Issue 
J. Space Weather Space Clim.
Volume 1, Number 1, 2011



Article Number  A03  
Number of page(s)  7  
DOI  https://doi.org/10.1051/swsc/2011003  
Published online  26 October 2011 
Two methods to forecast auroral displays
^{1}
The University Centre in Svalbard (UNIS), N9171 Longyearbyen, Norway
*
^{2}
Norwegian Space Centre, Oslo, Norway
^{3}
Polar Geophysical Institute, Murmansk Region, Apatity, Russia
^{4}
Geophysical Institute, University of Alaska, Fairbanks, USA
^{*} corresponding author: email: freds@unis.no
Received:
5
May
2011
Accepted:
6
September
2011
This work compares the methods by Starkov (1994a) and Zhang & Paxton (2008), that calculate the size and location of the auroral ovals as a function of planetary Kp index. The ovals are mapped in position and time onto a solar illuminated surface model of the Earth. It displays both the night and dayside together with the location of the twilight zone as Earth rotates under the ovals. The graphical display serves as a tool to forecast auroral activity based on the predicted value of the Kp index. The forecast is installed as a service at http://kho.unis.no/. The Zhang & Paxton (2008) ovals are wider in latitude than the Starkov (1994a) ovals. The nightside model ovals coincide fairly well in shape for low to normal auroral conditions. The equatorward border of the diffuse aurora is well defined by both methods on the nightside for Kp ≤ 7. The dayside needs further studies in order to conclude.
Key words: 2704: auroral phenomena / 1922: forecasting / 2753: numerical modeling
© Owned by the authors, Published by EDP Sciences 2011
This is an Open Access article distributed under the terms of creative Commons AttributionNoncommercial License 3.0
1. Introduction
On Earth the impact zones of energetic particles from the Sun, i.e. a circular belt of auroral emissions around each geomagnetic pole, are known as the auroral ovals (cf. Akasofu 1964). The location and size of these ovals have been studied extensively in the second half of the 20th century.
During the International Geophysical Year (1957–1958), auroral occurrence was determined from allsky camera studies for a wide variety of activity levels. The resulting figure was made up from a statistical study showing the poleward and equatorward auroral boundaries of the 75% occurrence probability (Feldstein 1963, 1973; Feldstein & Starkov 1970). The relationship between the morphology of the auroral oval and the level of geomagnetic activity allows us to develop models of the location of the aurora, independent of the vagaries of auroral observations (Holzworth & Meng 1975; Starkov 1994a).
Over the last three decades, new models have evolved that use data of particle precipitation measured by polar orbiting satellites (Gussenhoven et al. 1983; Hardy & Gussenhoven 1985; Hardy et al. 1987, 1989). Recently, Zhang & Paxton (2008) developed an auroral oval model based on data from the Ultraviolet Imager (GUVI) on board the TIMED (Thermosphere Ionosphere Mesosphere Energetics and Dynamics) satellite.
The planetary geomagnetic activity index Kp (Bartels et al. 1939) is directly related to the size and location of the auroral oval, and it is used as an input parameter to the above models. The Kp index is provided by the Helmholtz Centre in Potsdam, and it involves worldwide data collection and careful interpretation in line with a tradition that began in 1936. The traditional Kp index is not reported in real time. It is therefore not useful for forecasting purposes. However, an intermediate method of scaling the Kp from a small number of midlatitude stations has been developed by the US Air Force 55th Space Weather Squadron. This alternative Kp index is referred to as the estimated Kp index (Takahashi et al. 2001), and it will be used in the present work.
The advent of stationary spacecraft between the Sun and the Earth has led to studies of the relationship between the structure of the solar wind and the resulting auroral and geomagnetic disturbances. When the input data come from a satellite located approximately 1 h upstream in the solar wind, the resultant predicted Kp forecast is relatively short term (Costello 1997; Wing et al. 2005). It gives a 1 or 4h warning. This can be very useful both for auroral observers and experiments that are dependent on the location and intensity of the aurora.
In this study we will compare the models of Starkov (1994a) and Zhang & Paxton (2008). Our goal is to produce a realtime forecast, up to 1 h in advance, for the location and size of the aurora oval and mapped onto the Earth’s surface. Solar elevation and cloud cover are the main obstacles for an auroral observer at the ground level. Therefore, this forecast also includes the observing conditions for a particular site. To our knowledge, no such combined display of information currently exists.
