Video observation of meteors in the CEMeNt and SSOVMO networks in September and October 2025
September sees a temporary decrease in meteor shower activity, especially compared to August when the Perseid meteor shower and also relatively strong meteor showers from the antihelion complex with radiants in Capricorn and Aquarius are active. On the other hand, sporadic background activity reaches its maximum in September and also in October, with sporadic meteor rates up to double those in spring months. In October, the increase in meteor shower activity begins, continuing in November and culminating in the activity of the strongest regular shower of the year, which is the December Geminids. Meteor shower activity in this month is dominated in the second half of the period by the Orionid meteor shower (ORI), while throughout the month the activity continues of the massive complex of showers genetically belonging to comet 2P/Encke and related bodies mostly classified as asteroids. At least one meteor was recorded at some station of the CEMeNt network ( Central European Meteor Network ) on 23 nights in September and on 22 nights in October, with more than half of the nights being favorable with minimum cloudiness, or partially disturbed by high cloudiness, especially around the maximum of the Orionid meteor shower. However, at some lower-elevation stations, the typical phenomenon of autumn and winter months is beginning to appear – the inversion character of weather.
Meteor shower activity
At the beginning of September, the activity of the Aurigid meteor shower (AUR) is fading, whose maximum occurred according to the visual activity graph of IMO VMDB ( International Meteor Organization Visual Meteor Database ) on September 1, 2025 in the morning (2:05 UT) and the maximum corrected hourly rate of Aurigids reached 11.6 ± 1.8 meteors this year. The maximum of the September epsilon Perseid meteor shower (SPE) was not visually monitored, with the highest corrected hourly rate reaching 8.0 ± 2.3 meteors in the evening hours of September 16, 2025 (21:34 UT). The meteor shower is known for its irregular activity, which in some years shows short increases in activity, so-called outbursts (e.g. in 2013). At the end of the month, activity from the complex of comet 2P/Encke began to appear, with orbits of meteors belonging to the nu Piscid (NPS) and Northern (NPI) and Southern delta Piscid (SPI) meteor showers recorded. These showers are followed in October by the activity of the main meteor shower of the 2P/Encke comet complex, which are the Taurids. This meteor shower, known for bright fireballs, is also divided into Northern (NTA) and Southern (STA) branches.
Fig. 1: Composite image of meteors recorded at the Valašské Meziříčí SW station during the nights from October 18/19 to October 24/25, 2025 during the maximum of the Orionid meteor shower. The camera recorded 425 meteors during the specified period over 5 nights. Author: Valašské Meziříčí Observatory.
Fig. 2: Composite image of meteors recorded at the Blahová S station during the nights from October 18/19 to October 24/25, 2025 during the maximum of the Orionid meteor shower. The camera recorded 725 meteors during the specified period over 4 nights. Author: UMa Astronomy (Tibor Csörgei)
At the beginning of October, the maxima of the October Camelopardalid (OCT, maximum October 5) and Draconid (DRA, maximum October 8 at 15 UT) meteor showers occur in quick succession. Both showers are irregular, with the latter having produced meteor storms in the first half of the last century (in 1933 and 1946 with up to thousands of meteors per hour). This year, the activity of the October Camelopardalids was not detectable, in the case of the Draconids 2 multi-station orbits were recorded, and the predicted high activity (up to 500 met/h) was not observed. Another meteor shower also mentioned for visual observation is the Leo Minorids (LMI, maximum October 24), which provided thanks to the CEMeNt network cameras in October 2025 a total of 33 multi-station orbits and were thus the 4th strongest shower in this month. However, the main meteor shower in October is the Orionids (ORI, maximum October 21 with the possibility of secondary maxima), whose parent body is the most famous comet 1P/Halley (as in the case of the May eta Aquarids). The usual corrected hourly rate of the Orionids reaches 20 meteors, the maximum occurred according to the visual activity graph of IMO VMDB ( International Meteor Organization Visual Meteor Database ) on October 22, 2025 in the morning (1:56 UT) and the maximum corrected hourly rate reached 19.0 ± 4.1 meteors this year. However, the CEMeNt network cameras recorded a total of 437 multi-station Orionid orbits, which is the second highest number from meteor showers that were already active this year after the Perseid meteor shower. The activity of the 2P/Encke comet complex goes through its first maximum of activity in October (southern branch), multi-station orbits of complex members were recorded, predominantly with radiants in the constellations Pisces, Aries, and Taurus. These were the Southern Taurids (STA, 223 orbits), Northern Taurids (NTA, 80 orbits), Northern delta Piscids (NPI, 39 orbits), Southern delta Piscids (SPI, 17 orbits), and nu Piscids (NPS, 17 orbits).
