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Stations of the fireball network located in Czech Republic, Slovakia and Austria where DAFO are placed (status November 2015)
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Taurid meteor shower produces prolonged but usually low activity every October and November. In some years, however, the activity is significantly enhanced. Previous studies based on long-term activity statistics concluded that the enhancement is caused by a swarm of meteoroids locked in 7:2 resonance with Jupiter. Here we present precise data on 1...
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... first DAFO was installed at the observatory of the Slovak Academy of Sciences in Tatranská Lomnica, where one AFO also remains in full operation, and the second, installed at the Waldviertel Observatory in Martinsberg (Austria), substituted the previous AFO system in September 2015. This core of the EN as schematically shown in Figure 1 also cooperates with other parts and systems located in neighboring European countries but data used in this study are solely acquired by the stations based on the DAFO (vast majority of used records) and AFO cameras as described above. ...
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... data from the new digital system allow us to reliably determine all basic parameters of sufficiently bright fireballs up to the distance of 300 km from the stations (for special cases even up to 600 km). It means that with the current number and displacement of stations (see Figure 1) we effectively cover territory of roughly 3 million square kilometers at least, i.e., a large part of Central Europe. All the advantages mentioned above significantly increased the efficiency of our observations; and in direct comparison with the efficiency of the previous analog AFO system the number of recorded fireballs increased at least three times. ...
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... took into account the curvature of the trajectory of the bolide due to gravity, which was significant for such a long and low inclined fireball (change of direction of flight by 0.18 • over the recorded length). A detailed view of its luminous flight taken by the DAFO at Kunžak station is shown in Figure 10. Additional information about this fireball is given in Tables 4 and 5. ...
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... elements in this paper are given for equinox J2000.0. The data are presented in Table 4. Figure 11 shows the dependency of geocentric radiant and velocity on solar longitude (i.e., the longitude of the Sun at the time of fireball observation). Thirteen fireballs were classified as Northern Taurids. ...
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... of perihelion, inclination, eccentricity, and perihelion distance as a function of solar longitude are plotted in Fig. 12. Most notably, there is a concentration of orbits with longitude of perihelion, π (π = Ω + ω, where Ω is longitude of ascending node and ω is argument of perihelion), at 158 • ± 2 • (Fig. 12a). There is only a weak correlation with solar longitude. Similarly, there is a concentration of orbits with inclinations of 5.5 • ± 1 • (Fig. ...
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... of perihelion, inclination, eccentricity, and perihelion distance as a function of solar longitude are plotted in Fig. 12. Most notably, there is a concentration of orbits with longitude of perihelion, π (π = Ω + ω, where Ω is longitude of ascending node and ω is argument of perihelion), at 158 • ± 2 • (Fig. 12a). There is only a weak correlation with solar longitude. Similarly, there is a concentration of orbits with inclinations of 5.5 • ± 1 • (Fig. 12b). Regular Taurids show much larger spread, 145 -175 • in π and 2 -7 • in ...
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... plotted in Fig. 12. Most notably, there is a concentration of orbits with longitude of perihelion, π (π = Ω + ω, where Ω is longitude of ascending node and ω is argument of perihelion), at 158 • ± 2 • (Fig. 12a). There is only a weak correlation with solar longitude. Similarly, there is a concentration of orbits with inclinations of 5.5 • ± 1 • (Fig. 12b). Regular Taurids show much larger spread, 145 -175 • in π and 2 -7 • in ...
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... and perihelion distances of the members of the new branch are steep functions of solar longitude (Figs. 12c,d), ...
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... new branch is best recognized in the plot of longitude of perihelion, π, versus latitude of perihelion, β (sin β = sin ω sin i, where i is inclination), presented in Fig. 13. We can state that the new branch has π between 155.9 -160 • and β between 4.2 -5.7 • . For regular Southern Taurids the observed spread in β is 2.5 -6.5 • . Northern Taurids have negative ...
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... axes are plotted in Fig. 14. For regular Taurids, they lie between 1.9 and 2.4 AU. According to the model of ...