2. Two models of the auroral oval
This section describes the auroral oval models of Starkov (1994a) and Zhang & Paxton (2008). Both models are presented using the same mathematical notation.
2.1. The FeldsteinStarkov ovals
Starkov (1994a) compiled simple formulas of the poleward, equatorward and diffuse auroral boundaries as a function of magnetic activity.
The magnetic input parameter is the AL index. This index describes the polar or planetary magnetic disturbances that occur during auroras. The range of the index is of the order of ± 800 nT. In terms of Kp index it is given as (Starkov 1994b)(1)
The coefficients c _{ i } for i ∈ [0, …, 3] are given in Table 1.
Coefficients to convert Kp to AL indices by Starkov (1994b) used by equation (1) in units of nT.
The value of the Kp index varies from 0 to 9 with 0 being very quiet and 5 or more indicating geomagnetic storm conditions. In detail, Kp represents a 3h weighted average from a global network of magnetometers measuring the maximum deviation in the horizontal component of the Earth’s magnetic field.
In coordinates of corrected geomagnetic colatitude, θ, the boundaries of the oval are expressed as(2)where A _{ im } and α _{ im } for i ∈ [0, …, 3] are amplitudes in units of degrees of latitude and phases in units of decimal hours, respectively. t is local time. Equation (2) is valid for the poleward (m = 0), the equatorward (m = 1) and the diffuse aurora boundaries (m = 2). The challenge now is to find the coefficients of equation (2).
Starkov (1994a) does this using a new thirdorder polynomial for both the A _{ im } and α _{ im } coefficients(3)
In other words, for each coefficient A _{ im } or α _{ im } there is a set of b _{ im } values, i ∈ [0, …, 3], for each boundary with index m. Appendix A lists all the values.
Starting with the Kp index, equation (1) is used to obtain the AL index. Next, Appendix A is used to obtain the correct set of b _{ im } values to calculate the A _{ im } or α _{ im } coefficients by equation (3). Finally, the auroral boundaries are obtained using equation (2). Note that the procedure works for Kp indices that are floating point numbers. The ovals are expanding smoothly as the Kp index increases.
2.2. The ZhangPaxton ovals
This model uses Epstein functions to calculate either the electron flux or the mean energy flux for precipitating electrons based on data from the GUVI on board the TIMED satellite. The electron energy flux [ergs cm^{−2}·s^{−1}] is given as(4)where x = π/2 − θ is the comagnetic latitude. The index m ∈ [0, …, 5] refers to six subintervals of Kp index with center values k _{ m } = [0.75, 2.25, 3.75, 5.25, 7.00, 9.00]. The coefficients for i ∈ [0, …, 3] are calculated by a Fourier series(5) and for n ∈ [0, …, 6] are listed in Appendix B.
The electron flux, Q, at any Kp index, can then be found using a nonlinear interpolation(6)where the subscripts m and m + 1 refer to the closest subintervals that satisfy the conditions(7)
Note that if Kp is less than 0.75 then k _{0} = 0.75 and k _{1} = 2.25. Furthermore, the scale factors f _{ m } and f _{ m+1} in equation (6) are calculated as(8)and(9)
The function HP is the auroral hemispheric power as a function of Kp index in units of gigawatts(10)
In order to use the model it is necessary to scale the output. For each model run, the maximum value of the electron energy flux is stored. The net result is a polynomial fit that gives the maximum flux as a function of Kp index(11)
The coefficients for i ∈ [0 … 4] are given in Table 2.
3. Geographical transform
The ovals calculated in the previous section are centered on the magnetic poles (dipole). The Cartesian components in the graph are related to the polar magnetic coordinates by(12)where θ and ɸ are the magnetic latitude and longitude, respectively. In local magnetic time it becomes(13)where ∆ɸ(t) is the longitudinal difference between the subsolar point and the magnetic poles at time t (hours). It is important in order to make sure that the ovals are oriented correctly with magnetic noon pointing toward the Sun as Earth rotates around its own axis.
