig. 2
Crosscorrelation functions of different solarwind parameters with (a) GOES flux background (B) and (b) ratio (R) of hard (0.05–0.4 nm) and soft (0.1–0.8 nm) Xray flux data. 
Transit times of coronal mass ejections can range from less than 20 h to more than 80 h (e.g., Schwenn et al., 2005), however faster CMEs tend to be more geoeffective (Gonzalez et al., 1999; Srivastava & Venkatakrishnan, 2002). Hence weWe, therefore, apply a constant time lag of 48 h to the Xray flux derived parameters, consistent with a typical travel time from the Sun to Earth of geomagneticstorm associated interplanetary CMEs (Srivastava & Venkatakrishnan, 2004). Although we note that in future work it may be useful to explore the effects of choosing this lag over a different fixed lag, or even use of a variable lag.
2.2 Technical definitions & metrics for model evaluation
In this subsection, we define the technical terms and the metrics that we use in the latter part of this study to evaluate and compare the models’ performance. Good overviews of model performance metrics and model validation methodologies targeted at space weather have been given by Morley et al. (2018a), Liemohn et al. (2018), and Camporeale (2019).
For binary event analysis, we define correct “yes” events as True Positives (denoted as a). Similarly, we call incorrect “yes” events False Positives (b), incorrect “no” events are False Negatives (c), and correct “no” events are True Negatives (d).
Note that a perfect forecast will have HSS, MCC, PoD, Bias, CSI, R ^{2} equal to 1 and FAR equal to 0. Unskilled or random forecasts will have HSS, MCC, PoD, CSI, R ^{2} of 0, FAR of 1.
For assessing numerical predictions of the K _{ p } index we use:
where, x _{ i }, and n are observations, predicted output and a total number of observations, respectively. A perfect model will have zero RMSE and MAE, while a coefficient of determination of 1.
2.3 Model development
Figure 3 presents the distribution of 22 years of K _{ p } values, where the logscaled frequency of occurrence is shown on the vertical axis and the K _{ p } value is shown on the horizontal axis. From the figure, it is evident that most of the events are distributed between [0, 5^{−}), a relatively small number of events are distributed between [5^{−}, 7^{−}), and there are very few extreme events ≥7. Following the NOAA Gscale for geomagnetic storms, we choose K _{ p } ≥ 5^{−} as the threshold for “stormtime”, marked with a vertical line in Figure 3. Using this division, stormtime comprises approximately onetwentieth of the data set. This number continues to drop rapidly as K _{ p } increases. If we take the ratio of more extreme events (K _{ p } ≥ 8^{+}) versus nonstorm events, the number drops to . This effect is known as data imbalance (e.g., Estabrooks et al., 2004) and can lead to significant errors in a model fit to the data without accounting for the imbalance (see, e.g., Shprits et al., 2019).
Fig. 3
Distribution of K _{ p }. 20 years 1995–2014 of data has been used in this plot. f(K _{ p }) is the frequency (i.e., the number of events) plotted on a logarithmic scale. The black vertical line is K _{ p } = 5^{−}. 
Both oversampling and undersampling techniques have been used to address data imbalance (Estabrooks et al., 2004; Shprits et al., 2019), and both methods help develop models with a better predictive skill (Yap et al., 2014). Choosing a single regression model to predict K _{ p } across quiet and disturbed geomagnetic conditions will likely not provide an optimal forecast unless the data imbalance is addressed. Here we take a similar approach to Tan et al. (2018), Boberg et al. (2000) and minimize the data imbalance by separating the problem into two different categories: stormtime and nonstorm. This then leads to the first step in our model architecture, where we use a classifier to determine quiet or active conditions, and subsequently use a probabilistic regressor to predict the K _{ p } value.
In this study, we have used a deterministic longshort term memory (LSTM) neural network (Hochreiter & Schmidhuber, 1997). An LSTM is a type of recurrent neural network, where a “memory cell” is used to store information between time steps (see Tan et al., 2018, and references therein). LSTM neural networks are a special type of recurrent neural network, wellsuited to time series data analysis, and they require continuous data for training. However, we encounter missing IMF and solar wind data values issue. To handle the missing data issue we use the interpolation method described in Tan et al. (see Sect. 2.1 of 2018, and references therein). The method used by Tan et al. (2018) is appropriate for relatively small (up to 12 samples) data gaps, for larger data gaps we discarded the samples. As with other types of neural networks, an LSTM can be used as either a regressor or a classifier. The layout of our LSTM classifier is shown schematically in Figure 4. Panel 4a presents a schematic of a single LSTM unit. The LSTM unit consists of input, output, forget gates, and memory cell (C _{ t }) (see Hochreiter & Schmidhuber, 1997, and references therein). Panel 4b illustrates the overall architecture of the classifier, where the central layer is comprised of LSTM units. Panel 4c shows the implementation as layers in the Keras model. The “N” in the input/output shape of the model blocks shows the number of time samples, which can be varied at runtime. However, as described later in this section we use a 27day window at 3hourly cadence, therefore N = 216.
Fig. 4
Schematics showing architectures (a) of a single LSTM block, (b) of the classifier consisting of one input layer, one LSTM layer consists of 100 nodes (neurons), dropout, and output layer, and (c) of the classifier model implemented using Keras. 
As described in the previous paragraph LSTM classifier comprises an input layer with 10 neurons, a hidden layer with 100 neurons, and an output layer of 2 neurons. The MSE on the validation data reduced as the number of neurons in our hidden layer increased, but adding more than ~100 LSTM units led to smaller improvements. We therefore chose to retain only 100 LSTM units in our hidden layer. To help reduce overfitting and increase the generalizability of the model we included dropout regularization. The input shape of the data is therefore (N × 10 × 3), where N = 216, 10 and 3 are the number of data points, the number of input parameters (see Table 2), and the timelagged units (the input vector at times t, t − 1, and t − 2), respectively. Hence, the input shape for one data point is 10 × 3. Note, the input shape for one data point can also be 12 × 3, based on the choice of model (μ ^{OMNI} or , see the following paragraphs for details). To ensure that the classifier performance can be generalized beyond the training data, we split available data into two categories: training/validation and testing. For training and validation we used the intervals 1995–2000 and 2011–2014. To mitigate the effects of data imbalance we used a random downsampling strategy to balance the stormtime and nostorm intervals. After downsampling (from 29,200 to 5716 points), we split the data into “training” and “validation” sets and train the classifier, where the validation data is used for tuning the model parameters and comprises 20% of the training set. Data from 2001–2010 was reserved for outofsample testing of the predictions (26,645 points). The rationale behind using the above mentioned periods for train/validation and test the model is to increase the model performance throughput and reduce the model bias. Both train and test periods consist of different solar maximum and minimum data to capture solar cycle dynamics and testing with outofsample data ensures that the model generalizes well to unseen data.
Following Tan et al. (2018) we employ a twolayer architecture, where we use separate regression models to predict K _{ p } under quiet or active geomagnetic conditions. Unlike Tan et al. (2018) we use probabilistic regressors. The model structure is shown in Figure 5. The prediction made by the classifier is used to determine which regressor is going to be selected. As the primary aim of this work is to produce a probabilistic prediction of K _{ p }, we chose regression models that output a distribution rather than a single value. We used semiparametric Deep Gaussian Process Regression, commonly known as deepGPR, to build the regressors. DeepGPR (dGPR) is a Gaussian Process model with neural network architecture. A Gaussian Process is a random process that follows a multivariate normal distribution. Specifically, dGPR (AlShedivat et al., 2017) is a Gaussian Process Regression (Rasmussen & Williams, 2006) method, which uses a deep LSTM network to optimize the hyperparameters of the Gaussian Process kernels.
Fig. 5
Proposed model (μ) architecture: Classifier is deterministic in nature, and regressors are probabilistic in nature. The threshold for the classifier is K _{ p } = 5^{−}. Here, w _{ q } & w _{ s } are the variable training windows for two regressors. For details refer text. 