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... the contrary, some Southern Taurids with perihelia outside the new branch limits were also in the 7:2 resonance. As seen in Fig. 13, all of the Souther Taurids had an orientation of perihelia relatively close to the new branch. Nevertheless, some Northern Taurids were in the 7:2 resonance as well and they were far from the new ...
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... is evident that the new branch represents an orbital structure that is much more compact than regular Taurids. Since the activity of the new branch lasted almost one month, it cannot, however, be a narrow filament. In order to visualize the new branch, we plotted selected orbits covering the whole activity period in Fig. 15. Unlike usual meteoroid streams, where the orbits near perihelion largely overlap, here we see a concentric ring of orbits near perihelion, which is more than 0.2 AU wide. As the Earth moves around the Sun, it encounters first the orbits with smaller perihelia and larger eccentricities. With increasing solar longitude, orbits with ...
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... Taurids in our sample reached maximum absolute magnitude between −2 and −18.6. The photometric masses range from 0.1 gram to 1300 kg, i.e., there is a range of 7 orders of magnitude in mass. The mass distribution is given in Fig. 16, which shows that the new branch has a higher proportion of massive meteoroids. The data in Fig. 16 are biased because brighter meteors could be observed over large distances and under worse conditions than faint meteors, nevertheless, the bias is the same for all branches. The beginning, maximum brightness, and end heights of all ...
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... Taurids in our sample reached maximum absolute magnitude between −2 and −18.6. The photometric masses range from 0.1 gram to 1300 kg, i.e., there is a range of 7 orders of magnitude in mass. The mass distribution is given in Fig. 16, which shows that the new branch has a higher proportion of massive meteoroids. The data in Fig. 16 are biased because brighter meteors could be observed over large distances and under worse conditions than faint meteors, nevertheless, the bias is the same for all branches. The beginning, maximum brightness, and end heights of all studied fireballs are plotted as a function of photometric mass in Fig. 17. These heights are good ...
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... of massive meteoroids. The data in Fig. 16 are biased because brighter meteors could be observed over large distances and under worse conditions than faint meteors, nevertheless, the bias is the same for all branches. The beginning, maximum brightness, and end heights of all studied fireballs are plotted as a function of photometric mass in Fig. 17. These heights are good proxies to meteoroid structure, although they depend to some extent on observational circumstances (e.g., range to the fireball) and on the slope of the trajectory. Beginning heights show no dependence on mass and are generally between 90 and 110 km. For consistency we use only data from digital all-sky cameras ...
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... the asteroids did not impact Earth and their orbits do not intersect Earth's orbit, we used for comparison the solar longitude, as seen from the asteroid at the time when the asteroid is closest to the Earth's orbit. Figure 19 shows the comparison plot for eccentricity. We see that there is nearly random distribution of asteroids with eccentricities smaller than 0.84 in the solar longitudes of interest. ...
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... Spurny_Taurids Fig. 20. Semimajor axis, inclination, perihelion distance, and longitude of perihelion as a function for solar longitude at the closest approach to the Earth's orbit for 2015 Taurid fireballs and asteroids from JPL database. Asteroids, which are likely related to the new Taurid branch are highlighted. The symbols are the same as in Fig. 19. The inclinations of Northern Taurids and asteroids with Ω > 180 • , which encounter the Earth near their descending node in October/November, are plotted as ...
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... i all agree well with this assumption. For 2005 TF50 and 2015 TX24 e and q are also in agreement. The new Taurid branch can be also part of this relation. In fact, the orbital elements of the theoretical Southern Taurid meteors derived from 2004 TG10, as computed by Babadzhanov et al. (2008), fall perfectly among the Taurid branch fireballs in Fig. 12. Only in π there is a difference of 2.5 • . But only the central part of the new branch at λ ∼ 220 • can be explained in this ...
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Citations
... Olech et al. 2017). P. Spurný et al. (2017) and P. Spurny & J. Borovicka (2023) unambiguously reported several Taurid fireball outbursts occurring at the time the Earth's passage through the predicted Taurid swarm. Accurate orbital measurements of millimeter-to meter-sized Taurids showed that they were tightly clustered in a narrow range of semimajor axes and mean anomalies corresponding to the resonant region. ...
