Types of heat generation in Ukraine in 2016 and their cost
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Fig. 2 shows the annual mean values of global irradiation recorded during 2006 and 2007. The zones with the highest values of irradiation (greater than 14 MJ m2 day1) are located along the southwestern border of the Ourense province. This zone is characterized by low precipitations and relative humidity (Fig. 3); however, lowest average annual temperatures (Fig. 4a) compared to the rest of the region are due to the lowest cold temperatures in wintertime, that are not balanced by its highest hot temperatures in summertime; this is typical from this clearer sky zone than the rest of the region.
Fig. 4: Annual mean values of (a) temperature (°С) and (b) daily sunshine hours (hr) over the region.
On the other side, the lowest values of irradiation (less than 11 MJ m2 day1) are found in the northern edge of the region, in the southern edge (around Monte Aloia station) and near the stations of Ourense and Sergude. Typical foggy conditions over valleys close to rivers (Ourense and Sergude stations) or along coastal line (northern edge) reduce the sunshine hours, as it is shown on Fig. 4b), so irradiation is lower than in the rest of the region. At Monte Aloia mountain, high precipitation values are achieved (Fig. 3a), due to typical wintertime wet air masses from the Atlantic Ocean carrying rain clouds over this coastal mountain (Foehn effect) [16].
Annual clearness index, KT, was estimated in order to evaluate both the influence of local conditions and geographical coordinates over the solar irradiation. As it is observed on Fig. 5 compared to Fig. 2, KT distribution is quite similar to global irradiation map, with extreme values located at the same zones. Therefore, local conditions are the most important affecting the solar radiation that achieved the ground level.
Fig. 5: Annual mean values of clearness index (Xt) over the region.
This comparison shows that either high resolution solar irradiation maps or long term solar irradiation measurements are required to evaluate the solar resource in any location of this region.
G. Lopez1*, F. J. Batlles2 and J. L. Bosch2
1 Departamento de Ingenieria Electrica y Termica, Escuela Politecnica Superior, Universidad de Huelva,
21819, Huelva, Spain
2 Departamento de Fisica Aplicada, Universidad de Almeria, Almeria, Spain
Corresponding Author, gabriel. lopez@die. uhu. es
In this work we analyse a daily global irradiance time series into the framework of chaotic dynamic systems in order to examine a possible underlying nonlinear behaviour. Employed methods are based on a phase space reconstruction from the measured data and are devoted to the calculation of the properties of an underlying attractor, such as the Lyapunov exponents. Researches on these dynamical system invariants will point out the presence of chaos. We also use local lineal models as a test for nonlinearity.
The global solar radiation data were measured at the radiometric station of the University of Almeria (Spain) during eight years. Results have shown the nonexistence of any attractor in the phase space for the global irradiance time series. Negative Lyapunov exponents exclude a chaotic behaviour that might allow a better short term prediction than autoregressive models, and the idea of the existence of a nonlinear differential equation system. These results match with those obtained from applying local linear models for prediction, of which estimations suggest that the data are best described by a linear stochastic process.
Keywords: solar radiation, forecasting, chaos, nonlinear time series.
Information on the availability of solar radiation is needed in many applications dealing with the exploitation of solar energy. Particularly, global solar radiation is one of the most important input parameters for any solar energy system and different techniques have been developed to model and forecast it. Once the solar energy system (like concentrated solar power plants) is running, prediction of power load, normally done on an hourly basis with a prediction horizon between 1 and 24 hours, is instrumental for planning and operation of the total power system, e. g. for buying or selling power or for solving the unit commitment and dispatch problems.
Studies about solar radiation time series and other meteorological variables with autoregressive or stochastic models [13] have experienced an important growth in the last years, since synthetic sequences statistically indistinguishable from the original ones are needed to design the solar devices properly. However, using this type of model, prediction from past values is limited due to the random character exhibited by these time series. The main factor of randomness affecting global solar radiation data is due to variations in the sky cloud cover, which make the radiation on cloudy days difficult to predict.
Appearing of several nonlinear dynamical models developed by Lorenz [4], with a fully irregular and complex behaviour (generically named chaos), allows to study the nature of fluctuations in solar radiation data from a new methodology. Time series from many system evolutions, apparently evolving in a random way, can now be predicted with higher precision than with traditional ARMA models, at least for short term predictions. Detection of chaos in a time series would thus allow a better modelling of time series against statistically based models.
