Bright bolide over the Moravian-Slovak border

Just a few days after three bright bolides, which were recorded on December 27, 2023, by instruments of the European Fireball Network, another bright bolide was recorded over the territory of the former Czechoslovakia. This bolide, which flew over the Moravian-Slovak border after two o’clock in the morning on January 9, 2024, was recorded by stations of the CEMeNt network (Central European MetEor NeTwork) as well as stations of the GMN network (Global Meteor Network), whose national component CSMON (Czech and Slovak Meteor Observation Network) operates within the Czech Republic and Slovakia. The bolide’s flight was recorded by five cameras of the CEMeNt network, one of which was spectroscopic. Recording the spectrum of the bolide from spectrographs at the Valašské Meziříčí Observatory is very important because it provides us with a large amount of information about the chemical composition of the body. In the case of the CSMON network, the bolide’s flight was recorded by eight cameras. From the available data from the cameras of the CEMeNt and CSMON networks, the bolide’s trajectory in the atmosphere and the trajectory of the body in the Solar System were calculated.
 

Jakub Koukal¹ ² and Libor Lenža¹ ²

¹ Valašské Meziříčí Observatory,
Vsetínská 78, CZ75701 Valašské Meziříčí, Czech Republic
jkoukal@astrovm.cz, libor.lenza@astrovm.cz
² J. Heyrovský Institute of Physical Chemistry, Academy of Sciences of the Czech Republic, Dolejškova 3, CZ18223 Prague 8, Czech Republic

 

VIDEO OBSERVATION – CEMENT

The bolide 20240109_011828 was recorded by cameras of the CEMeNt network on January 9, 2024, at 1:18:27.6 ± 0.1s UT. Within the CEMeNt network (Central European MetEor NeTwork), the bolide was captured directly by four wide-angle stations (Fig. 1-4). The flight record of the bolide is available from the Valašské Meziříčí SW and SE stations (Czech Republic, Valašské Meziříčí Observatory), Ždánice E station (Czech Republic, Ždánice Observatory), and Partizánske NW station (Slovakia, Partizánske Observatory). In addition to these stations, the spectrum of the bolide’s flight was recorded by the spectrograph Valašské Meziříčí SPSW (Czech Republic, Valašské Meziříčí Observatory), which is crucial for determining the chemical properties of the body, namely the content of chemical elements. Unfortunately, it was negatively affected by weather conditions (quite heavy fog).

Fig. 1: Summary image of the bolide 20240109_011828 captured by the Valašské Meziříčí SW camera. Author: Valašské Meziříčí Observatory, p.o.	Fig. 2: Summary image of the bolide 20240109_011828 captured by the Valašské Meziříčí SE camera. Author: Valašské Meziříčí Observatory, p.o.
Fig. 3: Summary image of the bolide 20240109_011828 captured by the Ždánice E camera. Author: Ždánice Observatory	Fig. 4: Summary image of the bolide 20240109_011828 captured by the Partizánske NW camera. Author: Partizánske Observatory

 

VIDEO OBSERVATION – CSMON

The bolide 20240109_011828 was recorded by cameras of the CSMON network on January 9, 2024, at 1:18:27.7 ± 0.1s UT. Within the CSMON network (Czech and Slovak Meteor Observation Network), the bolide was directly captured by eight wide-angle stations, of which data from five of them were used (Fig. 5-8). The flight record of the bolide is available from stations CZ0003 (Czech Republic, Prague), CZ0007 (Czech Republic, Zlín), CZ000C and CZ000D (Czech Republic, Libňatov), and SK0002 (Slovakia, Sládkovičovo).

Fig. 5: Summary image of the bolide 20240109_011828 captured by the CZ0003 camera. Author: Milan Kalina	Fig. 6: Summary image of the bolide 20240109_011828 captured by the CZ0007 camera. Author: Richard Káčerek
Fig. 7: Summary image of the bolide 20240109_011828 captured by the CZ000C camera. Author: Luboš Morávek	Fig. 8: Summary image of the bolide 20240109_011828 captured by the SK0002 camera. Author: Radim Stano

 