For example, if the classifier predicts a geomagnetic storm then regressor dGPR_{ s } is selected, otherwise regressor dGPR_{ q } is used. At each time step, the dGPR is retrained using the interval of preceding data (the training window), and thus our regressors are dynamic nonlinear models. Dynamic models do not need to assume a constant functional relationship between the model covariates (e.g., solar wind drivers) and response (K _{ p }). Static models implicitly combine the effects of any potentially timeâ€varying relationships in the error terms or average over the effects in the estimation of model coefficients (see, e.g., Osthus et al., 2014). By using a relatively short, local training window, the data is used more efficiently and computational complexity is reduced. For training and validation of the dGPRbased dynamic model, including training window selection, we used the mean squared error (MSE) as our loss function.
Optimizing the hyperparameters of a dGPR is much easier while working with input parameters that are normallydistributed. To ensure better behavior of the Gaussian process model we transformed all the substantially nonnormally distributed input parameters listed in Table 2 using either a BoxCox transform or the Complementary Error Function. After the transformation, we check the skewness and kurtosis of the transformed variable to validate the transformation. We found BoxCox transformation worked well for all IMF and solar wind parameters except plasma beta. We transform the plasma beta using the Complimentary Error Function.
The quiettime and stormtime regressors each use different training windows, the lengths of which were selected to minimize the training error using the mean squared error (MSE) in K _{ p } as the loss function. Figure 6 shows one example of how the MSE varies with the training window (in days) for predictions over two months during 1995. It can be clearly seen that a training window of ≈27 days is optimal at this time, as this captures recurrent structure in the solar wind such as corotating interaction regions (Richardson & Cane, 2012). While the deep architecture helps to capture the nonlinear trends in data to provide better accuracy, the Gaussian process mappings are used to provide the error distribution with a mean predicted K _{ p }. The two dGPR regressors are different in terms of the length of the training window used for forecasting. The dGPR module dedicated for nonstorm, or quiet, conditions has a 27day training window, whereas the dGPR module for storm conditions uses a 14day training window.
Fig. 6
Variation of root mean square error (RMSE, ε) in with the length of the training window (τ) in days. Each point of this curve is generated using the average RMSE of two months of data. 
One of the difficulties in predicting the “events” – i.e., the stormtime K _{ p } values – is that these are typically driven by solar wind transients, which include interplanetary CMEs and corotating interaction regions (CIRs) (see, e.g., Kilpua et al., 2009; Zhang et al., 2018), with the largest storms driven by CMEs (Borovsky & Denton, 2006). The insitu solar wind measurements from an L1 monitor do not convey the information required to predict the occurrence of these transients for a 3hourahead prediction of K _{ p }, or for longer prediction horizons. For this reason, we perform a preliminary investigation in which we include information that may encode the likelihood of CME eruption. Following Winter & Balasubramaniam (2014) we use Xray flux data from the NOAA GOES platforms as a measure of possible solar activity.
To test whether the inclusion of a proxy for solar activity improves our ability to predict stormtime K _{ p }, we constructed two different prediction systems. The first was trained only on OMNI solar wind parameters (μ ^{OMNI}). The second added the Xray background (B) and the flux ratio (R) as extra model parameters (). When using the Xray data we add B and R as model features to the LSTM classifier as well as the stormtime regressor. Note that we do not use the Xray data for the quiettime regressor. Both the models are validated and evaluated against 10 years of K _{ p } (2001–2010), in addition to a specific stormtime validation using 38 intervals listed in Table 3.
List of storm events.
3 Results
In this section, we present model forecasts and quantitative comparison of predicted K _{ p }, comparing the models with and without the GOES Xray data. We further describe a simple method to exploit the uncertainty bounds of the predicted K _{ p } to provide a probabilistic geomagnetic storm prediction. Finally, we analyze the performance of the probabilistic K _{ p } prediction models.
3.1 K _{ p } forecast models
As the first step, we present 3h ahead predicted K _{ p } during two months of 2004. Panels (a) and (b) of Figure 7 shows predicted K _{ p } with a 95% confidence interval using models μ ^{OMNI} and , respectively. The horizontal dashed black line shows the storm versus nonstorm demarcation line. The root mean square error (ε) and mean absolute error () for this 2 month interval are given each panel as annotations. In the figure, we have discretized the K _{ p } values and the 95% confidence interval bounds by rounding them to the nearest valid K _{ p } values (see Sect. 4.2 of Morley et al., 2018b). We have chosen this time interval as an example to showcase the ability of the model to capture the dynamics of both stormtime and quiettime K _{ p }. Examining Figure 7, it is visually apparent that both the models can capture the change in K _{ p } during the transitions into, and out of, stormtime. The error metrics given in each panel suggest that models μ ^{OMNI} and are comparable in their performance. However, a more detailed analysis is required to allow us to draw firm conclusions and assess the impact of including the Xray flux data. Specifically, as the intent of including the Xray flux is to better capture stormtime transients, we need validation methods that allow us to determine the performance as a function of activity level.
Fig. 7
Threehour forecast of K _{ p } using LSTM classifier & Deep Gaussian Process Regression (Deep GPR) for a solar maximum period (1st July–31st August, 2004). Panels: (a) prediction from the model using OMNI solar wind data and (b) prediction from the model using OMNI solar wind data and GOES solar flux data. Blue and black dots in panels (a) and (b) are mean predictions and red dots show observed K _{ p }, respectively. Light blue and black shaded regions in panels (a) and (b) respectively show 95% confidence interval. RMSE (ε) and MAE () are mentioned inside each panel. 
We have conducted a thorough headtohead test of two K _{ p } forecast models, μ ^{OMNI} and , using predictions across our validation data set (from January 2001 through December 2010). We also compare the model predictions for 38 stormtime intervals (listed in Table 3). Summary statistics for the different models are presented in Table 4. When comparing the models across the full validation set, the error metrics are nearly identical between the model variants. The RMSE, MAE and correlation coefficient for both of our models show similar performance to the models of Boberg et al. (2000) and Bala & Reiff (2012). On the full data set our model does not perform as well as that of Tan et al. (2018). However, in addition to generating a probabilistic forecast, we seek to answer the question of whether including GOES Xray data provide a meaningful improvement in the prediction of stormtime K _{ p } intervals. Looking at the same metrics for the 38 stormtime intervals, a different picture emerges. The model variant incorporating Xray flux data () outperforms the standard model by a substantial margin. The RMSE of is 0.9 and the MAE is 0.67, showing that typical stormtime K _{ p } predictions are within 1 K _{ p } interval of observation. Of particular importance is that the correlation coefficient increases for relative to the performance across the full validation set. Here we note that the correlation coefficient can be considered a measure of potential performance, as it neglects conditional and unconditional bias (Murphy, 1995).
To graphically display the model bias across these two validation sets, Figure 8 plots observed K _{ p } against predicted K _{ p }. Panel (a) shows the comparison across the full 10year validation set and panel (b) shows the comparison for the 38 storm intervals. Black and blue colors represent predicted K _{ p } using μ ^{OMNI} and , respectively. The circles give the mean predicted K _{ p } and the vertical lines represent 1σ error bars associated with that predicted K _{ p } level. As above, the predictions from both models are comparable when we use the full validation set (Fig. 8a) and do not account for the activity level. For K _{ p } ≤ 3^{+} the predictions show little to no bias; the mean predicted K _{ p } is nearly identical to the observed value during quiet times. At higher levels of geomagnetic activity, we see a clear tendency for the mean predicted K _{ p } to be lower than the observation. That is, high values of K _{ p } tend to be underpredicted by both models. Comparing the two models shows a slight improvement in the bias at higher K _{ p } values using the model, but the most visible improvement using this display format is in the smaller error bars on the predictions.