The transformation to geographic coordinates is then(14)where is a rotational matrix. The invariant magnetic north pole is located in geographic coordinates at latitude and longitude .
The elements of the rotational matrix are then simply(15)where is the latitudinal difference between the geographic and the north magnetic pole.
Finally, the geographic latitude and longitude of the ovals are given as(16)
Note that the procedure is identical for the south magnetic pole if we assume that the ovals are mirrored.
4. Visualization
The ovals are visualized with a standalone 32bit executable Windows program called SvalTrack II. The program is written in Borland’s DelphiPascal and uses a Geographic Information System unit that displays interactively mapped data in real time onto a threedimensional spherical Globe representing the Earth. The twilight zone, night and dayside of the Earth are projected with grades of shade on the Globe as a function of time. The 3D globe can be rotated and zoomed to display a closeup of any region of the Earth.
The FeldsteinStarkov ovals are projected as semitransparent polygons onto the globe with an angular resolution of 1.5°. The equatorward boundary of the diffuse aurora is added as a polygonal line. The ZhangPaxton ovals are mapped onto the globe with transparent scaled intensities according to electron energy flux. Every pixel of the display is processed in real time to determine electron energy flux values or which colors to draw onto the surface of the globe.
The local observational position is added as a point (red triangle) with corresponding state information of the Moon and the Sun. In addition, the circle of ~ 10° around the observer represents a 180° field of sky view. The latter is under the assumption that the auroral emissions peak at an altitude of ~ 110 km.
All the above features are shown in Figure 1. A textured map is used to visualize the Earth on 24th December 2009. The twilight zone crosses most of Norway, and North America is on the nightside. The observer is located in Longyearbyen (78.2^{o}N, 16.0^{o}E), on the archipelago Svalbard, Norway. The Kp = 3 oval is typically broader on the night vs. the dayside, with magnetic noon or cusp located over the site at ~ 08:50 UT. The Moon is below the horizon, indicating favorable conditions to view the aurora. Also note that the island of Svalbard is uniquely located. It is possible to view both the day and nightside aurora from this location midwinter.
Fig. 1. SvalTrackII screen dumps: Panels (A) and (B) show the ovals by Starkov (1994a) and Zhang & Paxton (2008), respectively. (1) Equatorward boundary of the diffuse aurora, (2) FeldsteinStarkov aurora oval, (3) field of view aurora observer, (4) is ZhangPaxton oval, (5) observer location, (6) Moon and Sun information at local site. Time: 08:50 UT on 24th December 2009. The Kp index equals 3. 
The only inputs to the above visualizations are time and the Kp index. The program is set to update itself in real time based on the predicted Kp index provided by the Space Weather Prediction Centre at the National Oceanic and Atmospheric Administration (NOAA).
The index is predicted every 15 min by the use of the Wing Kp Predicted Activity Index model (Wing et al. 2005), which takes into account the most recent estimated Kp values and the response of solar wind parameters (neural network algorithm).
The result is a realtime auroral oval forecast up to approximately 1 or 4 h in advance. The software is installed to run automatically at the Kjell Henriksen Observatory (KHO) on Svalbard, Norway. See link: http://kho.unis.no/.
5. Model comparision
Figure 2 shows the results from the two models plotted on top of each other for different Kp indices. As expected, both models show ovals that are wider and more asymmetric with increasing Kp index. The ZhangPaxton ovals have a larger latitudinal spread than the FeldsteinStarkov ovals, but they are close and within the equatorward boundary of the diffuse aurora of Starkov (1994a) on the nightside, except for severe and extreme auroral storm conditions. The spread in latitude is seen as a diffuse effect on the ovals of Figure 2. The main difference between the model oval shapes is for storm conditions, where the FeldsteinStarkov dusk side of the ovals is poleward of the ZhangPaxton ovals.
Fig. 2. Animated model aurora ovals as a function of Kp index for 24th December 2009 at 08:50 UT. The transparent polygons represent FeldsteinStarkov ovals (A). The faint white outer ring is the equatorward boundary of the diffuse aurora (C). The ZhangPaxton ovals are displayed on top with green intensity values scaled according to the electron energy flux (B). The yellow scaled intensity areas are the intersection (A ∩ B) between the two models. 