Fig. 3: Overall 2D projection of multi-station atmospheric orbits recorded in the CEMeNt network in September and October 2025. Authors: Jakub Koukal, Alexandra Mikušková
Fig. 4: Radiants of shower and sporadic multi-station meteors recorded in the CEMeNt network in September and October 2025. A sinusoidal projection with an equatorial coordinate system is used for display. Authors: Jakub Koukal, Alexandra Mikušková
Overview of video observations in the CEMeNt and SSOVMO networks
In September 2025, cameras of the CEMeNt ( Central European Meteor Network ) and SSO VMO ( Southern Spectroscopic Observatory of the Valašské Meziříčí Observatory ) networks recorded 34,756 single-station meteors, the combination of which resulted in 6,508 multi-station orbits. The CEMeNt network cameras recorded 19,749 single-station meteors, the combination of which resulted in 4,139 multi-station orbits (Figs. 3 and 4), while the SSO VMO network cameras recorded 15,007 single-station meteors, the combination of which resulted in 2,369 multi-station orbits (Figs. 5-8). To date, observations from stations on the outer perimeter of the network are not included in the processing, namely from Rokycany (CZ), Plzeň (CZ), and Karlovy Vary (CZ), whose processing is not complete.
Fig. 5: Overall 2D projection of multi-station atmospheric orbits recorded in the SSO VMO network (UFO Capture stations) in September and October 2025. Authors: Jakub Koukal, Alexandra Mikušková
Fig. 6: Overall 2D projection of multi-station atmospheric orbits recorded in the SSO VMO network (RMS stations) in September and October 2025. Authors: Jakub Koukal, Alexandra Mikušková
Fig. 7: Radiants of shower and sporadic multi-station meteors recorded in the SSO VMO network (UFO Capture stations) in September and October 2025. A sinusoidal projection with an equatorial coordinate system is used for display. Authors: Jakub Koukal, Alexandra Mikušková
Fig. 8: Radiants of shower and sporadic multi-station meteors recorded in the SSO VMO network (RMS stations) in September and October 2025. A sinusoidal projection with an equatorial coordinate system is used for display. Authors: Jakub Koukal, Alexandra Mikušková
In October 2025, cameras of the CEMeNt ( Central European Meteor Network ) and SSO VMO ( Southern Spectroscopic Observatory of the Valašské Meziříčí Observatory ) networks recorded 36,950 single-station meteors, the combination of which resulted in 5,969 multi-station orbits. The CEMeNt network cameras recorded 22,065 single-station meteors, the combination of which resulted in 4,252 multi-station orbits (Figs. 3 and 4), while the SSO VMO network cameras recorded 14,885 single-station meteors, the combination of which resulted in 1,717 multi-station orbits (Figs. 5-8). To date, observations from stations on the outer perimeter of the network are not included in the processing, namely from Rokycany (CZ), Plzeň (CZ), and Karlovy Vary (CZ), whose processing is not complete.
Fig. 9: 3D projection of heliocentric multi-station orbits of meteors belonging to the Orionid meteor shower (ORI) in the Solar System. A total of 437 multi-station orbits of the ORI meteor shower were recorded in September and October 2025 within the CEMeNt network. Authors: Jakub Koukal, Alexandra Mikušková
Fig. 10: 3D projection of heliocentric multi-station orbits of meteors belonging to the Southern Taurids meteor shower (STA) in the Solar System. A total of 223 multi-station orbits of the STA meteor shower were recorded in September and October 2025 within the CEMeNt network. Authors: Jakub Koukal, Alexandra Mikušková
Most multi-station orbits within the CEMeNt network belong to the sporadic background (7,010 orbits), followed by the Orionid meteor shower (ORI, 437 orbits, Fig. 9), Southern Taurids (STA, 223 orbits, Fig. 10), Northern Taurids (NTA, 80 orbits), September epsilon Perseids (SPE, 54 orbits), Northern delta Piscids (NPI, 39 orbits), Leo Minorids (LMI, 33 orbits), and then other weaker meteor showers follow, including members of the antihelion source with radiants in Pisces and Aries. The number of single-station meteors (as well as multi-station orbits) in September and October is historically the highest ever within the CEMeNt network throughout its entire existence since 2009. Pairing efficiency in September 2025 decreased to 66.9%, which is related to the inversion character of weather at lower-elevation network stations. The station/orbit ratio oscillates around the average value during 2025 and is 3.19 stations per orbit in September, respectively 3.13 stations per orbit in October. In total, so far this year (as of October 31, 2025), 145,292 single-station meteors have been recorded, the combination of which resulted in 29,982 multi-station orbits (Tab. 1).