Fig. 8
The performance comparison of μ ^{OMNI} and models which predict K _{ p } 3h ahead. Panels present performance of μ ^{OMNI} (in black) and (in blue) models for (a) 10 years of prediction and (b) 38 stormtime prediction (listed in the Table 3). In each panel official (Postdam) K _{ p } is plotted on the xaxis and the model prediction is plotted on the yaxis. Perfect predictions would lie on the line with a slope of one. The error bar indicates one standard deviation and the correlation coefficient and coefficient of determination are mentioned inside each panel. 
Table 4 presents a summary of overall fit statistics, both both model, for the 2001–2010 data set as well as the stormtime data set. On both data sets there is an improvement in the fit when adding the Xray flux data to the model. Because the correlations have the observations in common, we test whether the improvement is significant using a test for correlated correlation coefficients (Steiger, 1980; Revelle, 2020), where we use the effective number of samples (n _{eff} where n _{eff} < n) estimated by correcting for the lag1 autocorrelation (see, e.g., Wilks, 2006). The improvements in r for both models are statistically significant, with a pvalue of 4.8 × 10^{−5} for the 2001–2010 data set and p < 10^{−5} for the stormtime data set. Given the results presented in both Table 4 and Figure 8, we conclude that including Xray flux information provides information that improves K _{ p } prediction accuracy during geomagnetically active intervals.
However, this analysis only uses the mean prediction and neglects the fact that we have used a probabilistic regressor. So, how can we use the uncertainties provided by the dGPR prediction and how well do our probabilistic predictions perform?
3.2 Probabilistic storm forecast
Here we describe how we exploit the uncertainty in predicted K _{ p } to provide a probabilistic geomagnetic storm forecast using the SWdriven model μ ^{OMNI} as an example. Figure 9 illustrates the probabilistic prediction of both the K _{ p } index and of geomagnetic storm occurrence. Figure 9a shows a “traffic light” display which gives the probability of K _{ p } exceeding 5^{−}, which we use to delineate stormtime, following the NOAA Gscale of geomagnetic storms (refer Table 1).The color represents the likelihood of storm activity: green is Pr ≤ 0.3, yellow is 0.33 < Pr ≤ 0.66, and red marks intervals where the probability of geomagnetic storm conditions exceeds 0.66. Note that, Pr is the probability of geomagnetic storm, using the NOAA SWPC definition of K _{ p } ≥ 5^{−} as the threshold for geomagnetic storm.
Fig. 9
Threehour forecast (using model) showing (a) probability of geomagnetic storms, (b) K _{ p } (22nd July–31st July, 2004) and (c) an illustration of the method to extract probability of storm occurrence for one prediction marked by vertical black line in panel (b). Black dashed lines in panels (b) and (c) represent the threshold K _{ p } = 5^{−}, red and blue thin lines in panel (c) are observed K _{ p }, and predicted mean respectively. Panel (b) is in the same format with Figure 7. The shaded region in panel (c) provides probability of geomagnetic storm (Pr[e] = 0.81, for details refer text). 
Figure 9b presents 10 days (21st–31st July 2004) of 3h ahead predictions of K _{ p }, using model (cf. Fig. 7b). The horizontal dashed line is at K _{ p } = 5^{−} and the vertical bar marks the time of the prediction shown in Figure 9c. Figure 9c illustrates how to calculate the probability of geomagnetic storm from the predicted distribution of K _{ p }. The blue curve gives the output Gaussian probability density function from the dGPR regressor while the blue and red vertical lines represent the mean prediction and the observed K _{ p }. The vertical dashed black line marks K _{ p } = 5^{−} and the integral of the shaded area is the probability of exceeding the threshold.
In a nonprobabilistic model, we would simply have a binary outcome of storm or nonstorm. Following this method, we see that the prediction of a probability distribution gives us both uncertainty bounds on our prediction of the actual K _{ p } as well as the probability of exceeding a given threshold in K _{ p }.
To assess the probabilistic storm prediction (i.e., the probability of exceeding a threshold), we will examine binary event forecasts. For this we convert each probabilistic prediction into a prediction of “event” or “no event”. For this, we need to choose a probability threshold. As our predicted probability distribution is Gaussian, the mean prediction is also the 50th percentile. Simply ignoring the predicted distribution and using the mean value is equivalent to using a threshold of 0.5. We can similarly convert the observed K _{ p } to a series of events and nonevents, and can subsequently determine whether the prediction was a true positive, false positive, false negative or true negative (see Sect. 2.2).
Figure 10 shows K _{ p } predictions using the μ ^{OMNI} model during a geomagnetic storm at the end of March 2001. One forecast from each of the true positive (TP), false positive (FP), false negative (FN) and (true negative) TN categories are shown by the vertical lines. Figure 10 is in a similar format to Figure 9, except that panel (c) is omitted. We use the simpler model for this graphic to illustrate the main effect that our model aims to combat. Specifically, the FP and FN cases are occurring in a specific pattern. At the start of the storm, we see a false negative and at the end of the storm, we see a false positive. This is typical for solar winddriven models for predictions that are further ahead than the lead time given by the solar wind. In this case, we have a 3h lead time to our prediction and so the model has no information to capture the sudden onset of the geomagnetic activity. By the next prediction, the model has “caught up” and now correctly predicts a very high likelihood of stormtime. The inverse is seen, though perhaps less clearly, at the trailing edge of the storm. The model is unable to predict the cessation of stormlevel geomagnetic activity, although we do note that the uncertainty bounds include a nonnegligible likelihood of K _{ p } < 5^{−}.
Fig. 10
Example model predictions using μ ^{OMNI} model showing true positive (TP), false positive (FP), false negative (FN), and true negative (TN) predictions, mentioned by vertical lines. Top and bottom panels show the probability of geomagnetic storms and K _{ p } with uncertainty bounds (shaded) region. 
The model prediction is, therefore, lagging the observation. While this figure shows one example where predicted K _{ p } is lagging the observations by 3 h, most of the stormtime predictions are lagging the observations by at least one 3h prediction window. This implies that the model μ ^{OMNI} has insufficient information to capture the imminent arrival of a solar wind transient from the L1 data alone, and the prediction is likely to be strongly persistent (giving high weight to the previous value of K _{ p }) in the model. By including the Xray data in the model as a proxy for the likelihood of CME occurrence, we aim to improve stormtime predictions and hopefully combat this “lag” effect.
3.3 Comparison of probabilistic predictions
In the previous sections, we described a method to use the uncertainty bound to a predict probabilistic storm forecast. Here we are going to compare the predictions using models (μ ^{OMNI} and ), using the different metrics defined in Section 2. We begin with the receiver operating characteristic (ROC) curve. The ROC curve is calculated from the probability of detection (PoD) and the probability of false detection (PoFD) over a range of decision thresholds. If we make a decision threshold of Pr = 0, then all predictions lie above it and thus every time is predicted as an event and the PoD and PoFD are both 1. Conversely, taking a decision threshold of Pr = 1 leads to no events being predicted, thus PoD and PoFD are both zero.
Figure 11 presents the ROC curves calculated for both the μ ^{OMNI} and models, using different K _{ p } threshold values. The solid lines are the ROC curves from model μ ^{OMNI} and the dashed lines are the ROC curves from model . Thresholds of K _{ p } = 2, 4 and 6 are shown in red, black and blue, respectively. We also use the area under the ROC curve (abbreviated as AUC) as a summary measure to compare the performance of our models (cf. Bradley, 1997), and the AUC for each ROC curve is given in the figure legend. For the lower K _{ p } threshold values are shown (K _{ p } = 2 or 4) the curves are similar and the AUC are correspondingly similar. For the higher K _{ p } threshold value (K _{ p } = 6) the ROC curves visibly diverge across a broad range of decision thresholds. The AUC for is higher than that for μ ^{OMNI}. This provides qualitative support for the hypothesis that the inclusion of GOES Xray data has improved the performance of our K _{ p } model for high geomagnetic activity.
Fig. 11
Receiver operating characteristic (ROC) curves showing the relative performance of individual the storm forecasting model μ ^{OMNI} (represented by solid curves) and (represented by dashed curves) with different storm intensity levels (for K _{ p } ≥ 2, 4, and 6). 