... We followed the procedure described in D. L. Clark et al. (2019) to guide the search. In brief, we generated 10,000 synthetic Taurid asteroids based on the high-precision fireball orbits reported by P. Spurný et al. (2017) and forced them inside the semimajor axis range appropriate for the 7:2 resonance zone. We then rotated the mean anomalies of the particles to To allow for brightness estimation for planning purposes, all these asteroids were assumed to have an absolute magnitude H = 24, equivalent to a diameter of 100 m assuming a cometlike geometric albedo of 0.04. ...
... Among the NEAs that might be associated with the Taurid Complex, a handful were serendipitously discovered during close encounters of the Taurid swarm: 2005 TB 15 , 2005 TF Spurný et al. 2017). 2005 UY 6 is the largest object in this sample with a diameter of 2.2 ± 1.1 km (J. ...
The Taurid Complex is a large interplanetary system that contains comet 2P/Encke, several meteoroid streams, and possibly a number of near-Earth asteroids. The size and nature of the system have led to the speculation that it was formed through a large-scale cometary breakup. Numerical investigations have suggested that planetary dynamics can create a resonant region with a large number of objects concentrated in a small segment of the orbit, known as the Taurid swarm, which approaches the Earth in certain years and provides favorable conditions for studying the Taurid Complex. Recent meteor observations confirmed the existence of the swarm for millimeter- to meter-sized objects. Here we present a dedicated telescopic search for potentially hazardous asteroids and other macroscopic objects in the Taurid swarm using the Zwicky Transient Facility survey. We determine from our nondetection that there are no more than 9–14 H ≤ 24 (equivalent to a diameter of D ≳ 100 m) objects in the swarm, suggesting that the Encke–Taurid progenitor was ∼10 km in size. A progenitor of such a size is compatible with the prediction of state-of-the-art solar system dynamical models, which expects ∼0.1 D > 10 km objects on Encke-like orbits at any given time.
... ref.1, where I 0 is the radiative output of a meteor of 0 absolute magnitude light source. Here the value of 1,500 W was used, as others have done63,84,85 . Next, the radiated energy was converted into source energy via the correspondence relation derived by ref. 86 from well-known atmospheric impacts. ...
Models predict that more than half of all impacting meteoroids should be carbonaceous, reflecting the abundance of carbon-rich asteroids in the main belt and near-Earth space. Yet carbonaceous chondrites represent only about 4% of meteorites recovered worldwide. Here we analyse 7,982 meteoroid impacts and 540 potential meteorite falls from 19 global observation networks and demonstrate that intense thermal stress at low perihelion distances coupled with the filtering effect of Earth’s atmosphere explains this mismatch. Meteoroids repeatedly subjected to intense thermal cycling near the Sun fracture and weaken, removing the most friable objects even before atmospheric entry. Our data also show that tidally disrupted meteoroid streams produce especially fragile fragments that rarely survive to the ground. Consequently, compact, higher-strength, thermally cycled bodies dominate the meteorite record. These findings reconcile the predicted carbonaceous flux with its scarcity in collections, underscoring how orbital evolution and atmospheric filtering shape the materials that reach Earth’s surface.
... from [1], where I 0 is the radiative output of a meteor of zero absolute magnitude light source. Here the value of 1500 W was used, as others have done [63,84,85]. Next, the radiated energy was converted into source energy via the correspondence relation derived by Anghel et al. [86] from well-known atmospheric impacts. ...
Models predict that more than half of all impacting meteoroids should be carbonaceous, reflecting the abundance of carbon-rich asteroids in the main belt and near-Earth space. Yet carbonaceous chondrites represent only about 4% of meteorites recovered worldwide. Here we analyse 7,982 meteoroid impacts and 540 potential meteorite falls from 19 global observation networks and demonstrate that intense thermal stress at low perihelion distances coupled with the filtering effect of Earth`s atmosphere explains this mismatch. Meteoroids repeatedly subjected to intense thermal cycling near the Sun fracture and weaken, removing the most friable objects even before atmospheric entry. Our data also show that tidally disrupted meteoroid streams produce especially fragile fragments that rarely survive to the ground. Consequently, compact, higher-strength, thermally cycled bodies dominate the meteorite record. These findings reconcile the predicted carbonaceous flux with its scarcity in collections, underscoring how orbital evolution and atmospheric filtering shape the materials that reach Earth`s surface.