ATMOSPHERIC TRAJECTORY, RADIANT AND HELIOCENTRIC ORBIT

The bright bolide 20240109_011828 is an ideal case for comparing the compatibility of data obtained by various systems and different processing techniques, as observations were recorded by both the CEMeNt and CSmon network systems.
For the CEMeNt network systems, the atmospheric trajectory and the orbit of the meteoroid in the Solar System were calculated using recordings from the Valašské Meziříčí SW and SE, Ždánice E, and Partizánske NW stations. Recordings from these stations were processed using the UFOCapture program, analyzed in the UFO Analyzer program, and the atmospheric trajectory and heliocentric orbit were calculated using the UFO Orbit program (SonotaCo, 2009). The projection of the beginning of the atmospheric trajectory was located at coordinates N48.7204° E17.1751° near the village of Petrova Ves (SK), with the meteor’s altitude at that moment being 89.6 km above the Earth’s surface. The projection of the end of the atmospheric trajectory was located at coordinates N48.9525° E17.8103° near the village of Paseky (CZ), with the meteor’s altitude at that moment being 37.4 km above the Earth’s surface (Fig. 9,10). The bolide reached an absolute magnitude of -5.4^m and traveled a distance of 75.0 km in the Earth’s atmosphere during a flight time of 3.75 s (Tab. 1). Given the initial mass of the body and the final altitude of the atmospheric trajectory, it is highly probable that fragments of the body could not have impacted the Earth’s surface as meteorites. Therefore, the body’s mass was most likely completely vaporized during the ablative phase of the bolide’s flight.

Fig. 9: 2D projection of the entire atmospheric trajectory of the bolide 20240109_011828 onto the surface of the Earth (source of map data: Google Earth, Google Inc.). Author: Jakub Koukal, Milan Kalina	Fig. 10: 2D projection of the final part of the atmospheric trajectory of the bolide 20240109_011828 onto the surface of the Earth (source of map data: Google Earth, Google Inc.). Author: Jakub Koukal, Milan Kalina

The body entered the Earth’s atmosphere at an angle of 44.42°, with a velocity of 22.41 km/s before entering the atmosphere. The velocity at the end of the observed atmospheric trajectory was 6.13 km/s. Therefore, it was a relatively slow bolide, with a geocentric velocity of the meteoroid being 19.65 km/s (Tab. 1). The body did not belong to any known meteor shower, so it is classified as a sporadic meteor. Before entering the atmosphere, the body moved along an elongated orbit (Fig. 11) with a relatively high eccentricity (0.721), a low inclination to the plane of the ecliptic (5.35°), and a perihelion inside the orbit of Venus (0.6767 AU).

In the case of the CSMON network systems, the calculation of the bolide’s atmospheric trajectory and its orbit in the Solar System utilized recordings from stations CZ0003, CZ0007, CZ000C, CZ000D and SK0002. The complete recording and processing were conducted using the open RMS system (Vida et al., 2020; 2021). The projection of the beginning of the atmospheric trajectory was located at coordinates N48.6986° E17.1225° near the town of Gbely (SK), with the meteor’s altitude at that moment being 94.9 km above the Earth’s surface. The projection of the end of the atmospheric trajectory was located at coordinates N48.9582° E17.8132° near the village of Paseky (CZ), with the meteor’s altitude at that moment being 37.3 km above the Earth’s surface (Fig. 9,10). The body entered the Earth’s atmosphere at an angle of 44.50°, with a velocity of 22.85 km/s before entering the atmosphere. Therefore, it was a relatively slow bolide, with a geocentric velocity of the meteoroid being 19.97 km/s (Tab. 1). The body was classified under the southern December delta Arietid meteor shower (IAU MDC 0288). Before entering the atmosphere, the body moved along an elongated orbit (Fig. 11) with a relatively high eccentricity (0.733), a low inclination to the plane of the ecliptic (5.32°), and a perihelion inside the orbit of Venus (0.6729 AU).

Element	CEMeNt	CSMON	Element	CEMeNt	CSMON
RA (°)	101.49 ± 0.14	101.54	HB (km)	89.6 ± 0.1	94.9
DEC (°)	14.06 ± 0.16	14.25	HE (km)	37.4 ± 0.1	37.3
vg (km/s)	19.65 ± 0.42	19.97	Evbeg (°)	44.42 ± 0.06	44.50
a (AU)	2.421 ± 0.164	2.523	Azbeg (°)	240.07 ± 0.06	240.12
q (AU)	0.6767 ± 0.0060	0.6729	Lngbeg (°)	17.1751 ± 0.0008	17.1225
e (-)	0.721 ± 0.015	0.733	Latbeg (°)	48.7204 ± 0.0019	48.6986
peri (°)	75.205 ± 0.279	75.296	Lngend (°)	17.8103 ± 0.0008	17.8132
node (°)	107.9183	107.937	Latend (°)	48.9525 ± 0.0019	48.9582
i (°)	5.35 ± 0.04	5.32	vi (km/s)	22.41 ± 0.35	22.66
Tab. 1: Comparison of parameters of the atmospheric trajectory, heliocentric, and geocentric orbital elements of the bolide 20240109_011828, including the influence of deceleration on the bolide’s trajectory. Author: Jakub Koukal, Milan Kalina

The comparison of all orbital elements (heliocentric and geocentric) of the bolide’s orbit, as well as the parameters of the atmospheric trajectory, shows that the data provided by the CEMeNt and CSMON network systems are compatible with each other and can be combined despite different recording systems and processing methods. The mutual deviations of the elements mostly fall within the measurement error range. The lower initial altitude of the bolide’s atmospheric trajectory in the case of the CEMeNt network systems is caused by the lower sensitivity of the analog cameras used within this network.