As the aim of including the Xray flux data was to potentially provide information relevant to predicting the intervals of higher K _{ p } with a longer lead time, we also test the difference between the AUC for and μ ^{OMNI}, when K _{ p } ≥ 6. Because the same test data is used for both ROC curves – the two blue curves in Figure 11 – we use DeLong’s nonparametric test for the area under correlated ROC curves (DeLong et al., 1988; Sun & Xu, 2014) as implemented in the pROC package (Robin et al., 2011). A twosided test yielded (Z = −8.27; p < 2.2 × 10^{−16}) showing that the visual difference between the ROC curves for the two models is statistically significant. This confirms the qualitative analysis presented above and supports the hypothesis that including even simple proxies for solar activity can improve the prediction of geomagnetic activity with lead times greater than the L1toEarth transit time.
Figure 12 also explores activitydependent model performance. Using Pr = 0.5 as our decision threshold again, we calculate a range of performance metrics (described in Sect. 2.2) while varying the K _{ p } threshold used to define an “event” (see also Liemohn et al., 2018). In each of the panels, the black markers show the results for μ ^{OMNI} and the blue markers show the results for . The error bars show the 95% confidence interval estimated using 2000 bootstrap resamplings (Morley, 2018; Morley et al., 2018b). Panel (a) shows the thresholddependent Heidke skill score (HSS), which measures model accuracy relative to an unskilled reference. Panel (b) shows the Matthews Correlation Coefficient, which can be interpreted in a similar way to a Pearson correlation. Panel (c) shows the probability of detection (PoD), also called hit rate or true positive rate. Panel (d) shows the false alarm ratio (FAR), which is the fraction of predicted events that did not occur. The ideal FAR is therefore zero. Panel (e) shows the critical success index (CSI), which can be interpreted as an accuracy measure after removing true negatives from consideration. Finally, panel (f) displays the frequency bias, where an unbiased forecast predicts the correct number of events and nonevents and scores 1. As a reminder, the metrics displayed in panels a, b, c and e are positivelyoriented, where 1 constitutes a perfect score. FAR (panel d) is negativelyoriented and a perfect model has an FAR of zero. The metrics shown in panels a–e have an upper bound of 1, and this is marked by the red dashed line. In every measure, the performance between the two models is indistinguishable at low values of K _{ p } – which, as we recall, constitutes the vast majority of geomagnetic conditions – but as the threshold for identifying an event increases we clearly see improved performance from the model. While the confidence intervals substantially overlap for these scores we note that parameter estimates with overlapping confidence intervals can be significantly different (Afshartous & Preston, 2010). In other words, while nonoverlapping confidence intervals are likely to show that the performance metrics are significantly different, the inverse is not necessarily true. Due to a variety of factors, we cannot assess the significance of the improvement in all performance metrics presented here. Among these are the fact that the metrics are correlated with each other, and we would need to correct for the effect of multiple significance tests. We have instead noted throughout this work where we were able to test for significance and described the consistent improvement in performance metrics. Although the improvement in these metrics is modest, we again conclude that adding the GOES Xray flux data improves the model’s ability to predict geomagnetically active times.
Fig. 12
Different performance metrics (a) HSS, (b) MCC, (c) PoD, (d) FAR, (e) CSI, and (f) Bias comparing the two variants of geomagnetic storm forecasting model at different K _{ p } thresholds. Model μ ^{OMNI} (in black circle) and (in blue diamonds). 
Finally, we assess the reliability of the probability distributions generated by our dGPR models. In this context, reliability assesses the agreement between the predicted probability and the mean observed frequency. In other words, if the model predicts a 50% chance of exceeding the storm threshold, is that prediction correct 50% of the time?
Figure 13 presents a reliability diagram of the observed probability of a geomagnetic storm (for different K _{ p } threshold levels, i.e. 2, 4, 6) plotted against the forecast probability of a geomagnetic storm. The top row – panels (a.1) and (a.2) – presents reliability diagram for models μ ^{OMNI} and , respectively. In this figure red, blue and black lines represent geomagnetic storm thresholds of K _{ p } = 2, 4 and 6 respectively. A perfectly reliable forecast should lie on the x = y line (black dashed line). For smaller chances of geomagnetic storms, both forecast models are reliable in their probabilistic predictions. As the predicted probability increases so do the tendency for the predicted probability to be higher than the observed probability. That is, the model tends to overforecast slightly. Comparing the reliability of μ ^{OMNI} to that of , we see similar results for activity thresholds of K _{ p } = 2 and 4. However, the model predictions for a stormtime threshold of K _{ p } = 6 are slightly more reliable than for its simpler counterpart.
Fig. 13
Reliability diagram showing observed frequency of a geomagnetic storm (for K _{ p } ≥ 2,4, and 6) plotted against the forecast probability of geomagnetic storms. 
The panels in the bottom row of Figure 13 are histograms showing the frequency of forecasts in each probability bin, also known as refinement distributions. These indicate the sharpness of the forecast, or the ability of the forecast to predict extremes in event probability. For example, a climatological mean forecast would have no sharpness and a deterministic model (i.e., a prediction with a delta function probability distribution) would be perfectly sharp, only ever predicting probabilities of zero or one. Ideally, a model would have both sharpness and reliability in its predicted probabilities. The refinement distributions presented here show that both μ ^{OMNI} and display sharpness, with local peaks near probabilities of zero and one.
Both models exhibit high sharpness, which can be interpreted as the confidence of the model in its event prediction (Wilks, 2006). Further, both models perform similarly for lower K _{ p } thresholds. The model, when using an event threshold of K _{ p } ≥6, has slightly improved calibration over the μ ^{OMNI}. The addition of the solar Xray flux data has consistently improved performance when assessing its performance in a deterministic setting, and here is shown to improve the calibration of the model at high activity levels without impact to the sharpness of the model. This analysis further supports the performance of our probabilistic model and confirms that the GOES Xray data adds value to our K _{ p } prediction model.
4 Discussion
In this study, we presented a novel, probabilistic, geomagnetic storm forecast model that predicts 3 h ahead. Our model structure combined an LSTM classifier and dynamicallytrained deep Gaussian processes to generate predictions of K _{ p } with an associated probability distribution. To test whether a simple, operationallyavailable data set could improve predictions of geomagnetic storm times, we trained two variants of our model: the first used only solar wind data and historical values of K _{ p }; the second added Xray fluxes from the NOAA GOES satellites, as a proxy for magnetic complexity at the Sun. Using a variety of model validation methods, we have confirmed that including the Xray data enhances the performance of the forecast model at times of high geomagnetic activity. Due to the low number of samples (at high K _{ p } levels) for model testing, many measures of model performance suggest an improvement in the model performance at high activity levels but statistical significance could not be demonstrated. Significance tests of the improvement in the correlation coefficients and the change of the ROC AUC show that there is a quantified, statisticallysignificant improvement in the model performance when GOES Xray flux data is included. In this section, we further analyze the performance metrics and compare them with prior studies.
Although exact comparisons should not be made as we use different data sets for model validation, we place our results in the context of previous work. In comparison with some earlier models (e.g., Boberg et al., 2000; Wing et al., 2005; Bala & Reiff, 2012) our models typically perform well, with an RMSE of 0.77. The performance, as measured by RMSE, is not as good as the RMSE for the 3 hahead predictions of Zhelavskaya et al. (2019) (RMSE = 0.67) and Tan et al. (2018) (RMSE = 0.64). To assess the performance of their model when predicting geomagnetic storm intervals (defined as K _{ p } ≥ 5), Tan et al. (2018) has calculated the F1score. This binary event metric is the harmonic mean of the precision and recall, using the nomenclature of machine learning literature. Using terminology from statistical literature, the precision is perhaps better known as the positive predictive value and represents the fraction of predicted positives that were correct. Similarly, the recall is the probability of detection and represents the fraction of observed events that were correctly predicted. The F1score for the Tan et al. (2018) model was 0.55. Our initial model (μ ^{OMNI}) gave an F1score of 0.56, while our model including the solar Xray flux data () gave an F1score of 0.6.