In this paper, we analyse a daily global solar irradiance time series into the framework of chaotic dynamic systems in order to examine a possible underlying nonlinear behaviour. Existence of chaos should help to improve the short term predictions performed by means of the traditional
statistical techniques. Employed methods are based on a phase space reconstruction from the measured data and are devoted to the calculation of the properties of an underlying attractor, such as the Lyapunov exponents. We also use local lineal models as a test for nonlinearity.
The horizontal global solar radiation time series (symbolized by {xt}, being t the time step in days) consisted of 2945 daily values. They were obtained by integration from experimental values averaged every ten minutes during the years 19901992 and every five minutes during the years 19931998. The measurements were recorded at the radiometric station of the University of Almeria (36.8° N, 2.44° W) in southeastern Spain by means of a Kipp and Zonen CM11 pyranometer. Measurements from other two pyranometers (LICOR, model LI200) were also available. They were used to detect and replace any anomalous value measured by the CM11 pyranometer. The calibration constants of the pyranometers were checked periodically by our research group. Measurements by the LI200 pyranometers were also corrected following [5].
Again, as for the ordinary kriging, a seasonal pattern is present, with the summer months showing the lowest RMSE values and the winter months the highest ones. Particularly, lowest RMSE relative value are found for February 0.54 MJ m2day1 (4.5%) and the highest for October 1.31 MJ m2day1 (10.2 %). MAE ranges from 0.22 MJ m2day1 (2.2%) in January to 0.70 MJ m2day1 (5.4%) in October. Regarding the ME, the model tends to slightly overestimate the solar radiation, for all the months, but ME values are fairly low. Figure 4 shows the estimated H maps based on the residual kriging procedure.
The clear sky index is an appropriate and thus an established quantity for the description of the transmission properties of the Earth’s atmosphere.
It is defined by
k* = Ig / Idear (3)
where the current global radiation Ig is related to the expected clear sky radiation Idear. In addition a model is needed, which describes the atmospheric conditions, a so called clear sky model, see sec. 2.2.
[Beyer et al. 96] introduced the relation
k* = 1 — n (4)
into the Heliosat method. This relation can be used without a previous calibration with ground data, but it is necessary that the clear sky model is optimally adapted to the regarded area. By Fontoynont et al. [2] relation (4) was improved in order to detail the case of complete cloudiness and to limit the clear sky index to meaningful values.
The influence of the albedo on the SSI varies with the solar zenith angle and the atmospheric turbidity. This influence is assessed by computing the difference between the SSIs obtained with the ground albedo equal to respectively 0 and 0.2 (Fig. 5).
The influence of the albedo on the SSI decreases as the wavelength increase because the intensity of diffusion decreases. It increases with increasing atmospheric turbidity and so, decreases also with increasing visibility. This influence decreases when the solar zenith angle is growing because of the decreasing of the SSI; this is also true for the relative deviation. Presence of clouds increases the relative influence of the albedo: the larger tc, the larger the relative deviation.
The dataset used in this study is based on pyranometric global solar irradiance ground measurements which belongs to stations of the Spanish National Radiometric Network from Agencia Espanola de Meteorologia (AEMet) sited in Madrid (40.45°N, 3.72°W, 680 m.). The period of data acquired goes from 1st of January 1979 up to 31st of December 2003 having 17376 of half daily values.
The quality of pyranometric available data and temporal acquisition of measurements are two crucial factors related to adjustment of proposed models. In this study an exhaustive quality analysis has been done on both important factors which influence high quality measurements (based on BSRN recommendations). Manufacturer of pyranometers used is the Dutch firm Kipp&Zonen and belong to CM11 series.
The mean daily solar radiation presents a seasonal variation due principally to the variation of the position of the earth to the sun and a stochastic aspect introduced by atmospheric components (aerosols, H2O, O3,…).
Half daily ground solar radiation shows a seasonal trend with fluctuations from day to day due to cloudiness, changing air mass and aerosols. The seasonal trend can be separated in several different ways: (1) “clearness sky index” based on extracting the influence of latitude, dividing between measured ground solar radiation and extraterrestrial solar radiation values, (2) subtraction of the annual harmonic (first harmonic of Fourier analysis), (3) “lost component” which is based on the subtraction of each value of the extraterrestrial radiation the corresponding value of ground solar radiation. In general, approach (1) leads to a procedure much simpler from the point of view of the user, but it is not suitable because statistical forecasting methods needs predictors with stationary behaviour and Gaussian distribution.