... Asher & Izumi 1998;Olech et al. 2017). Spurný et al. (2017) and Spurny & Borovicka (2023) unambiguously reported several Taurid fireball outbursts occurring at the time the Earth's passage through the predicted Taurid swarm. Accurate orbital measurements of mm-to m-sized Taurids showed that they were tightly clustered in a narrow range of semi-major axes and mean anomalies corresponding to the resonant region. ...
... We followed the procedure described in (Clark et al. 2019) to guide the search. In brief, we generated 10,000 synthetic Taurid asteroids based on the high-precision fireball orbits reported by Spurný et al. (2017) and forced them inside the semimajor axis range appropriate for the 7:2 resonance zone. We then rotated the mean anomalies of the particles to ±40 • to cover the estimated extent of the Taurids swarm (cf. ...
... Among the near-Earth asteroids that might be associated with the Taurid Complex, a handful were serendipitously discovered during close encounters of the Taurid (Spurný et al. 2017). 2005 UY 6 is the largest object in this sample with a diameter of 2.2 ± 1.1 km (Masiero et al. 2017); the other three asteroids are sub-km in diameter. ...
The Taurid Complex is a large interplanetary system that contains comet 2P/Encke, several meteoroid streams, and possibly a number of near-Earth asteroids. The size and nature of the system has led to the speculation that it was formed through a large-scale cometary breakup. Numerical investigations have suggested that planetary dynamics can create a resonant region with a large number of objects concentrated in a small segment of the orbit, known as the Taurid swarm, which approaches the Earth in certain years and provides favorable conditions to study the Taurid Complex. Recent meteor observations confirmed the existence of the swarm for mm- to m-sized objects. Here we present a dedicated telescopic search for potentially hazardous asteroids and other macroscopic objects in the Taurid swarm using the Zwicky Transient Facility survey. We determine from our non-detection that there are no more than 9--14 (equivalent to a diameter of ~m) objects in the swarm, suggesting that the Encke--Taurid progenitor was ~km in size. A progenitor of such a size is compatible with the prediction of state-of-the-art Solar System dynamical models, which expects ~km objects on Encke-like orbits at any given time.
... That is most obvious for shower 628, the s-Taurids, which cause meteor outbursts every 3 years from the Southern Taurid component, with no similar component in the Northern Taurids, likely due to dust trapped in the 7:2 mean motion resonance (Asher and Izumi, 1998;Spurny et al., 2017). The likely parent body is asteroid 2015 TX 24 , which broke from comet 2P/Encke about 5200 years ago (Devillepoix et al., 2019). ...
... The sharp increase in the number of ground-based networks utilizing digital cameras for observing fireballs [1,2,3,4,5] in recent years has resulted in near continuous coverage of almost 2% of the Earth's atmosphere for small impactors. Supplementing these ground-based instruments in fireball detection is the Geostationary Lightning Mapper (GLM) instrument on board the GOES-16 and 17 satellites. ...
... Records from decades of meteor shower observations have not revealed any macroscopic (> cm-sized) lithic material mixed in with fragile HTC or LPC meteoroids. Smaller inclusions have been documented, notably several mm−sized Type I fragments of Leonid fireballs were observed during the 1998 Leonid fireball storm [57,58,59] as have some gram-sized Type I Taurids [1]. However, the Taurids are an unusual stream; they are on the dynamical boundary between JFC and asteroidal orbits, are generally classified as Type II material, can be difficult to separate from the sporadic background, and have an origin likely related to fragmentation rather than gas drag sublimation [60]. ...