Recent studies mainly focused on the predictive skill of the K _{ p } forecast models, whereas, in this paper, we aim to provide a probabilistic prediction of K _{ p } without compromising the predictive skill of the model. We have further demonstrated that including a simple, operationallyavailable proxy for the likelihood of solar activity improves the prediction of geomagnetic storms. The inability of K _{ p } prediction models to predict larger storms (K _{ p } ≥ 5) well from L1 solar wind data has previously been discussed in the literature (see, e.g., Zhelavskaya et al., 2019), and this work shows that including solar Xray flux can directly improve the prediction of high levels of geomagnetic activity. In this work we found that including solar Xray flux in our model features reduces the overall RMSE by 0.01, from 0.78 to 0.77. At the same time the correlation coefficient increased by a small but statistically significant amount (from 0.82 to 0.83). Importantly, for the stormtime test data the RMSE was reduced by 0.58, from 1.48 to 0.9, and the correlation coefficient increased from 0.69 to 0.75. For details of the results and the significance testing, see Table 4 and Section 3.1. Similarly, we note that analyzing the area under the ROC curve shows a significant improvement in the probabilistic predictions of K _{ p }, for high activity levels, when Xray flux is included (see Sect. 3.3). These comparisons show that inclusion of solar flux can enhance the storm time forecasting capability without diminishing the performance during less active periods.
Although we present only one sample model architecture, we use this to highlight a straightforward method by which uncertainty bounds can be predicted using machinelearning models, and also improve predictions of intervals of high geomagnetic activity. This clear demonstration that the Xray flux data meaningfully improves our prediction of geomagnetic storms strongly suggests that future work including solar data sources are a promising way to extend the meaningful forecast horizon for high levels of geomagnetic activity. However, other operationallyavailable data sources exist that are likely to carry more information about magnetic complexity at the Sun (e.g., solar magnetograms; Arge et al., 2010), and hence using these will further improve the prediction of both the CME and nonCMEdriven geomagnetic activity. Further work is planned to investigate this work as well as incorporating other recent advances that will help improve the fidelity of our predictive model.
We also note that Zhelavskaya et al. (2019) explored methods for selecting model features and reducing a large number of candidate features to a smaller selection of those that are most important. Relative to their work we use a small number of features, all of which were selected based on a physicallymotivated interpretation and subject to the constraint of being products generally available operationally. Applying their feature selection methods and further developing the architecture, such as using convolution neural network to process and extract CME features from 2dimensional solar Xray and magnetogram data, would likely yield immediate improvements in the model performance.
5 Conclusion
The two main objectives addressed by this work were to: 1. build a probabilistic K _{ p } forecast model; and 2. test whether the inclusion of operationallyavailable proxies for solar activity could improve the prediction of geomagnetic storms (using K _{ p }, following the NOAA Gscale).
We presented a twolayer architecture, using an LSTM neural network to predict the likelihood of stormtime and deep Gaussian Process Regression models to predict the value of K _{ p } including uncertainty bounds. We then exploited these uncertainty bounds to provide a probabilistic geomagnetic storm forecast. Our analysis demonstrates that this architecture can be used to build probabilistic space weather forecast models with good performance.
Further, we tested two variants of our model that differed only in the input parameters (“features”). The first used only upstream solar wind data and the second added solar Xray flux data from the GOES spacecraft. Analysis of the predictions and the errors, for both the values of K _{ p } as well as the probability of exceeding a threshold in K _{ p }, showed that the addition of Xray flux data resulted in significant model performance improvements during geomagnetically active periods. The model using Xray flux data had a significantly higher correlation coefficient on the stormtime test data (increased from 0.69 to 0.75), with other performance metrics showing improvements. The RMSE on the stormtime data set decreased from 1.48 to 0.9. This improvement in model performance was also seen across all contingency tablebased metrics, with improvements in skill and reductions in false alarms. Similarly, the probabilistic predictions were shown to be significantly better by testing the difference in the area under the ROC curve. The probabilistic predictions were shown to be wellcalibrated and sharp.
Adding solar Xray flux data to empirical or machinelearned models can add useful information about transient solar activity, improving the 3h ahead prediction of the K _{ p } index for high geomagnetic activity levels. Although including this relatively simple data set increased the accuracy of the forecast, supporting the suggestion that Xray data is a reasonable proxy for solar magnetic activity, our model still shows lags in predicting large geomagnetic storms. Capturing uncertainty, providing probabilistic predictions and improving our ability to capture transient behavior are all within reach with modern tools and do not require sacrificing model predictive performance. We hope that future work continues to bring together recent advances in feature selection (e.g., Zhelavskaya et al., 2019), model design to accommodate probabilistic prediction, and more complex solar data sources such as solar magnetograms, to provide accurate forecasting of strong geomagnetic activity with longer lead times.
Acknowledgments
SC thanks to the Space Science and Applications group and the Center for Space and Earth Science (CSES) at Los Alamos National Laboratory for organizing and supporting the Los Alamos Space Weather Summer School. Portions of this work by SKM were performed under the auspices of the US Department of Energy and were partially supported by the Laboratory Directed Research and Development (LDRD) program, award number 20190262ER. The authors wish to acknowledge the use of the OMNI solar wind data, available at https://omniweb.gsfc.nasa.gov/ow.html. The K _{ p } index and GOES Xray datasets were accessed through the GFZPotsdam website https://www.gfzpotsdam.de/en/kpindex/ and NOAA FTP server https://satdat.ngdc.noaa.gov/sem/goes/data/, respectively. The majority of analysis and visualization was completed with the help of free, opensource software tools, notably: Keras (Chollet, 2015); matplotlib (Hunter, 2007); IPython (Perez & Granger, 2007); pandas (McKinney, 2010); Spacepy (Morley et al., 2011); PyForecastTools (Morley, 2018); and others (see, e.g., Millman & Aivazis, 2011). The code developed during this work is available at https://github.com/shibaji7/Codebase_Kp_Prediction. The editor thanks two anonymous reviewers for their assistance in evaluating this paper.