Fig. 11: 3D projection of heliocentric multi-station orbits of meteors belonging to the Southern Taurids meteor shower (STA) in the Solar System. A total of 103 multi-station orbits of the STA meteor shower were recorded in September and October 2025 within the SSO VMO network. Authors: Jakub Koukal, Alexandra Mikušková
Fig. 12: 3D projection of heliocentric multi-station orbits of meteors belonging to the A Carinid meteor shower (CRN) in the Solar System. A total of 16 multi-station orbits of the CRN meteor shower were recorded in September and October 2025 within the SSO VMO network. Authors: Jakub Koukal, Alexandra Mikušková
Most multi-station orbits within the SSO VMO network belong to the sporadic background (3,490 orbits), followed by the Orionid meteor shower (ORI, 116 orbits), Southern Taurids (STA, 103 orbits, Fig. 11), Northern delta Piscids (NPI, 39 orbits), Northern Taurids (NTA, 33 orbits), Southern delta Piscids (SPI, 23 orbits), A Carinids (16 orbits, Fig. 12), and then other weaker meteor showers follow. The number of single-station meteors (as well as multi-station orbits) is the lowest in September and October within the SSO VMO network throughout its entire existence since June 2025, with July being comparable to June. Pairing efficiency decreased to 38.5% in September and 29.0% in October. The station/orbit ratio increased to 2.44 stations per orbit in September, respectively to 2.51 in October 2025. In total, so far this year (as of October 31, 2025), 92,180 single-station meteors have been recorded, the combination of which resulted in 14,364 multi-station orbits (Tab. 1).
Tab. 1: Overview of the number of recorded and paired meteors in 2025 at stations of the CEMeNt and SSOVMO networks. Authors: Jakub Koukal, Alexandra Mikušková
Meteor spectra
At the Valašské Meziříčí Observatory, within the CEMeNt network, 3 spectrographs with monochromatic CMOS cameras PointGrey Grasshopper3 GS3-U3-32S4M-C (2048 × 1536 px) are currently installed. The actual resolution of the recorded meteor spectrum (1st order spectrum) averages 0.48 nm/px. These spectrographs are oriented in the SE, SW, and NE directions. In the NW direction, a spectrograph with a monochromatic CMOS camera QHY-III 178M (3072 × 2048 px) is installed. The actual resolution of the recorded meteor spectrum (1st order spectrum) for the QHY-III 178M spectrograph averages 0.35 nm/px. As part of test operations, a spectrograph is installed in the NEN direction, which consists of a monochromatic CMOS camera Flir BFS-U3-200S6M-C (5472 × 3648 px). The actual resolution of the recorded meteor spectrum (1st order spectrum) averages 0.19 nm/px. In September and October, 7 spectra from 6 individual fireballs were recorded by spectrographs at the Valašské Meziříčí Observatory (Tab. 2).
Fig. 13: Composite image of the spectrum of fireball CM20250930_065808 SPO from the La Silla SPNE spectrograph (resolution 0.35 nm/px). Author: Valašské Meziříčí Observatory.
Fig. 14: Composite image of the spectrum of fireball CM20250930_065808 SPO from the La Silla SPSE spectrograph (resolution 0.34 nm/px). Author: Valašské Meziříčí Observatory.
At the La Silla Observatory, within the SSO VMO network, 4 spectrographs with monochromatic CMOS cameras QHY5III 678M with a resolution of 3856 × 2180 px (8.4 MPx) are currently installed. The actual resolution of the recorded meteor spectrum (1st order spectrum) averages 0.35 nm/px. These spectrographs are oriented in the SE, SW, NE, and NW directions. In September and October, 9 spectra from 6 individual fireballs were recorded by spectrographs at the Southern Spectroscopic Observatory (Tab. 2).
Fig. 15: Composite image of fireball CM20250930_065808 SPO from the El Sauce N overview camera. Author: Valašské Meziříčí Observatory.
Fig. 16: Composite image of fireball CM20250930_065808 SPO from the La Silla SE overview camera. Author: Valašské Meziříčí Observatory.
Detection of meteor spectra within both networks is performed using the FireCapture program into sequences of 3 minutes in length. The resulting sequence is divided into individual frames, each frame is then corrected for dark frame and flat field, in the case of dark frames using frames preceding the spectrum recording. Calibration of the spectrum in the x-axis is performed using a 4th order polynomial using known emission lines that occur in meteor spectra and with regard to the specific properties of each recorded spectrum (e.g. the proportion of spectrum intensity of the trail after meteor passage, meteor velocity, relative brightness, etc.). Sensitivity calibration of the spectrograph as a whole (y-axis) in the range of observed wavelengths is performed using a combination of line and continuous emission spectrum sources (e.g. Ne or Hg lamps).