... [49]), for which the data set is complete. This mass is also significantly larger than any previously observed refractory inclusions in cometary material; the largest Type I Taurids are an order of magnitude smaller [1]. ...
The Oort cloud is thought to be a reservoir of icy planetesimals and the source of long-period comets (LPCs) implanted from the outer Solar System during the time of giant planet formation. The abundance of rocky ice-free bodies is a key diagnostic of Solar System formation models as it can distinguish between ``massive" and ``depleted" proto-asteroid belt scenarios and thus disentangle competing planet formation models. Here we report a direct observation of a decimeter-sized ( kg) rocky meteoroid on a retrograde LPC orbit (, i = ). During its flight, it fragmented at dynamic pressures similar to fireballs dropping ordinary chondrite meteorites. A numerical ablation model fit produces bulk density and ablation properties also consistent with asteroidal meteoroids. We estimate the flux of rocky objects impacting Earth from the Oort cloud to be to a mass limit of 10 g. This corresponds to an abundance of rocky meteoroids of \% of all objects originating in the Oort cloud and impacting Earth to these masses. Our result gives support to migration-based dynamical models of the formation of the Solar System which predict that significant rocky material is implanted in the Oort cloud, a result not explained by traditional Solar System formation models.
... These differing strengths explain why cometary fireballs break up at heights above 70 km (ref. 1 ), whereas meteorite-dropping fireballs break up typically below 40 km (ref. 49 ). ...
The Oort cloud is thought to be a reservoir of icy planetesimals and the source of long-period comets (LPCs) implanted from the outer Solar System during the time of giant-planet formation. The abundance of rocky ice-free bodies is a key diagnostic of Solar System formation models as it can distinguish between ‘massive’ and ‘depleted’ proto-asteroid-belt scenarios and thus disentangle competing planet formation models. Here we report a direct observation of a decimetre-sized (~2 kg) rocky meteoroid on a retrograde LPC orbit (eccentricity ~1.0, inclination 121°). During its flight, it fragmented at dynamic pressures similar to fireballs dropping ordinary chondrite meteorites. A numerical ablation model fit produces bulk density and ablation properties also consistent with asteroidal meteoroids. We estimate the flux of rocky objects impacting Earth from the Oort cloud to be 1.08−0.95+2.81 meteoroids per 106 km2 yr−1 to a mass limit of 10 g. This corresponds to an abundance of rocky meteoroids of ~6−5+13% of all objects originating in the Oort cloud and impacting Earth to these masses. Our result gives support to migration-based dynamical models of the formation of the Solar System, which predict that significant rocky material is implanted in the Oort cloud, a result not explained by traditional Solar System formation models. Observations of a meteoroid coming from the Oort cloud show that it is made of rocky and not icy material, constraining the ratio of rocky to icy objects impacting Earth from the Oort cloud to 6−5+13%.
... In general, the Taurid stream exhibits high heterogeneity of material strengths and composition, and was speculated to include stronger asteroidal material (Brown et al. 2013;Olech et al. 2016;Spurný et al. 2017). Recent studies have however confirmed that the majority of Taurids have cometary characteristics and are likely produced by comet 2P/Encke (Matlovič et al. 2017;Borovička & Spurný 2020). ...
The hydrogen emission from meteors is assumed to originate mainly from the meteoroid composition, making it a potential tracer of HO molecules and organic compounds. H line was previously detected in individual fireballs, but its variation in a larger meteor dataset and dependency on the dynamical origin and physical properties have not yet been studied. Here we investigate the relative intensity of H within 304 meteor spectra observed by the AMOS network. We demonstrate that H emission is favored in faster meteors ( 30 km s) which form the high-temperature spectral component. H was found to be a characteristic spectral feature of cometary meteoroids with 92\% of all meteoroids with detected H originating from Halley-type and long-period orbits. Our results suggest that hydrogen is being depleted from meteoroids with lower perihelion distances (q 0.4 au). No asteroidal meteoroids with detected H emission were found. However, using spectral data from simulated ablation of different meteorite types, we show that H emission from asteroidal materials can occur, and apparently correlates with their water and organic matter content. Strongest H emission was detected from carbonaceous chondrites (CM and CV) and achondrites (ureilite and aubrite), while it was lacking in most ordinary chondrites. The detection of H in asteroidal meteoroids could be used to identify meteoroids of carbonaceous or achondritic composition. Overall, our results suggest that H emission correlates with the emission of other volatiles (Na and CN) and presents a suitable tracer of water and organic matter in meteoroids.