References
 Afshartous D, Preston RA. 2010. Confidence intervals for dependent data: Equating nonoverlap with statistical significance. Comput Stat Data Anal 54(10): 2296–2305. https://doi.org/10.1016/j.csda.2010.04.011. [CrossRef] [Google Scholar]
 AlShedivat M, Wilson AG, Saatchi Y, Hu Z, Xing EP. 2017. Learning scalable deep kernels with recurrent structure. J Mach Learn Res 18(82): 1–37. URL http://jmlr.org/papers/v18/16498.html. [Google Scholar]
 Arge CN, Henney CJ, Koller J, Compeau CR, Young S, MacKenzie D, Fay A, Harvey JW. 2010. Air force data assimilative photospheric flux transport (ADAPT) model. Twelfth Int Sol Wind Conf 1216: 343–346. https://doi.org/10.1063/1.3395870. [Google Scholar]
 Baker DN, Hones EW, Payne JB, Feldman WC. 1981. A high time resolution study of interplanetary parameter correlations with AE. Geophys Res Lett 8(2): 179–182. https://doi.org/10.1029/GL008i002p00179. [CrossRef] [Google Scholar]
 Bala R, Reiff P. 2012. Improvements in shortterm forecasting of geomagnetic activity. Space Weather 10(6): S06001. https://doi.org/10.1029/2012SW000779. [CrossRef] [Google Scholar]
 Bartels JR. 1949. The standardized index, Ks and the planetary index, Kp. IATME 97(12b): 0001. [Google Scholar]
 Bingham Suzy, Murray Sophie A, Guerrero Antonio, Glover Alexi, Thorn Peter. 2019. Summary of the plenary sessions at European Space Weather Week 15: Space weather users and service providers working together now and in the future. J Space Weather Space Clim 9: A32. https://doi.org/10.1051/swsc/2019031. [CrossRef] [Google Scholar]
 Boberg F, Wintoft P, Lundstedt H. 2000. Real time Kp predictions from solar wind data using neural networks. Phys Chem Earth Part C Sol Terr Planet Sci 25(4): 275–280. https://doi.org/10.1016/S14641917(00)000167. [Google Scholar]
 Borovsky JE. 2013. Physical improvements to the solar wind reconnection control function for the Earth’s magnetosphere. J Geophys Res Space Phys 118(5): 2113–2121. https://doi.org/10.1002/jgra.50110. [CrossRef] [Google Scholar]
 Borovsky JE. 2014. Canonical correlation analysis of the combined solar wind and geomagnetic index data sets. J Geophys Res Space Phys 119(7): 5364–5381. https://doi.org/10.1002/2013JA019607. [CrossRef] [Google Scholar]
 Borovsky JE, Denton MH. 2006. Differences between CMEdriven storms and CIRdriven storms. J Geophys Res Space Phys 111(A7) : A07S08. https://doi.org/10.1029/2005JA011447. [Google Scholar]
 Borovsky JE, Thomsen MF, Elphic RC, Cayton TE, McComas DJ. 1998. The transport of plasma sheet material from the distant tail to geosynchronous orbit. J Geophys Res Space Phys 103(A9): 20297–20331. https://doi.org/10.1029/97JA03144. [CrossRef] [Google Scholar]
 Bradley AP. 1997. The use of the area under the ROC curve in the evaluation of machine learning algorithms. Pattern Recogn 30(7): 1145–1159. https://doi.org/10.1016/S00313203(96)001422. [CrossRef] [Google Scholar]
 Camporeale E. 2019. The challenge of machine learning in space weather: Nowcasting and forecasting. Space Weather 17(8): 1166–1207. https://doi.org/10.1029/2018SW002061. [CrossRef] [Google Scholar]
 Carbary JF. 2005. A Kpbased model of auroral boundaries. Space Weather 3(10): S10001. https://doi.org/10.1029/2005SW000162. [CrossRef] [Google Scholar]
 Choi HS, Lee J, Cho KS, Kwak YS, Cho IH, Park YD, Kim YH, Baker DN, Reeves GD, Lee DK. 2011. Analysis of GEO spacecraft anomalies: Space weather relationships. Space Weather 9(6): S06001. https://doi.org/10.1029/2010SW000597. [Google Scholar]
 Chollet F. 2015. Keras. https://keras.io. [Google Scholar]
 Costello K.A.. 1998. Moving the rice MSFM into a realtime forecast mode using solar wind driven forecast modules. PhD Thesis. URL https://scholarship.rice.edu/handle/1911/19251. [Google Scholar]
 DeLong ER, DeLong DM, ClarkePearson DL. 1988. Comparing the areas under two or more correlated receiver operating characteristic curves: A nonparametric approach. Biometrics 44(3): 837–845. https://doi.org/10.2307/2531595. [CrossRef] [Google Scholar]
 Dungey JW. 1961. Interplanetary magnetic field and the auroral zones. Phys Rev Lett 6(2): 47–48. https://doi.org/10.1103/PhysRevLett.6.47. [NASA ADS] [CrossRef] [Google Scholar]
 Eastwood JP, Biffis E, Hapgood MA, Green L, Bisi MM, Bentley RD, Wicks R, McKinnell LA, Gibbs M, Burnett C. 2017. The Economic impact of space weather: Where do we stand? Risk Anal 37(2): 206–218. https://doi.org/10.1111/risa.12765. [CrossRef] [Google Scholar]
 Estabrooks A, Jo T, Japkowicz N. 2004. A multiple resampling method for learning from imbalanced data sets. Comput Intell 20(1): 18–36. https://doi.org/10.1111/j.08247935.2004.t01100228.x. [CrossRef] [Google Scholar]
 Garcia HA. 1994. Temperature and emission measure from GOES soft Xray measurements. Sol Phys 154(2): 275–308. https://doi.org/10.1007/BF00681100. [NASA ADS] [CrossRef] [Google Scholar]
 Gonzalez WD, Tsurutani BT, Clúa de Gonzalez AL. 1999. Interplanetary origin of geomagnetic storms. Space Sci Rev 88(3): 529–562. https://doi.org/10.1023/A:1005160129098. [NASA ADS] [CrossRef] [Google Scholar]
 Haiducek JD, Welling DT, Ganushkina NY, Morley SK, Ozturk DS. 2017. SWMF global magnetosphere simulations of January 2005: Geomagnetic indices and crosspolar cap potential. Space Weather 15(12): 1567–1587. https://doi.org/10.1002/2017SW001695. [CrossRef] [Google Scholar]
 Hochreiter S, Schmidhuber J. 1997. Long shortterm memory. Neural Comput 9(8): 1735–1780. https://doi.org/10.1162/neco.1997.9.8.1735. [CrossRef] [PubMed] [Google Scholar]
 Horne RB, Glauert SA, Meredith NP, Boscher D, Maget V, Heynderickx D, Pitchford D. 2013. Space weather impacts on satellites and forecasting the Earth’s electron radiation belts with SPACECAST. Space Weather 11(4): 169–186. https://doi.org/10.1002/swe.20023. [CrossRef] [Google Scholar]
 Hundhausen AJ. 1970. Composition and dynamics of the solar wind plasma. Rev Geophys 8(4): 729–811. https://doi.org/10.1029/RG008i004p00729. [CrossRef] [Google Scholar]
 Hunter JD. 2007. Matplotlib: A 2D graphics environment. Comput Sci Eng 9(3): 90–95. https://doi.org/10.1109/MCSE.2007.55. [NASA ADS] [CrossRef] [Google Scholar]
 Johnson JR, Wing S, Camporeale E. 2018. Transfer entropy and cumulantbased cost as measures of nonlinear causal relationships in space plasmas: applications to D_{st}. Ann Geophys 36(4): 945–952. https://doi.org/10.5194/angeo369452018. [CrossRef] [Google Scholar]
 Kahler SW, Ling AG. 2018. Forecasting solar energetic particle (SEP) events with fare Xray peak ratios. J Space Weather Space Clim 8: A47. https://doi.org/10.1051/swsc/2018033. [CrossRef] [Google Scholar]
 Kay HRM, Harra LK, Matthews SA, Culhane JL, Green LM. 2003. The soft Xray characteristics of solar flares, both with and without associated CMEs. Astron Astrophys 400(2): 779–784. https://doi.org/10.1051/00046361:20030095. [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Kilpua EKJ, Luhmann JG, Gosling J, Li Y, Elliott H, et al. 2009. Small solar wind transients and their connection to the largescale coronal structure. Sol Phys 256(1): 327–344. https://doi.org/10.1007/s1120700993661. [NASA ADS] [CrossRef] [Google Scholar]
 Liemohn MW, McCollough JP, Jordanova VK, Ngwira CM, Morley SK, et al. 2018. Model evaluation guidelines for geomagnetic index predictions. Space Weather 16(12): 2079–2102. https://doi.org/10.1029/2018SW002067. [CrossRef] [Google Scholar]