Three different methods are currently proposed to forecast solar radiation. The first is based on time series models, which use a series of the daily average of the measured solar radiation as input data. It has been shown in different papers that a RMSE of 5.1 % [7], 8.3 % [8], and 8.4 % [9] can be obtained, for local predictions using ANN — wavelet methods. Whereas in [7] and [8] the Continuous Wavelet Transform (CTW) is used, [9] employs the Discrete Wavelet Transform (DWT). The author of [8] uses the day number of the year and defuzzficated cloud cover information from the weather forecast service, as auxiliary information. These models are applicable for sites where the solar radiation was measured during one year [7], two years [8], or longer time intervals [7], [9]. The second method is able to forecast the motion of clouds using satellite imaging over the earth surface. It can forecast the solar radiation for any site or area, but the uncertainty related to the utilized models increases substantially over 22% to 30%, for forecast horizons larger than six hours, as reported by Lorenz [10]. The author obtained the former value for low and the latter for high cloud variability. The third method, used in the present article, is based on the NWP with its statistical correction MOS.
This study has been conducted within the Natural Park of Sierra Magina, in Southern Spain (37.6° N, 3.4° W) (Fig. 1). The area has a rough extension of 30 km x 48 km and shows a relatively complex topography, with a minimum height above sea level of 600 m and a maximum of 2150 m, with the 50% of the grids points above 800 m. The maximum surface slope is 56.94° and the 25% of the grids have a slope higher than 16.41°. The predominant surface orientation is around North. This aspects distribution benefits the existence of terrain patches with no direct solar beam along the year. The local climate is that of a typical middle and high Mediterranean mountainous environment, with dry hot summers, cold winters and relatively high precipitation during autumn and spring.
Located within the park, our research group have deployed a total of 11 radiometric stations (Figure 2). The radiometric stations are equipped, among other instrumentation, with HOBO (Onset Corporation) dataloggers that record the global irradiance registered by Licor 200SZ radiometers. An annual calibration and intercomparison of the sensors is carried out and the instrumental error is estimated to be less than 5%, typically 3%. The data set consists on data recorded on a 10 minutes basis and, for the purposes of this work, they were averaged to a hourly basis. In order to avoid the cosine error of the sensors, those data corresponding to a solar height below 7° were discarded. The location of the stations cover a range of elevations, slopes and aspects as wide as was possible. Table 1 shows the topographic features of the stations.





5
8
Mr
Fig. 2. Location of the stations. Results at stations 4, 5 and 11 are evaluated in this study.
Station 
Name 
Elevation(m. a.s. l.) 
Slope (°) 
Aspect (°) 
1 
Jaen 
443 
0 
0 
2 
Mancha Real 
762 
0 
0 
3 
Almaden 
1982 
0 
0 
4 
Torres 
1075 
25 
250 
5 
Albanchez 
854 
30 
100 
6 
Bedmar 
634 
15 
270 
7 
Cuadros 
603 
25 
115 
8 
Moraleda 
704 
16 
110 
9 
Huelma 
859 
0 
0 
10 
Cedefo 
1155 
0 
0 
И 
Pegalajar 
791 
15 
170 
Table 1. Topographic features of the stations. Aspect values are presented in decimal degrees measured from North, increasing clockwise. Results presented in this study correspond to stations 4, 5 and 11 (underlined). 
Differences between global solar radiation interpolated from ground level measurements (Fig. 2 values) and published in [7] were shown on Fig. 6. As it is observed, a nonhomogeneous distribution of significant relative differences (from +25 to 60 %) indicates the high dependence of solar radiation from the local conditions in every location. Therefore, it should be recommended a calibration of satellite data from a number of ground level measurements (ideally, from all of the available stations) that can represent these local effects.
From the 34 students registered in the Solar Radiation subject, 32 started their work selecting a meteorological station to process. 31 students passed the subject in the first attempt (including a written exam by 60 % of the total qualification); just one student required to repeat the written exam, in order to pass the subject. The other two students abandon the subject.