... In general, the Taurid stream exhibits high heterogeneity of material strengths and composition, and was speculated to include stronger asteroidal material (Brown et al. 2013;Olech et al. 2016;Spurný et al. 2017). Recent studies have however confirmed that the majority of Taurids have cometary characteristics and are likely produced by comet 2P/Encke (Matlovič et al. 2017;Borovička & Spurný 2020). ...
The hydrogen emission from meteors is assumed to originate mainly from the meteoroid composition, making it a potential tracer of H2O molecules and organic compounds. Hα line was previously detected in individual fireballs, but its variation in a larger meteor dataset and dependency on the dynamical origin and physical properties have not yet been studied. Here we investigate the relative intensity of Hα within 304 meteor spectra observed by the AMOS network. We demonstrate that Hα emission is favored in faster meteors (vi > > 30 km s−1) which form the high-temperature spectral component. Hα was found to be a characteristic spectral feature of cometary meteoroids with ∼ 92 per cent of all meteoroids with detected H originating from Halley-type and long-period orbits. Our results suggest that hydrogen is being depleted from meteoroids with lower perihelion distances (q < 0.4 au). No asteroidal meteoroids with detected H emission were found. However, using spectral data from simulated ablation of different meteorite types, we show that H emission from asteroidal materials can occur, and apparently correlates with their water and organic matter content. Strongest H emission was detected from carbonaceous chondrites (CM and CV) and achondrites (ureilite and aubrite), while it was lacking in most ordinary chondrites. The detection of Hα in asteroidal meteoroids could be used to identify meteoroids of carbonaceous or achondritic composition. Overall, our results suggest that Hα emission correlates with the emission of other volatiles (Na and CN) and presents a suitable tracer of water and organic matter in meteoroids.
... All-sky cameras are simple and inexpensive devices, that generally consist of a camera, a fish-eye lens, an electronic system and a waterproof enclosure. These cameras have been proven to be a powerful tool for the continuous acquisition of a visible hemisphere image in a single frame and they have been widely used in astronomical observation around the world (e.g., Trigo-Rodríguez et al. 2004;Walker et al. 2006;Skidmore et al. 2011;Sims et al. 2013;Spurný et al. 2017;Shang et al. 2018). ...
... In the area of site testing, wide-angle imaging can be used for the measurement of cloud coverage and night-sky brightness (e.g., Mandat et al. 2013;Pascual et al. 2017;Hänel et al. 2018), which is a significant problem not only for active observatories but also for the candidate sites of future observatories (Schöck et al. 2009;Thomas-Osip et al. 2010). In the field of meteor astronomy, positional astrometric reduction can be used to calculate the initial orbit of the meteoroid and predict the final fall position, which can improve the efficiency of recovering samples of fresh meteorites (Weryk et al. 2008;Spurný et al. 2017;Devillepoix et al. 2019Devillepoix et al. , 2020Daly et al. 2020). ...
The night images obtained with an all-sky camera can provide spatial and time sampling, which can be used for measurement cloud coverage measurement and meteor monitoring. The astrometric calibration of an all-sky camera is necessary because of strong field distortions. We use machine learning to complete the calibration of an all-sky camera. In order to prepare the data sets needed for machine learning, a particle swarm optimization algorithm is used to determine the parameters of the method proposed by Borovicka in 1995. Machine learning can transform plate coordinates to celestial coordinates and transform celestial coordinates to plate coordinates. The actual test shows that the standard deviation of residuals is of the order of 1′ for the transformation from plate coordinates to celestial coordinates and the standard deviation of residuals is of the order of 0.3 px for the transformation from celestial coordinates to the plate coordinates.