 Lippiello E, de Arcangelis L, Godano C. 2008. Different triggering mechanisms for solar flares and coronal mass ejections. Astron Astrophys 488(2): L29–L32. https://doi.org/10.1051/00046361:200810164. [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Luo B, Liu S, Gong J. 2017. Two empirical models for shortterm forecast of Kp. Space Weather 15(3): 503–516. https://doi.org/10.1002/2016SW001585. [CrossRef] [Google Scholar]
 Mayaud PN. 1980. Derivation, meaning and use of geomagnetic indices. In: Vol. 22 of Geophysical monograph, American Geophysical Union. https://doi.org/10.1029/GM022. [Google Scholar]
 McKinney W. 2010. Data structures for statistical computing in python. In: Proceedings of the 9th Python in Science Conference, van der Walt S, Millman J, (Eds.), pp. 56–61. https://doi.org/10.25080/Majora92bf1922012. [Google Scholar]
 Michalek G. 2009. Two types of flareassociated coronal mass ejections. Astron Astrophys 494(1): 263–268. https://doi.org/10.1051/00046361:200810662. [CrossRef] [EDP Sciences] [Google Scholar]
 Millman KJ, Aivazis M. 2011. Python for scientists and engineers. Comput Sci Eng 13(2): 9–12. https://doi.org/10.1109/MCSE.2011.36. [CrossRef] [Google Scholar]
 Morley S.. 2018. drsteve/PyForecastTools: PyForecastTools. https://doi.org/10.5281/zenodo.1256921. [Google Scholar]
 Morley SK. 2019. Challenges and opportunities in magnetospheric space weather prediction. Space Weather 18(3): e2018SW002108. https://doi.org/10.1029/2018SW002108. [Google Scholar]
 Morley SK, Koller J, Welling DT, Larsen BA, Henderson MG, Niehof JT. 2011. Spacepy – A pythonbased library of tools for the space sciences. In: Proceedings of the 9th Python in Science Conference (SciPy 2010), Austin, TX, pp. 67–71. URL https://conference.scipy.org/proceedings/scipy2010/pdfs/morley.pdf. [Google Scholar]
 Morley SK, Brito TV, Welling DT. 2018a. Measures of model performance based on the log accuracy ratio. Space Weather 16(1): 69–88. https://doi.org/10.1002/2017SW001669. [CrossRef] [Google Scholar]
 Morley SK, Welling DT, Woodroffe JR. 2018b. Perturbed input ensemble modeling with the space weather modeling framework. Space Weather 16(9): 1330–1347. https://doi.org/10.1029/2018SW002000. [CrossRef] [Google Scholar]
 Murphy AH. 1995. The coefficients of correlation and determination as measures of performance in forecast verification. Weather Forecast 10(4): 681–688. https://doi.org/10.1175/15200434(1995)010<0681:TCOCAD>2.0.CO;2. [CrossRef] [Google Scholar]
 Newell PT, Sotirelis T, Liou K, Meng CI, Rich FJ. 2007. A nearly universal solar windmagnetosphere coupling function inferred from 10 magnetospheric state variables. J Geophys Res Space Phys 112(A1): A01206. https://doi.org/10.1029/2006JA012015. [Google Scholar]
 Núñez M. 2018. Predicting wellconnected SEP events from observations of solar soft Xrays and nearrelativistic electrons. J Space Weather Space Clim 8: A36. https://doi.org/10.1051/swsc/2018023. [CrossRef] [Google Scholar]
 Obrien TP. 2009. SEAESGEO: A spacecraft environmental anomalies expert system for geosynchronous orbit. Space Weather 7(9): S09003. https://doi.org/10.1029/2009SW000473. [Google Scholar]
 Osthus D, Caragea PC, Higdon D, Morley SK, Reeves GD, Weaver BP. 2014. Dynamic linear models for forecasting of radiation belt electrons and limitations on physical interpretation of predictive models. Space Weather 12(6): 426–446. https://doi.org/10.1002/2014SW001057. [CrossRef] [Google Scholar]
 Perez F, Granger BE. 2007. IPython: A system for interactive scientific computing. Comput Sci Eng 9(3): 21–29. https://doi.org/10.1109/MCSE.2007.53. [CrossRef] [Google Scholar]
 Qiu Q, Fleeman JA, Ball DR. 2015. Geomagnetic disturbance: A comprehensive approach by American electric power to address the impacts. IEEE Elect Mag 3(4): 22–33. https://doi.org/10.1109/MELE.2015.2480615. [CrossRef] [Google Scholar]
 Rasmussen CE, Williams CKI. 2006. Gaussian processes for machine learning. MIT Press. URL http://www.gaussianprocess.org/gpml/. [Google Scholar]
 Revelle W.R.. 2020. psych: Procedures for personality and psychological research. R package version 1.9.12.31, URL https://CRAN.Rproject.org/package=psych. [Google Scholar]
 Richardson IG, Cane HV. 2012. Solar wind drivers of geomagnetic storms during more than four solar cycles. J Space Weather Space Clim 2: A01. https://doi.org/10.1051/swsc/2012001. [Google Scholar]
 Robin X, Turck N, Hainard A, Tiberti N, Lisacek F, Sanchez JC, Müller M. 2011. pROC: An opensource package for R and S+ to analyze and compare ROC curves. BMC Bioinform 12(77). https://doi.org/10.1186/147121051277. [CrossRef] [Google Scholar]
 Schrijver CJ, Kauristie K, Aylward AD, Denardini CM, Gibson SE, et al. 2015. Understanding space weather to shield society: A global road map for 2015–2025 commissioned by COSPAR and ILWS. Adv Space Res 55(12): 2745–2807. https://doi.org/10.1016/j.asr.2015.03.023. [NASA ADS] [CrossRef] [Google Scholar]
 Schwenn R, Dal Lago A, Huttunen E, Gonzalez WD. 2005. The association of coronal mass ejections with their effects near the Earth. Ann Geophys 23(3): 1033–1059. https://doi.org/10.5194/angeo2310332005. [NASA ADS] [CrossRef] [Google Scholar]
 Sexton ES, Nykyri K, Ma X. 2019. Kp forecasting with a recurrent neural network. J Space Weather Space Clim 9: A19. https://doi.org/10.1051/swsc/2019020. [CrossRef] [Google Scholar]
 Sharpe MA, Murray SA. 2017. Verification of space weather forecasts issued by the met office space weather operations centre. Space Weather 15(10): 1383–1395. https://doi.org/10.1002/2017SW001683. [CrossRef] [Google Scholar]
 Shprits YY, Vasile R, Zhelavskaya IS. 2019. Nowcasting and predicting the Kp index using historical values and realtime observations. Space Weather 17(8): 1219–1229. https://doi.org/10.1029/2018SW002141. [CrossRef] [Google Scholar]
 Srivastava N, Venkatakrishnan P. 2002. Relationship between CME speed and geomagnetic storm intensity. Geophys Res Lett 29(9): 11–14. https://doi.org/10.1029/2001GL013597. [CrossRef] [Google Scholar]
 Srivastava N, Venkatakrishnan P. 2004. Solar and interplanetary sources of major geomagnetic storms during 1996–2002. J Geophys Res Space Phys 109(A10): A10103. https://doi.org/10.1029/2003JA010175. [NASA ADS] [CrossRef] [Google Scholar]
 Steiger JH. 1980. Tests for comparing elements of a correlation matrix. Psychol Bull 87(2): 245–251. https://doi.org/10.1037/00332909.87.2.245. [CrossRef] [Google Scholar]
 Sun X, Xu W. 2014. Fast implementation of DeLong’s algorithm for comparing the areas under correlated receiver operating characteristic curves. IEEE Sig Proc Lett 21(11): 1389–1393. https://doi.org/10.1109/LSP.2014.2337313. [CrossRef] [Google Scholar]
 Tan Y, Hu Q, Wang Z, Zhong Q. 2018. Geomagnetic index Kp forecasting with LSTM. Space Weather 16(4): 406–416. https://doi.org/10.1002/2017SW001764. [CrossRef] [Google Scholar]
 Tóth G, Sokolov IV, Gombosi TI, Chesney DR, Clauer CR, et al. 2005. Space weather modeling framework: A new tool for the space science community. J Geophys Res Space Phys 110(A12): A12226. https://doi.org/10.1029/2005JA011126. [NASA ADS] [CrossRef] [Google Scholar]
 Wilks DS. 2006. Statistical methods in the atmospheric sciences, 2nd edn, Academic Press. https://www.elsevier.com/books/statisticalmethodsintheatmosphericsciences/wilks/9780123850225. [Google Scholar]
 Wing S, Johnson JR, Jen J, Meng CI, Sibeck DG, Bechtold K, Freeman J, Costello K, Balikhin M, Takahashi K. 2005. Kp forecast models. J Geophys Res Space Phys 110(A4): A04203. https://doi.org/10.1029/2004JA010500. [Google Scholar]