Tab. 2: Overview of the number of recorded meteor spectra in 2025 at stations of the CEMeNt and SSO VMO networks. Author: Jakub Koukal
Expansion and modernization of the CEMeNt network
In October (October 3, 2025), the imaging camera at the Zvolenská Slatina station (SK) was changed. The existing CCD camera KPF 131 HR was replaced with a system with a CMOS camera with a Sony Starvis IMX 290 LQR chip. This camera operates at FHD resolution of 1920 × 1080 px (2.1 MPx) and with a frame rate of 30 fps. The Starlight lens used with high light sensitivity (f/0.95) with a fixed focal length (4 mm) in this configuration provides a field of view of 89 (± 1) × 50°. The station operator is Assoc. Prof. RNDr. Vladimír Bahýl, CSc.
Fig. 17: Overall view of the Zvolenská Slatina NW station (SK). Author: Alexandra Mikušková
Fig. 18: Overall view of the Blahová station (SK). Author: Alexandra Mikušková
In October (October 18, 2025), the imaging cameras (cameras S and W) at the Blahová station (SK) were changed. The existing CCD cameras Watec 902 H2 Ultimate and KPF 131 HR were replaced with systems with CMOS cameras with Sony Starvis IMX 290 LQR chips. These cameras operate at FHD resolution of 1920 × 1080 px (2.1 MPx) and with a frame rate of 30 fps. The Starlight lens used with high light sensitivity (f/0.95) with a fixed focal length (4 mm) in this configuration provides a field of view of 89 (± 1) × 50°. The station operator is Tibor Csörgei.
Acknowledgements
Thanks go to the companies DEZA , a. s. and CS CABOT , spol. s r. o., which contributed to the acquisition of equipment for FHD stations located at the Valašské Meziříčí Observatory and also within the CEMeNt network. Thanks go to all partner observatories (Ždánice, Vsetín, Rokycany, Plzeň, Karlovy Vary, Partizánske, Kysucké Nové Mesto) and also to private station owners (Milan Čermák, Richard Kačerek, Jakub Kapuš, Tibor Csörgei, Vladimír Bahýl, Ivo Míček) for supporting the activities and growth of the network. Thanks also go to all interested institutions for supporting the activities and growth of the network. The RPOS project (Development of Cross-Border Observational Network) was co-financed from the Small Projects Fund program of the Interreg V-A Slovak Republic – Czech Republic 2014 – 2020 program, call code 5/FMP/11b, reg. no. CZ/FMP/11b/05/058. The KOSOAP projects (Cooperating Network in the Field of Astronomical Professional-Observational Programs) and RPKS (Development of Cross-Border Cooperating Network for Professional Work and Education) were implemented by the observatories of Valašské Meziříčí (CZ) and Kysucké Nové Mesto (SK) in cooperation with SMPH (Society for Interplanetary Matter). The projects were co-financed from the Microprojects Fund of the Operational Program for Cross-Border Cooperation Slovak Republic – Czech Republic 2007-2013. The project for the purchase and operation of high-resolution spectroscopic cameras is partially funded by the Program for Regional Cooperation of the Czech Academy of Sciences, reg. no. R200402101. The installation of the Southern Spectroscopic Observatory of the Valašské Meziříčí Observatory in Chile is part of the KKC project (Cultural and Creative Center), co-financed by the European Union and the National Recovery Plan, as part of call no. 0231/2022 – Development of Regional Cultural and Creative Centers (project reg. no. 0231000014), administered by the Ministry of Culture of the Czech Republic. Installation costs were paid from co-financing provided by the Zlín Region. We thank the PLATOSpec consortium, which provided the opportunity to place spectral cameras and cooperation in installation and operation. The PLATOSpec project was built and is operated by a consortium consisting of the Astronomical Institute of the Czech Academy of Sciences in Ondřejov in the Czech Republic (ASU), the Thuringian State Observatory (Thüringer Landessternwarte - Germany), University Catholica in Chile (PUC - Chile), with smaller partners including Masaryk University (Czech Republic), Universidad Adolfo Ibañez (Chile), and the Institute of Plasma Physics of the Czech Academy of Sciences (Czech Republic). Financing of the 1.52m telescope modernization was provided by ASU and personnel costs were partially covered by grant LTT-20015. Financing of the PLATOSpec construction was provided by the Free State of Thuringia, represented by the "Thuringian Ministry of Education, Science and Culture" within the "Research Support Directive" and the German Center for Aviation and Tourism (DLR). Financial support for observations is within the institutional support for the development of the research organization of Masaryk University. Use of the 1.52m telescope was made possible by an agreement between ESO and the PLATOSpec consortium. Installation of the El Sauce station was made possible at the private El Sauce Observatory in cooperation with OBSTECH SpA .