 

PHYSICAL PROPERTIES

In the case of the bolide 20240109_011828, the estimation of the initial mass of the body and its other physical properties can be based on the heliocentric orbit elements, the atmospheric trajectory and also the chemical properties (elemental analysis) obtained from the analysis of the spectrum of the bolide from the Valašské Meziříčí SPSW spectrograph (Fig. 12).
For the initial determination of the parameters of the heliocentric orbit of the meteoroid, the Tisserand parameter with respect to Jupiter was calculated. Depending on the value of the Tisserand parameter, the inclination of the orbit, and the distance of the aphelion, the bodies can be divided into 4 groups. The bolide 20240109_011828 has a Tisserand parameter value of TP_J = 3.091.

According to this classification, the bolide belongs to the AST group, i.e., to the group of meteoroids with an asteroidal origin. However, according to the parameter K_B (7.555), which is a function of material properties and surface temperature (Ceplecha, 1968; Ceplecha and McCrosky, 1976; Ceplecha 1988), it belongs to the group of carbonaceous chondrites. According to the parameter P_E (-4.076), the bolide belongs to the group of ordinary chondrites. Using parameters that characterize the shape, velocity, and other properties of the body (Tab. 1), it was possible to calculate the initial mass of the body. Parallel to the calculation of the dynamic entry mass m_d, the calculation of the photometric entry mass m_f was performed. The initial dynamic mass of the meteoroid before entering the Earth’s atmosphere was 0.92 kg (m_d), so it is unlikely that fragments of the original body could be found as meteorites on the Earth’s surface. The calculation of the fragmentation strength of the meteoroid is based on the equality of dynamic pressure and the strength of the body as a whole at the moment of meteoroid breakup. The parameters of the atmosphere model at the given breakup altitude are calculated according to the NRLMSISE-00 model (Picone et al., 2002). The moment of breakup (fragmentation) of the body was determined from the course of the absolute brightness values of the bolide from the Partizánske NW station (Fig. 13). The fragmentation strength of the main part of the body is 0.165 MPa (Popova et al., 2011), which places the body more in the group of ordinary chondrites (OC). The determined mineralogical density (Benyukh, 1974) of the body (2.72 g/cm³) also suggests that the bolide 20190109_011828 was a body belonging to ordinary chondrites originating from the outer part of the main asteroid belt between Mars and Jupiter.

 

ACKNOWLEDGMENT

Thanks go to the coordinator of the CSMON network, Milan Kalina, for providing the data, as well as to all operators and owners of stations in the CEMeNt and CSMON networks. Thanks also go to all involved institutions for supporting the activities and growth of the network. The RPOS project (Cross-Border Observational Network Development) was co-financed from the Small Projects Fund of the Interreg V-A Program Slovakia – Czech Republic 2014 – 2020, call code 5/FMP/11b, reg. no. CZ/FMP/11b/05/058. The KOSOAP (Cooperating Network in the Field of Astronomical Observation Programs) and RPKS (Development of Cross-Border Cooperating Network for Professional Work and Education) projects were implemented by the Valašské Meziříčí Observatory (Czech Republic) and the Kysucké Nové Mesto Observatory (Slovakia) in cooperation with SMPH (Society for Interplanetary Matter). The projects were co-financed from the Micro-Projects Fund of the Operational Program for Cross-Border Cooperation Slovakia – Czech Republic 2007-2013. The purchase and operation of high-resolution spectroscopic cameras are partially funded by the Program for Regional Cooperation of the Czech Academy of Sciences, reg. no. R200402101 and grant APVV-0517-12 (FMFI UK). The purchase of instrument equipment located at the Valašské Meziříčí Observatory, p.o., was also supported by DEZA, a.s. and CS CABOT, spol. s r.o.

 

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Ceplecha Z. (1988). Earth’s influx of different populations of sporadic meteoroids from photographic and television data. Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), July 1988, 39, p. 221-236.
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