In order to quantify the difference, we define the intersection between the modeled ovals as the percentage fraction of the ZhangPaxton points that are inside the FeldsteinStarkov ovals (polygons). The yellow glow of Figure 2 represents the intersection. Table 3 lists the results. Note that the overall intersection percentage is quite low (A ∩ B < 36%). This is due to the diffuse effect mentioned earlier. The ZhangPaxton ovals are based on data from spaceborne ultraviolet cameras. These cameras see radiation that is not detected by groundbased instruments. This is due to the ultraviolet absorption in the middle atmosphere. Diffuse aurora equatorward of the discrete/visible aurora, caused by high energy particles that are lost from the ring current/radiation belts, may be more visible from space than from the ground.
Auroral intersection (A ∩ B) between the ZhangPaxton (A) and the FeldsteinStarkov (B) ovals as a function of Kp index. (A ∩ C) is the interception between (A) and the equatorward boundary of diffuse aurora from Starkov (1994a) (C). Q _{max} is the maximum electron flux. Q _{min} = 0.25 ergs cm^{−2}·s^{−1}.
On the other hand, the intersection A ∩ C > 80% for Kp ≤ 7. The diffuse equatorward border of Starkov (1994a) is close to the Zhang & Paxton (2008) equatorward oval border on the nightside. On the dayside the situation is opposite. The Starkov (1994a) diffuse border is clearly equatorward of the Zhang & Paxton (2008) equatorward oval border. We suspect that the lack or quality of the data from the dayside region both from space or ground may be the reason for the difference. On the dayside, the oval is contaminated by ultraviolet radiation from the Sun, and from the ground there are fewer observations compared to the nightside.
Note that this study uses the same threshold electron flux as Zhang & Paxton (2008), Q _{min} = 0.25 ergs cm^{−2}·s^{−1}. Raising the threshold value will cut low flux contributions both poleward and equatorward of the ovals. The intersection of the ovals will then increase correspondingly. If we set the threshold too high, then the intersection also becomes too high. An intersection that equals 100% may only plot high flux values inside a small portion of the FeldsteinStarkov ovals. The relation between the threshold as a function of Kp index and what is detectable from ground is an aim for future studies.
6. Concluding remarks
The two methods by Starkov (1994a) and Zhang & Paxton (2008) are used to mathematically calculate the size and location of the auroral oval mapped onto a solar illuminated Earth globe. Both models only use Kp index and time as input, which makes them ideal candidates for forecasting aurora when the predicted Kp value is estimated from satellite data 1 hour upstream in the solar wind. The forecast is found at http://kho.unis.no/. As expected the ZhangPaxton ovals deduced by spaceborne data are wider than the groundbased FeldsteinStarkov ovals. In spite of difference in methods and platforms, the model ovals coincide fairly well in shape for low to normal conditions on the nightside. In addition, the equatorward border of the diffuse aurora is well defined by both methods on the nightside for Kp ≤ 7. On the dayside, there is a need to study further oval shapes for all levels of auroral activity, especially the equatorward border of the diffuse aurora.
Acknowledgments
We wish to thank the National Oceanic and Atmospheric Administration – Space Weather Prediction Centre for allowing us to download the predicted value of the estimated Kp index every 15 min. The work is financially supported by The Research Council of Norway through the project named: Norwegian and Russian Upper Atmosphere Cooperation On Svalbard part 2 # 196173/S30 (NORUSCA2), the Nordic Council of Ministers: Arctic Cooperation Programme # A10162, and COST action ES0803.
Appendix A
Expansion coefficients for auroral boundaries by Starkov (1994a) used in equation (3).