 Wing S, Johnson JR, Camporeale E, Reeves GD. 2016. Information theoretical approach to discovering solar wind drivers of the outer radiation belt. J Geophys Res Space Phys 121(10): 9378–9399. https://doi.org/10.1002/2016JA022711. [CrossRef] [Google Scholar]
 Winter LM, Balasubramaniam KS. 2014. Estimate of solar maximum using the 1–8Å geostationary operational environmental satellites X–ray measurements. Astrophys J 793(2): L45. https://doi.org/10.1088/20418205/793/2/l45. [CrossRef] [Google Scholar]
 Winter LM, Balasubramaniam K. 2015. Using the maximum Xray flux ratio and Xray background to predict solar flare class. Space Weather 13(5): 286–297. https://doi.org/10.1002/2015SW001170. [NASA ADS] [CrossRef] [Google Scholar]
 Wintoft P, Wik M, Matzka J, Shprits Y. 2017. Forecasting Kp from solar wind data: input parameter study using 3hour averages and 3hour range values. J Space Weather Space Clim 7: A29. https://doi.org/10.1051/SWSC/2017027. [CrossRef] [Google Scholar]
 Wu DJ, Feng HQ, Chao JK. 2008. Energy spectrum of interplanetary magnetic flux ropes and its connection with solar activity. Astron Astrophys 480(1): L9–L12. https://doi.org/10.1051/00046361:20079173. [CrossRef] [EDP Sciences] [Google Scholar]
 Xu F, Borovsky JE. 2015. A new fourplasma categorization scheme for the solar wind. J Geophys Res Space Phys 120(1): 70–100. https://doi.org/10.1002/2014JA020412. [NASA ADS] [CrossRef] [Google Scholar]
 Yap BW, Rani KA, Rahman HAA, Fong S, Khairudin Z, Abdullah NN. 2014. An application of oversampling, undersampling, bagging and boosting in handling imbalanced datasets. In: Proceedings of the First International Conference on Advanced Data and Information Engineering (DaEng2013), Herawan T., Deris M.M., Abawajy J. (Eds.), Springer Singapore, Singapore, pp. 13–22. [Google Scholar]
 Zhang J, BlancoCano X, Nitta N, Srivastava N, Mandrini CH. 2018. Editorial: Earthaffecting solar transients. Sol Phys 293: 80. https://doi.org/10.1007/s1120701813029. [CrossRef] [Google Scholar]
 Zhelavskaya IS, Vasile R, Shprits YY, Stolle C, Matzka J. 2019. Systematic analysis of machine learning and feature selection techniques for prediction of the Kp index. Space Weather 17(10): 1461–1486. https://doi.org/10.1029/2019SW002271. [CrossRef] [Google Scholar]
 Zhou G, Wang J, Cao Z. 2003. Correlation between halo coronal mass ejections and solar surface activity. A&A 397(3): 1057–1067. https://doi.org/10.1051/00046361:20021463. [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Cite this article as: Chakraborty S & Morley S. 2020. Probabilistic prediction of geomagnetic storms and the K_{p} index. J. Space Weather Space Clim. 10, 36.
All Tables
Table showing different categories of geomagnetic storm and associated K _{ p } levels. The categorization is done based on the intensity of the geomagnetic storm following the NOAA SWPC scales.
Table showing input features of the model, transformations used (if any), and which models use each feature. The given transformation is only used prior to fitting the Gaussian process model. BoxCox → B(x) = sgn(x) × log_{e} x and Erf → erf(x) = .
All Figures
Fig. 1
Autocorrelation functions of different solarwind parameters during: (a) solar minima, and (b) solar maxima. 

In the text 
Fig. 2
Crosscorrelation functions of different solarwind parameters with (a) GOES flux background (B) and (b) ratio (R) of hard (0.05–0.4 nm) and soft (0.1–0.8 nm) Xray flux data. 

In the text 
Fig. 3
Distribution of K _{ p }. 20 years 1995–2014 of data has been used in this plot. f(K _{ p }) is the frequency (i.e., the number of events) plotted on a logarithmic scale. The black vertical line is K _{ p } = 5^{−}. 

In the text 
Fig. 4
Schematics showing architectures (a) of a single LSTM block, (b) of the classifier consisting of one input layer, one LSTM layer consists of 100 nodes (neurons), dropout, and output layer, and (c) of the classifier model implemented using Keras. 

In the text 
Fig. 5
Proposed model (μ) architecture: Classifier is deterministic in nature, and regressors are probabilistic in nature. The threshold for the classifier is K _{ p } = 5^{−}. Here, w _{ q } & w _{ s } are the variable training windows for two regressors. For details refer text. 

In the text 
Fig. 6
Variation of root mean square error (RMSE, ε) in with the length of the training window (τ) in days. Each point of this curve is generated using the average RMSE of two months of data. 

In the text 
Fig. 7
Threehour forecast of K _{ p } using LSTM classifier & Deep Gaussian Process Regression (Deep GPR) for a solar maximum period (1st July–31st August, 2004). Panels: (a) prediction from the model using OMNI solar wind data and (b) prediction from the model using OMNI solar wind data and GOES solar flux data. Blue and black dots in panels (a) and (b) are mean predictions and red dots show observed K _{ p }, respectively. Light blue and black shaded regions in panels (a) and (b) respectively show 95% confidence interval. RMSE (ε) and MAE () are mentioned inside each panel. 

In the text 
Fig. 8
The performance comparison of μ ^{OMNI} and models which predict K _{ p } 3h ahead. Panels present performance of μ ^{OMNI} (in black) and (in blue) models for (a) 10 years of prediction and (b) 38 stormtime prediction (listed in the Table 3). In each panel official (Postdam) K _{ p } is plotted on the xaxis and the model prediction is plotted on the yaxis. Perfect predictions would lie on the line with a slope of one. The error bar indicates one standard deviation and the correlation coefficient and coefficient of determination are mentioned inside each panel. 

In the text 
Fig. 9
Threehour forecast (using model) showing (a) probability of geomagnetic storms, (b) K _{ p } (22nd July–31st July, 2004) and (c) an illustration of the method to extract probability of storm occurrence for one prediction marked by vertical black line in panel (b). Black dashed lines in panels (b) and (c) represent the threshold K _{ p } = 5^{−}, red and blue thin lines in panel (c) are observed K _{ p }, and predicted mean respectively. Panel (b) is in the same format with Figure 7. The shaded region in panel (c) provides probability of geomagnetic storm (Pr[e] = 0.81, for details refer text). 

In the text 
Fig. 10
Example model predictions using μ ^{OMNI} model showing true positive (TP), false positive (FP), false negative (FN), and true negative (TN) predictions, mentioned by vertical lines. Top and bottom panels show the probability of geomagnetic storms and K _{ p } with uncertainty bounds (shaded) region. 

In the text 
Fig. 11
Receiver operating characteristic (ROC) curves showing the relative performance of individual the storm forecasting model μ ^{OMNI} (represented by solid curves) and (represented by dashed curves) with different storm intensity levels (for K _{ p } ≥ 2, 4, and 6). 

In the text 
Fig. 12
Different performance metrics (a) HSS, (b) MCC, (c) PoD, (d) FAR, (e) CSI, and (f) Bias comparing the two variants of geomagnetic storm forecasting model at different K _{ p } thresholds. Model μ ^{OMNI} (in black circle) and (in blue diamonds). 

In the text 
Fig. 13
Reliability diagram showing observed frequency of a geomagnetic storm (for K _{ p } ≥ 2,4, and 6) plotted against the forecast probability of geomagnetic storms. 

In the text 
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