The interest of the students in this work was higher than the theoretical issues and practical problems of the subject. Specially, processing meteorological datasets from real stations selected by the students was an extra incentive. And, in addition, processed datasets result very useful to get a solar resource evaluation in the region over the studied period, as only minor revisions of students’ calculations were required.
In this work an estimation of the annual solar resource over Galicia was developed, in the framework of a selflearning experience with the collaboration of students of the MSc in Renewable Energies and Energetic Sustainability. This educational experience was very successful, as the interest of the students was very high and their results were very useful to achieve the solar resource maps.
From the solar global irradiation distribution, solar resource in this region is extremely connected to the local conditions (local cloudiness, rain, fog), that are very variable because of the changeable weather and complex topography of this region. Although the validity of these results is limited to an annual period, irradiation distribution shows the necessity to consider local conditions in the application of any methodology to estimate solar resources at Galicia.
As the main conclusion, satellite data processing has to be completed with a high number of ground level measurements. Other techniques, as Digital Terrain Models (DTM) [17], allow to estimating ground level irradiation considering topographic effects; these technique can help to cover complex terrain zones with lack of ground level data.
Meteorological dataset provided by MeteoGalicia (Xunta de Galicia) from its web page is acknowledged. Dataset processing was partially developed by the students of the MSc in Renewable Energies and Energetic Sustainability of the University of Santiago de Compostela (200708 academic year).
This work was partially funded by Galician regional R&D Programme (Xunta de Galicia) under project 07REM02CT.
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The first step in any analysis of chaotic data is to reconstruct an attractor (defined as set of points in phase space visited by a signal trajectory after transients are gone) from the data. Taken [6] suggested a method of phase space reconstruction that is known as the method of delays. This method consists of embedding the time series into a ddimensional space, ^d, which is equivalent to the original unknown phase space composed of all the dynamical variables. Figure 1a shows the lag space plot for the global solar radiation time series using a lag of one. Points are distributed around a 45° straight line denoting a periodic nonchaotic time series. This is also evidenced observing the correlogram showed in Fig. 1b. An annual cycle of 365 days is presented. This is an expected result as the daily values of solar radiation are mainly affected by the earth motion.
xt (MJ/m2) Lags (days)
Fig. 1. a) Phase space structure of the global solar radiation time series using lags of one; b) Correlogram for
the global solar radiation time series.
In order to remove periodicity and trend, a transformation of the time series is undertaken by differencing. The new data are arithmetic differences between pairs of observations using a lag of one day (Axt = xt+I — xt). The differenced time series is denoted as {Axt}. Figure 2a shows the phase space plot for the differenced time series. The periodic pattern shown in the above figure seems to be removed. This result is corroborated analysing the correlogram displayed in Figure 2b. Autocorrelation coefficients fall to within the randomlike zone after the first lag and, for the most part, remain in that zone thereafter. It is thus assumed that periodicity is removed.
Although point distribution in Fig. 2a seems to be due to some nonrandom complex underlying behaviour, the presence of a chaotic attractor in that phase space is not clear. To search the
optimum time delay г we have used the method of mutual information [7]. Mutual information, like autocorrelation, tries to measure the extent to which values Axt+m are related to values of Axt, at a given lag. However, mutual information has the advantage of using probabilities, rather than a linear basis, to asses the correlation and thus, nonlinear correlations are taken into accounts. The software implementation of that algorithm (and of those used hereafter) is from the TISEAN package [8].
400
As a prescription, a good candidate for the time delay г will be where the first marked minimum of mutual information occurs. From Fig. 3 it is noted that the first minimum is for г = 3. Once the time delay is chosen, the next step is to select the embedding dimension. Kennel et al. [9] introduce the method called the false nearest neighbors, which calculates the minimal embedding dimension. Two points in a ddimensional phase space are false neighbors, in the sense of some distance function, when the distance, xjd — x/, is small but the distance xi+1d+1 — Xj+1d+1 in a d+1 dimensional phase space is not. Given a distance function, the Euclidean distance in our case, and some threshold size, the percentage of false near neighbors becomes zero as the dimension of phase space goes to the minimal embedding dimension. Figure 4 shows the percentage of false nearest neighbors as a function of the embedding dimension d. The main characteristic is that the fraction of false nearest neighbors does not fall to zero as d increases. This implies that the differenced time series has residual ‘noise’ in it, and thus the existence of low dimensional chaos is to be discarded.