Units  [^{o}]  [^{o}]  [^{o}]  [^{o}]  [h]  [h]  [h] 

align="center">A _{00}  A _{10}  A _{20}  A _{30}  α _{10}  α _{20}  α _{30}  
m = 0 Poleward boundary of the auroral oval  
b _{00}  −0.07  −10.06  −4.44  −3.77  −6.61  6.37  −4.48 
b _{10}  24.54  19.83  7.47  7.90  10.17  −1.10  10.16 
b _{20}  −12.53  −9.33  −3.01  −4.73  −5.80  0.34  −5.87 
b _{30}  2.15  1.24  0.25  0.91  1.19  −0.38  0.98 
A _{01}  A _{11}  A _{21}  A _{31}  α _{11}  α _{21}  α _{31}  
m = 1 Equatorward boundary of the auroral oval  
b _{01}  1.61  −9.59  −12.07  −6.56  −2.22  −23.98  −20.07 
b _{11}  23.21  17.78  17.49  11.44  1.50  42.79  36.67 
b _{21}  −10.97  −7.20  −7.96  −6.73  −0.58  −26.96  −24.20 
b _{31}  2.03  0.96  1.15  1.31  0.08  5.56  5.11 
A _{02}  A _{12}  A _{22}  A _{32}  α _{12}  α _{22}  α _{32}  
m = 2 Equatorward boundary of the diffuse aurora  
b _{02}  3.44  −2.41  −0.74  −2.12  −1.68  8.69  8.61 
b _{12}  29.77  7.89  3.94  3.24  −2.48  −20.73  −5.34 
b _{22}  −16.38  −4.32  −3.09  −1.67  1.58  13.03  −1.36 
b _{32}  3.35  0.87  0.72  0.31  −0.28  −2.14  0.76 
Appendix B
EpsteinFourier coefficients by Zhang & Paxton (2008) used in equation (5).
Units  [ergs cm^{2}·s^{−1}]  [^{o}]  [^{o}]  [^{o}] 

m = 0 (Kp: 0.0–1.5) k _{0} = 0.75  
3.2402978  18.221647  2.8442195  1.8336810  
1.3291109  6.0779378  0.2931214  −0.3873319  
0.4209809  −1.3235271  −0.5383766  0.0094550  
0.4779546  0.2553541  0.2728634  0.0548413  
−0.3673774  0.0980007  0.2950094  −0.0113930  
0.0557991  0.0075817  −0.0456968  −0.0434681  
−0.0556684  −0.0050137  0.0073026  0.0562728  
−0.1914775  1.3812608  0.8133630  0.1214365  
0.0802700  −0.0211661  −0.3734801  −0.2901524  
−0.4206442  −0.1240047  −0.0874247  0.2791531  
−0.0354484  0.3415960  −0.0607254  −0.1764180  
−0.2017480  −0.1074103  0.1679693  0.0400522  
−0.0298214  0.2863931  −0.0456554  −0.1214534  
m = 1 (Kp: 1.5–3.0) k _{1} = 2.25  
6.3011691  19.882410  2.9663179  1.8560835  
3.2522103  6.5577617  0.8165399  −0.3102606  
−0.2114976  −1.5086115  −0.3559603  0.0363061  
0.3216365  0.5457940  0.3101074  0.0574751  
−0.3236900  −0.0926016  0.0969373  −0.0304515  
0.1705425  −0.0363445  −0.0530104  0.0657831  
0.0919870  −0.0801630  −0.0685254  0.0046886  
−0.6934043  1.6156140  0.7957589  −0.0660346  
−0.1779372  −0.0385058  −0.4427029  −0.3614867  
−0.3675894  −0.1844160  −0.1514768  0.1820734  
−0.0095432  0.2427321  0.0079244  −0.1546944  
−0.2508516  −0.1503851  0.1311359  0.0449006  
−0.0501051  0.1889811  −0.0278058  −0.0735363  
m = 2 (Kp: 3.0–4.5) k _{2} = 3.75  
9.5988037  21.479304  3.1926672  1.9755171  
5.1430543  6.6075450  1.2270596  −0.3518031  
−1.7371661  −1.2566572  −0.0054540  −0.0143734  
−0.2230598  0.3451542  0.1229414  −0.0291659  
0.0422935  −0.0564700  0.0573293  −0.0337693  
−0.0122696  −0.1576626  −0.0562889  0.0388444  
0.0080510  0.2253359  0.0956040  0.0575712  
−0.6726416  1.2164832  0.4361579  −0.1477385  
−0.0727642  −0.2300587  −0.5028849  −0.2390160  
0.1200389  −0.3520732  −0.2906078  0.1048181  
0.0465696  0.2226716  0.0514080  −0.1010366  
−0.4557674  −0.0385575  0.0760109  −0.0255308  
−0.1550104  0.1310600  0.0308203  −0.0628866  
m = 3 (Kp: 4.5–6.0) k _{3} = 5.25  
12.246801  23.511121  3.7091436  2.1764069  
7.0481969  6.1681312  1.3842879  −0.4713056  
−3.0928509  −0.7124293  0.1899543  −0.0948302  
−1.2935699  0.2640897  0.0647574  −0.1372124  
0.0884275  −0.2602568  −0.0045988  −0.0509513  
−0.0274394  0.0211500  0.0295777  0.0340843  
−0.2723690  0.2260950  0.1237925  −0.0056936  
−1.0729358  1.0434480  0.4866616  −0.2832799  
0.1829594  −0.3088645  −0.4396647  −0.0853116  
0.6604424  −0.6493409  −0.3368631  0.0876408  
0.1005881  0.3886247  0.2038886  0.0708100  
−0.3857214  −0.0406112  0.0022551  −0.0345108  
−0.3237388  −0.0072146  0.0360084  −0.0328183  
m = 4 (Kp: 6.0–8.0) k _{4} = 7.0  
17.185531  27.197799  5.1669995  2.5417068  
11.323595  5.3379375  1.1495666  −0.6063337  
−1.2885997  −1.1071272  0.0676676  0.0136708  
−0.8853908  0.3888829  −0.1339100  −0.0624044  
1.2169522  −0.4494379  −0.0978956  0.0024086  
0.9936972  −0.2346430  −0.2247035  0.0623906  
0.3355213  0.3541175  0.0702655  0.0125311  
−1.8969096  −0.7900455  0.0107553  −0.3075880  
−1.5002061  0.5940236  0.2318213  0.0774584  
−0.4722835  −0.7037725  −0.1692764  −0.1040405  
−1.8746630  0.4504852  0.5258857  −0.0402230  
−0.8323257  0.2860252  0.1850265  −0.0989170  
0.1062067  −0.4846608  −0.2689677  0.0636382  
m = 5 (Kp: 8.0–10.) k _{5} = 9.0  
33.435440  30.688625  5.9308809  4.1004123  
24.269584  3.9275374  0.3238901  −0.4237273  
−4.0539849  −2.4440639  −0.9602533  −0.1556447  
−5.0305214  1.8123949  0.2338884  0.2188714  
−1.7500538  −0.2253542  0.4168486  −0.0093918  
−0.8196342  0.4044060  −0.1198387  −0.0095218  
−0.7520601  −1.2894243  −0.5288058  0.0896570  
−5.9059449  −2.6264976  0.8511741  −0.6852183  
−0.1670781  3.0068989  0.9358651  −0.0488459  
2.8623939  −2.5030701  −1.2186771  0.3298003  
0.9153974  0.7056867  0.1745191  0.1314771  
1.5992821  −0.1550183  −0.3299605  −0.1826762  
0.9162504  −0.7857376  −0.2456667  0.2985601 
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All Tables
Coefficients to convert Kp to AL indices by Starkov (1994b) used by equation (1) in units of nT.
Auroral intersection (A ∩ B) between the ZhangPaxton (A) and the FeldsteinStarkov (B) ovals as a function of Kp index. (A ∩ C) is the interception between (A) and the equatorward boundary of diffuse aurora from Starkov (1994a) (C). Q _{max} is the maximum electron flux. Q _{min} = 0.25 ergs cm^{−2}·s^{−1}.
All Figures
Fig. 1. SvalTrackII screen dumps: Panels (A) and (B) show the ovals by Starkov (1994a) and Zhang & Paxton (2008), respectively. (1) Equatorward boundary of the diffuse aurora, (2) FeldsteinStarkov aurora oval, (3) field of view aurora observer, (4) is ZhangPaxton oval, (5) observer location, (6) Moon and Sun information at local site. Time: 08:50 UT on 24th December 2009. The Kp index equals 3. 

In the text 
Fig. 2. Animated model aurora ovals as a function of Kp index for 24th December 2009 at 08:50 UT. The transparent polygons represent FeldsteinStarkov ovals (A). The faint white outer ring is the equatorward boundary of the diffuse aurora (C). The ZhangPaxton ovals are displayed on top with green intensity values scaled according to the electron energy flux (B). The yellow scaled intensity areas are the intersection (A ∩ B) between the two models. 

In the text 
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